# Solar Neutrinos

Authors: V. Antonelli; L. Miramonti; C. Peña Garay; A. Serenelli
Journal: Advances in High Energy Physics
 (2013)

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## Abstract

The study of solar neutrinos has given a fundamental contribution both to astroparticle and to elementary particle physics, offering an ideal test of solar models and offering at the same time
relevant indications on the fundamental interactions among particles. After reviewing the striking results of the last two decades, which were determinant to solve the long standing solar neutrino puzzle and refine the Standard Solar Model, we focus our attention on the more recent results in this field and on the experiments presently running or planned for the near future. The main focus at the moment is to improve the knowledge of the mass and mixing pattern and especially to study in detail the lowest energy part of the spectrum, which represents most of the solar neutrino spectrum but is still a partially unexplored realm. We discuss this research project and the way in which present and future experiments could contribute to make the theoretical framework more complete and stable, understanding the origin of some “anomalies” that seem to emerge from the data and contributing to answer some present questions, like the exact mechanism of the vacuum to matter transition and the solution of the so-called solar metallicity problem.


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## Body

## 1. Motivations for the Solar Neutrino Study

The analysis of neutrinos emitted in the fusion processes inside the Sun is one of most significant examples of the relevant role played by the study of neutrino properties in elementary particle physics and astrophysics and in creating a link between these two sectors [1–13]. The pioneering work in the sixties [14–16] had the main goal of understanding better the way in which our star shines and to test solar models. But the surprising result of an apparent deficit in the electron neutrino flux reaching the detector marked the raise of the so-called solar neutrino puzzle and opened a whole new field of research, that has been central in elementary particle physics for many decades.The experimental results obtained using different techniques in more than thirty years [17] and the parallel theoretical advancements confirmed at the end the validity of Pontecorvo’s revolutionary idea of neutrino oscillation [18, 19], proving in a crystal clear way that neutrinos are massive and oscillating particles. This is one of the first pieces of clear evidence of the need to go beyond the standard model of electroweak interactions and the attempt to accommodate the experimental results about neutrino masses and mixing is a test that every theory “beyond the Standard Model” has to pass. Therefore, it is clear why these results had a great impact on elementary particle physics and also on cosmological models. At the same time, the possibility of measuring directly at least some components of the solar neutrino spectrum and of recovering in an indirect way the value of total solar neutrino flux have been fundamental for the progressive refinement of the standard solar model (SSM), which evolved during these years and is now in a general good agreement with the solar neutrino experiments.Despite the fundamental steps forward made in the last decades, many questions are still open about the real nature and the main properties of neutrinos and the exact mixing mechanism, for example, are neutrinos Majorana or Dirac fermions, the determination of mass hierarchy and exact mass values, accurate determination of the mixing angles, and presence of CP violation. The solar neutrino experiments presently running or planned for the future can contribute to solve at least some of these puzzles. The new frontier in this field is the study of the low energy part of the solar neutrino spectrum, which represents the great majority of the spectrum and is still an almost unexplored realm. Some of the challenges ahead are reducing significantly the indetermination onpep and CNO neutrinos and attaching the pp solar neutrino measurement. This would be essential to test the stability and consistency of the standard explanation of the oscillation mechanism, confirming or definitely disproving the presence of discrepancies between theory and experiments, which has lately stimulated a flourishing of models introducing the so-called “Non Standard Interactions” (Section 6.1). Once more, these results would be of great interest to improve the knowledge both of elementary particle properties and interactions and of the astrophysical models of the Sun. They could help also to discriminate between different versions of the solar models, for instance, for what concerns the so-called “solar abundance problem,” and to deepen the comparison with the results coming from other studies of solar properties, for example, from helioseismology. These studies would of course imply a further improvement of the already known detection techniques and the introduction of new ones (see, for instance, Section 7). Also from this point of view, solar neutrino physics will continue to give a stimulating contribution both to elementary particle physics and to astrophysics.In the present paper we are going to treat all of these topics, focusing our attention on the important advancements of the last years, on the main open questions, and the future perspectives of solar neutrino physics. In Section2, the interested reader can find a short review of the history of the so-called “solar neutrino puzzle,” from the the radiochemical experiments results up to the first data obtained by SNO and the reactor experiment KamLAND, that solved this puzzle. The following section is devoted to the standard solar model, its main input parameters (with the relative uncertainties) and predictions, the helioseismology, and the “metallicity problem.” The other ingredient essential for the calculation of the expected neutrino signal, the neutrino flavor conversion probability (in vacuum and matter), is discussed in Section 4. In Section 5, we report and discuss the important advancements which took place after 2002: from the results of the different phases of SNO and Super-Kamiokande to the discussion of the impact on solar neutrino physics of the data obtained by the reactor experiment KamLAND and finally to the first real-time measurements of the low energy solar neutrinos performed by Borexino. The discussion on the present phenomenological situation is completed in Section 6, with a particular attention to three flavors and to free fluxes analyses. We close the paper turning our attention to the near and far future, discussing the experimental and the theoretical challenges in Sections 7, 8, and 9.


## 2. Brief History and Solution of the Solar Neutrino Problem

### 2.1. From Homestake to Super-Kamiokande

The first experiment built to detect solar neutrinos took place in the Homestake gold mine in South Dakota [14–16]. The detector consisted of a large tank containing 615 metric tons of liquid perchloroethylene, chosen because it is rich in chlorine and the experiment operated continuously from 1970 until 1994. Neutrinos were detected via the reaction:
(1)νe+37Cl→37Ar+e-.
The energy threshold of this reaction, Eth=814 keV, allowed the detection of  7Be and 8B (and a small signal from the CNO and pep) but not that of pp neutrinos, because of their low maximal energy of 0.42MeV. The radioactive 37Ar isotopes decay by the electron capture with a τ1/2 of about 35 days into 37Cl*:
(2)37Ar+e-→37Cl*+νe.
Once a month, after bubbling helium through the tank, the 37Ar atoms were extracted and counted. The number of atoms created was only about 5 atoms of 37Ar per month in 615 metric tons C2Cl4. The number of detected neutrinos was lower (about 1/3 than the value expected) by the Solar Standard Model. This discrepancy is the essence of the solar neutrino problem, which has been for many years an important puzzle among physicists.There were three possible explanations to the solar neutrino problem. The first one was to consider that Homestake could be wrong, that is, the Homestake detector could be inefficient and, in this case, its reactions would not have been predicted correctly. After all, to detect a handful of atoms per week in more than 600 metric tons of material is not an easy task (the science that studies the interior of the Sun by looking at its vibration modes). The second one was to consider that the SSM was not correct, but as helioseismology started to provide independent tests of solar models, the SSM passed all tests. Indeed, nonstandard solar models constructed ad hoc to resolve the solar neutrino problem seemed very unlikely when scrutinized under the light of helioseismology. The third one, and the strangest hypothesis, was to consider that something happens to the neutrinos while traveling from the core of the Sun to the Earth.The first real-time solar neutrino detector, Kamiokande, was built in Japan in 1982-1983 [20]. It consisted of a large water Čerenkov detector with a total mass of 3048 metric tons of pure water. In real-time neutrino experiments, scientists study the bluish light produced by the electrons scattered by an impinging neutrino according to the following equation:
(3)νx+e-→νx+e-.
In the Kamiokande detector, light is recorded by 1000 photomultiplier tubes (PMT) and the energy threshold of the reaction is Eth=7.5 MeV; therefore, only 8B and hep neutrinos are detected (Here and in the rest of the paper, following the convention commonly adopted in the literature, we use the term “energy threshold” to indicate the lowest observable neutrino energy also for Čerenkov’s detector experiments. However, it is important to bear in mind that for these experiments, differently from the radiochemical ones, there is not a real energy threshold for the reaction and the lowest limit on the detectable energy is, instead, mainly due to the difficulty of separating the signal from the radioactive background due to natural sources and impurities.) At the beginning of the 90s, a much larger version of the detector was built, Super-Kamiokande, where the active mass was more than 50000 metric tons of pure water viewed by about 11200 PMTs. In Super-Kamiokande, the energy threshold was lowered to Eth=5.5 MeV [21].Radiochemical experiments integrate in time and in energy because they are slow and need time to produce measurable results. This causes the loss of information about single individual energy values. In real-time experiments, instead, it is possible to obtain single values and therefore a spectrum energy to distinguish the different neutrino contributions. Furthermore, given that the scattered electron maintains the same direction of the impinging neutrino, it is possible to infer the direction of the incoming neutrino and therefore to point at its source. This proved that the detected neutrinos actually came from the Sun. The number of detected neutrinos was about 1/2 lower than the number of expected ones, aggravating the solar neutrino problem.Until 1990, there were no observations of the initial reaction in the nuclear fusion chain, that is, the detection ofpp neutrinos, which are less model dependent and hence more significant to test the hypothesis that fusion of hydrogen powers the Sun. Two radiochemical experiments were built in order to detect solar pp neutrinos, both employing the reaction
(4)νe+Ga71→Ge71+e-,
which has a threshold of Eth=233keV.In the Gallex experiment, located at the Gran Sasso underground laboratory in Italy, 30 metric tons of natural gallium were employed [22, 23], while in the Soviet-American experiment (SAGE), located in the Baksan underground laboratory, there were more than 50 metric tons of metallic gallium [24]. Calibration tests with an artificial neutrino source, 51Cr, confirmed the efficiency of both detectors. Once again, the measured neutrino signal was smaller than predicted by the SSM (≈60%).All experiments detected fewer neutrinos than expected from the SSM. Table1 summarizes the ratios between the observed and the expected neutrino interaction rates for all the experiments before SNO.Table 1
Ratios of the observed versus expected neutrino rates in the four solar neutrino experiments (before SNO, see later).
Homestake
0.34
±
0.03
Super-K
0.46
±
0.02
SAGE
0.59
±
0.06
Gallex and GNO
0.58
±
0.05


### 2.2. The Advent of SNO and KamLAND: The Solution of the Solar Neutrino Problem

The real breakthrough in solar neutrino physics was due to the advent of the SNO (Sudbury Neutrino Observatory) experiment. It had the peculiarity to measure simultaneously, by means of a deuterium Čerenkov detector, three different interaction channels for neutrinos: the neutral current (NC:νX+d→νX+p++n), receiving contributions from all active flavors, the elastic scattering (ES: νX+e-→νX+e-), and the charged current (CC: νe+d→e-+p++p+), that is, sensitive only to electronic neutrinos. In this way, it has been possible to prove in a clear and direct way that the measured total neutrino flux was in a very good agreement with the SSM predictions, but only a fraction of these neutrinos had conserved its flavor during their way from the production point in the Sun to the detector.The first SNO data [25], including elastic scattering and charged current analysis, published in 2001, confirmed the results obtained by previous solar neutrino experiments, mainly by Super-Kamiokande [26], providing a significant evidence (at the 3.3σ level) of the presence of a nonelectronic active neutrino component in the solar flux. For the first time, it was possible to indicate the large mixing angle (LMA) as the preferred solution of the solar neutrino puzzle, even if different alternative possibilities (and in particular the low probability, low mass -LOW- solution) were still surviving [27, 28]. In the following years, the SNO experiment measured also the neutral current channel, using different techniques. The data of these different “phases” of the experiment are usually reported as SNO I [29], SNO II [30] (characterized by the addition of salt to improve the efficiency of neutral current detection) and SNO III [31] (with the use of helium chamber proportional counters).The year 2002 is very often denoted as the “annus mirabilis” of solar neutrino physics: in April the first SNO results including neutral current detection [29, 32] marked a turning point in the history of the solar neutrino problem, in October the Nobel prize for physics was awarded to Davis [33] and Koshiba (for their pioneering work on the detection of cosmic neutrinos), and in December of the same year the first results of the Kamiokande Liquid scintillator antineutrino detector (KamLAND) [34] offered the first clear terrestrial confirmation of the validity of the oscillation solution to the solar neutrino problem.The total8B neutrino flux, ϕNC=5.09-0.43+0.44 (stat)-0.43+0.46(syst)×106cm-2s-1, measured by SNO with neutral currents was in a very good agreement with the SSM [35]. Assuming the standard shape for the component of the solar neutrino flux (undistorted spectrum hypothesis), the SNO collaboration recovered also a value of the nonelectronic component of the flux which was 5.3σ different from zero, providing a direct proof of the validity of the oscillation hypothesis. These data were also decisive to indicate the LMA region as the solution to the solar neutrino puzzle.Looking at the oscillation probability it is apparent that the reactor experiments that run before KamLAND, and used neutrino energy beams of the order of the MeV with a baseline of the order of 1 km, could test only values ofΔm2 above 10-3 eV2 (For instance, in a simple 2-flavor analysis, the flavor transition probability is given by the expression P12=sin2(2θ12)sin2(Δm122(eV2)L(km)/4E(GeV)), where θ12 is the mixing angle between the two flavors, Δmij2≡m12-m22 the difference of the masses squared, L the distance traveled, and E the neutrino energy.) The KamLAND experiment, instead, with an average baseline of about 180 km, was ideal to probe the LMA region, which corresponds to values of Δm2 of the order 10−5–10−4 eV2 [36–38]. The KamLAND experiment studied the ratio of the number of inverse β decay events (due to reactor ν-e with an energy threshold of 3.4 MeV) to the expected number of events without disappearance and also the spectrum shape [34]. The observed deficit of events was inconsistent with the expected rate in absence of oscillation at the 99.95% confidence level.Since one would expect a negligible reduction of theν-e flux from the SMA, LOW, and vacuum solar neutrino solutions, the LMA was the only oscillation solution compatible with KamLAND results and CPT invariance. This evidence was further reinforced by the data published by the collaboration in the following years (with greater statistical precisions and reduced systematic errors), which showed also a spectral distortion in a very good agreement with the oscillation solution [39–41]. KamLAND data also restricted the allowed LMA region in a significant way. The preferred values for Δm122 and θ12 are slightly higher than the ones corresponding to the best fit solution of the solar neutrino experiments, but this small tension can be explained by taking into account the experimental uncertainties. Moreover, the difference on the Δm122 parameter has been reduced by the more recent solar neutrino data.


## 2.1. From Homestake to Super-Kamiokande

The first experiment built to detect solar neutrinos took place in the Homestake gold mine in South Dakota [14–16]. The detector consisted of a large tank containing 615 metric tons of liquid perchloroethylene, chosen because it is rich in chlorine and the experiment operated continuously from 1970 until 1994. Neutrinos were detected via the reaction:
(1)νe+37Cl→37Ar+e-.
The energy threshold of this reaction, Eth=814 keV, allowed the detection of  7Be and 8B (and a small signal from the CNO and pep) but not that of pp neutrinos, because of their low maximal energy of 0.42MeV. The radioactive 37Ar isotopes decay by the electron capture with a τ1/2 of about 35 days into 37Cl*:
(2)37Ar+e-→37Cl*+νe.
Once a month, after bubbling helium through the tank, the 37Ar atoms were extracted and counted. The number of atoms created was only about 5 atoms of 37Ar per month in 615 metric tons C2Cl4. The number of detected neutrinos was lower (about 1/3 than the value expected) by the Solar Standard Model. This discrepancy is the essence of the solar neutrino problem, which has been for many years an important puzzle among physicists.There were three possible explanations to the solar neutrino problem. The first one was to consider that Homestake could be wrong, that is, the Homestake detector could be inefficient and, in this case, its reactions would not have been predicted correctly. After all, to detect a handful of atoms per week in more than 600 metric tons of material is not an easy task (the science that studies the interior of the Sun by looking at its vibration modes). The second one was to consider that the SSM was not correct, but as helioseismology started to provide independent tests of solar models, the SSM passed all tests. Indeed, nonstandard solar models constructed ad hoc to resolve the solar neutrino problem seemed very unlikely when scrutinized under the light of helioseismology. The third one, and the strangest hypothesis, was to consider that something happens to the neutrinos while traveling from the core of the Sun to the Earth.The first real-time solar neutrino detector, Kamiokande, was built in Japan in 1982-1983 [20]. It consisted of a large water Čerenkov detector with a total mass of 3048 metric tons of pure water. In real-time neutrino experiments, scientists study the bluish light produced by the electrons scattered by an impinging neutrino according to the following equation:
(3)νx+e-→νx+e-.
In the Kamiokande detector, light is recorded by 1000 photomultiplier tubes (PMT) and the energy threshold of the reaction is Eth=7.5 MeV; therefore, only 8B and hep neutrinos are detected (Here and in the rest of the paper, following the convention commonly adopted in the literature, we use the term “energy threshold” to indicate the lowest observable neutrino energy also for Čerenkov’s detector experiments. However, it is important to bear in mind that for these experiments, differently from the radiochemical ones, there is not a real energy threshold for the reaction and the lowest limit on the detectable energy is, instead, mainly due to the difficulty of separating the signal from the radioactive background due to natural sources and impurities.) At the beginning of the 90s, a much larger version of the detector was built, Super-Kamiokande, where the active mass was more than 50000 metric tons of pure water viewed by about 11200 PMTs. In Super-Kamiokande, the energy threshold was lowered to Eth=5.5 MeV [21].Radiochemical experiments integrate in time and in energy because they are slow and need time to produce measurable results. This causes the loss of information about single individual energy values. In real-time experiments, instead, it is possible to obtain single values and therefore a spectrum energy to distinguish the different neutrino contributions. Furthermore, given that the scattered electron maintains the same direction of the impinging neutrino, it is possible to infer the direction of the incoming neutrino and therefore to point at its source. This proved that the detected neutrinos actually came from the Sun. The number of detected neutrinos was about 1/2 lower than the number of expected ones, aggravating the solar neutrino problem.Until 1990, there were no observations of the initial reaction in the nuclear fusion chain, that is, the detection ofpp neutrinos, which are less model dependent and hence more significant to test the hypothesis that fusion of hydrogen powers the Sun. Two radiochemical experiments were built in order to detect solar pp neutrinos, both employing the reaction
(4)νe+Ga71→Ge71+e-,
which has a threshold of Eth=233keV.In the Gallex experiment, located at the Gran Sasso underground laboratory in Italy, 30 metric tons of natural gallium were employed [22, 23], while in the Soviet-American experiment (SAGE), located in the Baksan underground laboratory, there were more than 50 metric tons of metallic gallium [24]. Calibration tests with an artificial neutrino source, 51Cr, confirmed the efficiency of both detectors. Once again, the measured neutrino signal was smaller than predicted by the SSM (≈60%).All experiments detected fewer neutrinos than expected from the SSM. Table1 summarizes the ratios between the observed and the expected neutrino interaction rates for all the experiments before SNO.Table 1
Ratios of the observed versus expected neutrino rates in the four solar neutrino experiments (before SNO, see later).
Homestake
0.34
±
0.03
Super-K
0.46
±
0.02
SAGE
0.59
±
0.06
Gallex and GNO
0.58
±
0.05


## 2.2. The Advent of SNO and KamLAND: The Solution of the Solar Neutrino Problem

The real breakthrough in solar neutrino physics was due to the advent of the SNO (Sudbury Neutrino Observatory) experiment. It had the peculiarity to measure simultaneously, by means of a deuterium Čerenkov detector, three different interaction channels for neutrinos: the neutral current (NC:νX+d→νX+p++n), receiving contributions from all active flavors, the elastic scattering (ES: νX+e-→νX+e-), and the charged current (CC: νe+d→e-+p++p+), that is, sensitive only to electronic neutrinos. In this way, it has been possible to prove in a clear and direct way that the measured total neutrino flux was in a very good agreement with the SSM predictions, but only a fraction of these neutrinos had conserved its flavor during their way from the production point in the Sun to the detector.The first SNO data [25], including elastic scattering and charged current analysis, published in 2001, confirmed the results obtained by previous solar neutrino experiments, mainly by Super-Kamiokande [26], providing a significant evidence (at the 3.3σ level) of the presence of a nonelectronic active neutrino component in the solar flux. For the first time, it was possible to indicate the large mixing angle (LMA) as the preferred solution of the solar neutrino puzzle, even if different alternative possibilities (and in particular the low probability, low mass -LOW- solution) were still surviving [27, 28]. In the following years, the SNO experiment measured also the neutral current channel, using different techniques. The data of these different “phases” of the experiment are usually reported as SNO I [29], SNO II [30] (characterized by the addition of salt to improve the efficiency of neutral current detection) and SNO III [31] (with the use of helium chamber proportional counters).The year 2002 is very often denoted as the “annus mirabilis” of solar neutrino physics: in April the first SNO results including neutral current detection [29, 32] marked a turning point in the history of the solar neutrino problem, in October the Nobel prize for physics was awarded to Davis [33] and Koshiba (for their pioneering work on the detection of cosmic neutrinos), and in December of the same year the first results of the Kamiokande Liquid scintillator antineutrino detector (KamLAND) [34] offered the first clear terrestrial confirmation of the validity of the oscillation solution to the solar neutrino problem.The total8B neutrino flux, ϕNC=5.09-0.43+0.44 (stat)-0.43+0.46(syst)×106cm-2s-1, measured by SNO with neutral currents was in a very good agreement with the SSM [35]. Assuming the standard shape for the component of the solar neutrino flux (undistorted spectrum hypothesis), the SNO collaboration recovered also a value of the nonelectronic component of the flux which was 5.3σ different from zero, providing a direct proof of the validity of the oscillation hypothesis. These data were also decisive to indicate the LMA region as the solution to the solar neutrino puzzle.Looking at the oscillation probability it is apparent that the reactor experiments that run before KamLAND, and used neutrino energy beams of the order of the MeV with a baseline of the order of 1 km, could test only values ofΔm2 above 10-3 eV2 (For instance, in a simple 2-flavor analysis, the flavor transition probability is given by the expression P12=sin2(2θ12)sin2(Δm122(eV2)L(km)/4E(GeV)), where θ12 is the mixing angle between the two flavors, Δmij2≡m12-m22 the difference of the masses squared, L the distance traveled, and E the neutrino energy.) The KamLAND experiment, instead, with an average baseline of about 180 km, was ideal to probe the LMA region, which corresponds to values of Δm2 of the order 10−5–10−4 eV2 [36–38]. The KamLAND experiment studied the ratio of the number of inverse β decay events (due to reactor ν-e with an energy threshold of 3.4 MeV) to the expected number of events without disappearance and also the spectrum shape [34]. The observed deficit of events was inconsistent with the expected rate in absence of oscillation at the 99.95% confidence level.Since one would expect a negligible reduction of theν-e flux from the SMA, LOW, and vacuum solar neutrino solutions, the LMA was the only oscillation solution compatible with KamLAND results and CPT invariance. This evidence was further reinforced by the data published by the collaboration in the following years (with greater statistical precisions and reduced systematic errors), which showed also a spectral distortion in a very good agreement with the oscillation solution [39–41]. KamLAND data also restricted the allowed LMA region in a significant way. The preferred values for Δm122 and θ12 are slightly higher than the ones corresponding to the best fit solution of the solar neutrino experiments, but this small tension can be explained by taking into account the experimental uncertainties. Moreover, the difference on the Δm122 parameter has been reduced by the more recent solar neutrino data.


## 3. Standard Solar Model

SSMs have to be understood, primarily, as a framework within which solar models can be constructed and clear predictions can be made with respect to the properties of the solar interior, including the production of solar neutrinos. The defining characteristics are simple: the SSM is the result of the evolution of a 1M⊙ star since its formation and the evolutionary models have to include the physical ingredients considered standard in stellar structure and evolution models (here, standard also implies trying to keep to a minimum the number of free tunable parameters—knobs—in the model). SSMs are therefore progressively refined as our understanding of stellar physics progresses.In practice, an SSM is constructed as follows. An initial chemically homogeneous model of a 1M⊙ stellar model on the premain sequence is constructed with a composition determined by a guess (educated one) for the initial mass fractions of hydrogen Xini, helium Yini, and metals Zini(Xini+Yini+Zini=1); additionally, a third free parameter has to be specified, the mixing length parameter αMLT of convection. This model is then evolved up to the solar system age τ⊙=4.57 Gyr [42, 43]. At this age, the model is required to match the present-day solar luminosity L⊙ and radius R⊙, as well as the surface metal-to-hydrogen abundance ratio (Z/X)⊙. The initial and final surface metal-to-hydrogen ratios differ by about 10% to 15% due to the effects of gravitational settling. In general, the SSM constructed with the first set of guesses for αMLT, Yini, and Zini will not lead to a satisfactory agreement with the surface constraints, and an iterative procedure is used to refine the free parameters until the right surface conditions are achieved at τ⊙. In general, surface conditions are matched to one part in 105 or 106 within two or three iterations. It is important to keep in mind that the SSM is not just a snapshot aimed at representing the present-day structure of the Sun, but actually the result of taking into account all its previous history. There are alternative ways to construct a model of the present-day solar structure using, for example, helioseismic constraints. This kind of models is constructed “ad-hoc” to match helioseismic data and is, therefore, a limited predictive power.The internal structure of an SSM depends on the values adopted for the three constraints mentioned above and, of course, on the physical inputs of the models such as the radiative opacities, cross-sections of nuclear reactions, and others. Next, we describe the changes/updates that have occurred during the last decade that impact predictions of solar models.


### 3.1. Input Physics and Parameters

#### 3.1.1. Solar Surface Composition

The constraint imposed by the surface metallicity of the Sun or, more precisely, the surface metal-to-hydrogen ratio(Z/X)⊙ is critical in the construction of solar models. The reason is that, aside from the 10 to 15% change in this value due to the action of gravitational settling, (Z/X)⊙ determines almost directly the metallicity of solar models. As for any other star, the metal content in the Sun has a fundamental role in its structure through its contribution to the radiative opacity κ, which determines, in turn, the temperature gradient in the radiative solar interior. It is important, in fact, that the abundance of individual metals are accurately determined, because different elements contribute to the radiative opacities in different regions of the Sun.The abundance of metals in the solar surface has to be determined or inferred from a variety of sources: photospheric abundances from solar spectra, chemical analysis of primitive meteorites, emission lines from the solar corona, and composition of the solar wind [44]. While meteoritic abundances are the most precisely determined, at 2/3 of the solar metallicity is composed by the volatile elements C, N, and O and can only be determined from the analysis of the solar spectrum.Over the last decade, the development of three-dimensional radiation hydrodynamic (3D RHD) models of the solar atmosphere has prompted a thorough revision of the solar composition determined from the solar spectrum. These 3D RHD models of the solar atmosphere capture the dynamics of convection and its interaction with the radiation field and are able to reproduce features such as the solar granulation pattern, observed limb-darkening, and asymmetries in the shapes of spectral lines [45]. The structure of the solar model atmospheres derived by different groups are nicely consistent with each other, adding to the credibility of the models. Newly derived spectroscopic abundances rely on the 3D atmosphere model or more appropriately on a one-dimensional model obtained from a suitably averaged 3D model, as the background on top of which detailed radiative transfer and line formation calculations are performed a posteriori. It is this second step that leads, finally, to the determination of the abundances of the different elements. The most thorough and consistent determination of the solar photospheric abundances based on 3D model atmospheres has been presented by Asplund and collaborators [46, 47], although the revision on key elements like oxygen was initially published already in 2001 [48]. In addition to using 3D RHD atmosphere models, nonlocal thermodynamic equilibrium has been taken into account when computing the line formation for some key elements such as C, N, and O. Also, and this is of particular importance for oxygen, blends in the solar spectrum that had been previously unnoticed were identified and taken into account in the determination of abundances. The most relevant result in the context of solar models and neutrinos is that abundances of CNO elements (also Ne, but this is mostly because its abundance ratio to oxygen is assumed fixed) have been revised down by 30% to 40%. Combining the abundance of all metals, the present-day metal-to-hydrogen ratio that has been obtained is (Z/X)⊙=0.0178 [46]. This represents a large decrease in comparison with previously accepted values, 0.0245 [49] and 0.0229 [50], that have been widely used in solar modeling. We note, however, that results by Asplund have not been unchallenged. In fact, also based on 3D RHD model solar atmospheres, larger CNO abundances have been derived [51] to yield (Z/X)⊙=0.0209, much closer to older determinations. Discrepancies between authors seem to have their origin at the preferred set of spectral lines each group uses and on using either a spectral synthesis or equivalent width techniques to determine the final abundances.In the last decade, there have been two flavors in SSM calculations. In one case, ahigh solar metallicity from older determinations [49, 50] is adopted; we will generically refer to these models as high-Z solar models. In the other case, a low(Z/X)⊙ [46, 47] is taken from and we refer to these, not surprisingly, as the low-Z solar models. Differences in the structure of high-Z and low-Z models are readily noticeable in quantities such as the internal sound speed and density profiles, the depth of the solar convective envelope, and the surface helium abundance among others. The deficit that low-Z models have in matching helioseismic constraints has been named the solar abundance problem in the literature, in clear analogy to the solar neutrino problem. We discuss it in some detail in Section 3.2.


#### 3.1.2. Radiative Opacities

The most widely used calculations of atomic radiative opacities, appropriate for solar interiors, are those from OPAL [52]. However, the opacity project (OP) released in 2005 a completely independent set of atomic radiative opacities for stellar interiors [53]. In the case of the solar radiative interior, differences between OPAL and OP Rosseland mean opacities are of the order of a few percent, with OP being larger by about 3% at the base of the convective zone and 1% to 2% smaller in the central regions (see Figure 7 in [53]). At low temperatures neither OP nor OPAL atomic opacities are adequate, because the possible formation of molecules have to be taken into account and, therefore, they have to be complemented by low-temperature opacities [54]. However, due to the relatively high solar temperature, their influence in the properties of solar models is rather limited.


#### 3.1.3. Nuclear Reactions Cross-Sections

Experimental and theoretical work on the determination of nuclear cross-sections have been very active fields with a strong impact on solar model predictions of solar neutrino fluxes (A nonresonant charged-particle induced reaction cross-section can be written asσ(E)=(S(E)/E)exp[-2πη(E)] where η(E)=Z1Z2α/v is the Sommerfeld parameters, v=(2E/μ), α the fine structure constant in natural units, and μ the reduced mass of the interacting nuclei. The nuclear physics is isolated in S(E), the astrophysical or S-factor, a slowly varying function of energy that can be more accurately extrapolated from experimental data down to the energy of the Gamow peak.) Recently, a set of recommended rates and uncertainties, expressed through the S-factor for all the reactions both in the pp-chains and CNO-bicycle that are relevant to solar modeling and neutrino production, has been published (Solar Fusion II, [55], hereafter SFII). The results presented in SFII reflect the progress made in laboratory and theoretical nuclear astrophysics over the last decade, since the publication of the seminal Solar Fusion I (SFI) article [56]. Unfortunately, for reasons of space, here we cannot review in detail every reaction. Instead, we provide in Table 2 the standard S-factors at zero energy, S(0), and the uncertainties recommended in SFII for the most relevant reactions. For comparison, with results from SFI are also shown. The impact of changes in key reactions on the production of neutrino fluxes is discussed in Section 3.3. The reader is referred to the SFII paper and references therein for details on the experimental and theoretical developments in nuclear astrophysics related to the Sun during the last decade.Table 2
Standard astrophysical factors and uncertainties for key nuclear reactions in thepp-chains and CNO-bicycle. SFII represents the state-of-the-art [55]; SFI [56] shows, for comparison, the situation around 1998.
Reaction
SFII
SFI
S
(
0
)
[
keV
b
]
S
(
0
)
[
keV
b
]
S
11
p
(
p
,
e
+
ν
e
)
d
4.01
×
1
0
-
22
(
1
±
0.010
)
4.00
×
1
0
-
22
(
1
±
0.005
)
S
33
3

He
(
3
He
,
2
p
)
4
He
5.21
×
1
0
3
(
1
±
0.052
)
5.4
×
1
0
3
(
1
±
0.074
)
S
34
3

He
(
4
He
,
γ
)
7
Be
5.6
×
1
0
-
1
(
1
±
0.054
)
5.3
×
1
0
-
1
(
1
±
0.094
)
Shep
3

He
(
p
,
e
+
ν
e
)
4
He
8.6
×
1
0
-
20
(
1
±
0.30
)
2.3
×
1
0
-
20
S
17
7

Be
(
p
,
γ
)
8
B
2.08
×
1
0
-
2
(
1
±
0.077
)
1.9
×
1
0
-
2
(
1
-
0.10
+
0.20
)
S
1,14
14

N
(
p
,
γ
)
15
O
1.66
(
1
±
0.072
)
3.5
(
1
-
0.46
+
0.11
)


### 3.2. Solar Models: Helioseismology

Helioseismology, the study of the natural oscillations of the Sun, provides a unique tool to determine the structure of the solar interior. The 90s witnessed a rapid development of helioseismic observations and analysis techniques, which led, in very few years, to an accurate characterization of the solar interior [57]. The agreement between SSMs and helioseismic inferences of the solar structure [35, 58] provided a strong support to the accuracy with which SSMs could predict the 8B neutrino flux and, therefore, a strong indication, before Kamland and SNO results found evidence of neutrino flavor oscillations, that the solution to the solar neutrino problem had to be found in the realm of particle physics.In the context of the present paper, the most relevant results from helioseismology are the following (The Sun is characterized by an outer region where energy is transported by convection. The boundary between this region, located atRCZ, and the radiative interior can be accurately located by helioseismology because the discontinuity in the slope of the temperature gradient across this boundary leaves its imprint in the solar sound speed profile. The depth of the envelope can be located by helioseismology because properties of solar oscillations are sensitive to the derivative of the sound speed as a function of depth.) The depth of the convective envelope is RCZ=0.713±0.001 R⊙ [59] and the surface helium abundance YS=0.2485±0.0034 [60]. The sound speed differences between the Sun and a reference solar model can be obtained by inversion from the oscillation frequencies with a formal error of a few parts per 10-4 for most of the solar interior 0.07≲R/R⊙≲0.95 [61, 62]. Most recently, using a time series 4752 days long from the Birmingham Solar Oscillation Network, improved results on the sound speed in the solar core have been obtained [63]. The density profile can also be determined from the inversion of frequencies, but with worse precision than for the sound speed, and we therefore assign to it a secondary role in constraining the solar structure.As mentioned previously, metals determine to a large extent the radiative opacity in the solar interior and, in this way, define the temperature stratification from below of the convective envelope inwards, to the solar center. At the base of the convective zone, for example, metals are responsible for about 70% of the total radiative opacity with O, Fe, and Ne being the main contributors. In the solar core, where light metals are completely ionized, the contribution from Fe and, to a lesser extent Ni, Si, and S, is still above 30%. In view of this, it is not surprising that the low CNO and Ne abundances determined from 3D model atmospheres have a strong impact on the structure of the solar interior.It has been clear since initial works wherelow-Z SSMs were presented that low (Z/X)⊙ values posed a problem, later named the solar abundance problem, for solar modeling [60, 67–69]. In short, all helioseismic predictions of these models are in disagreement with observations. On the other hand, high-Z SSMs have consistently reproduced earlier success [58]. The solar abundance problem represents the incompatibility between the best solar atmosphere and interior models available [70]. In this paper, we will base the presentation and discussion of results on the most up-to-date standard solar models that we identify as SFII-GS98 and SFII-AGSS09 [64], representative of high-Z and low-Z SSM families defined in Section 3.1, respectively. With the exception made on small quantitative variations, results based on these models are extensible to results for all SSMs available in the literature corresponding to each of the two families.The most important characteristics of the SFII-GS98 and SFII-AGSS09 models are summarized in Table3. Helioseismic constraints are also included for comparison when appropriate. The disagreement between SFII-AGSS09 and helioseismic data is evident in the surface metallicity and helium abundances, ZS and YS, and in the depth of the convective envelope RCZ. A similar conclusion could be drawn from comparing Yini; however, the determination of the solar value of Yini [71] depends strongly on the seismic value for YS and, therefore, it is not an independent constraint. When model uncertainties are included, the discrepancy between SFII-AGSS09 and seismic results are, for each of the quantities mentioned above, of the order 3 to 4-σ [72]. On the contrary, the SFII-GS98 model performs very well, within 1-σ, when model uncertainties are accounted for.Table 3
Main characteristics of SSMs representative ofhigh-Z (GS98) and low-Z (AGSS09) solar compositions. Models have been computed including the most up-to-date input physics [64]. Helioseismic constraints are given when available. See text for details.
SFII-GS98
SFII-AGSS09
Helioseismology
(
Z
/
X
)
⨀
0.0229
0.0178
—
Z
S
0.0170
0.0134
0.0172
±
0.002 [65]
Y
S
0.2429
0.2319
0.2485
±
0.0034 [60]
R
CZ
/
R
⨀
0.7124
0.7231
0.713
±
0.001 [59]
〈
δ
c
/
c
〉
0.0009
0.0037
—
〈
δ
ρ
/
ρ
〉
0.011
0.040
—
Z
C
0.0200
0.0159
—
Y
C
0.6333
0.6222
—
〈
μ
C
〉
0.7200
0.7136
0.7225
±
0.0014 [66]
Z
ini
0.0187
0.0149
—
Y
ini
0.2724
0.2620
—Very explicit manifestations of the solar abundance problem are shown in the plots in Figure1, where degradation in the sound speed and density profiles found in low-Z SSMs are clearly evident. Particularly the peak in the sound speed profile differences found right below the convective zone is 4 times larger in the low-Z SFII-AGSS09 than in the high-Z SFII-GS98 model. The reason is the wrong location of RCZ in the model, caused by the lower opacity which, in turn, is due to the low abundance of metals. The density profile also shows very large discrepancies, but they are less telling. Density inversions include as a constraint the known value of the solar mass and for this reason small differences in the core, where density is large, translate into the large difference seen in the outer envelope. The average rms in the sound speed and density differences, 〈δc/c〉 and 〈δρ/ρ〉, also show that low-Z models are about 4 times worse than high-Z models.Figure 1
Sound speed and density relative differences between solar models and the Sun as determined from helioseismic inversions [72]. The convective envelope is depicted by the grey area.Low-degree helioseismology provides useful information about the solar innermost regions. Specific combinations of mode frequencies enhance the signal that the structure of the solar core imprints on the oscillation pattern [73]. This has been used to determine the mean molecular weight averaged over the innermost 20% solar core [66], 〈μC〉 in Table 3. Comparison with SSMs results shows that 〈μC〉 is too low in low-Z models as a result of the lower helium abundance (YC). This is due to the lower temperature in the solar core and the constraint imposed by the solar luminosity. The decreased nuclear energy production originated by a smaller core temperature has to be compensated by an increased hydrogen mass fraction, therefore leading to a lower molecular weight. It is interesting to note this puts a stringent constraint in the amount of rotational mixing that can take place in the solar core if the low-Z abundances are correct, since any mixing would lower the molecular weight even more, by bringing fresh hydrogen from outer regions, and make the agreement with helioseismic data worse.The current situation regarding SSMs and their performance against helioseismic inferences on the solar structure can be summarized as follows. SSMs that use solar abundances derived from 1D model atmospheres [49, 50], that is, high-Z models, reproduce overall the most important seismic constraints. Improvements in the input physics, for example, radiative opacities and nuclear reaction rates, that have occurred over the last 10 years introduce only small changes to the solar structure as seen by helioseismology. On the other hand, the solar abundance problem arises if the solar surface composition used to construct SSMs are derived from the most sophisticated 3D RHD solar model atmospheres. The family of low-Z SSMs does not match any helioseismic constraint.Have we reached the limit where the paradigm of the SSM is not good enough as a model of the solar interior? Are the 3D-based determinations of solar abundances systematically underestimating the metallicity of the solar surface? Does the microscopic input physics in solar models, for example, radiative opacities, need to be thoroughly revised? It is not possible to advance answers to these questions, but solar neutrino experiments can play an important role in guiding the research towards the solution of the solar abundance problem. In the next section, we discuss the current status on the theoretical predictions of solar neutrino fluxes and the prospects of using solar neutrinos to constraint the properties of the solar core.


### 3.3. Solar Models: Neutrino Fluxes

#### 3.3.1. Production

Based on theoretical arguments and indirect evidence, it has long been believed that the source of energy of the Sun is the conversion of protons into helium,4p→He4+2e++2νe+γ. The original quest for solar neutrinos was indeed the search for the experimental confirmation of this hypothesis (Under peculiar conditions reached in advanced phases of stellar evolution, hydrogen can be converted into helium by other cycles like the NaMg-cycle. While important for nucleosynthesis or intermediate mass elements, these processes are not energetically relevant.) In more detail, hydrogen burning in the Sun (and in all other hydrogen-burning stars) takes place either through the pp-chains or the CNO-bicycle [43, 75]. Proton fusion through the pp-chains is a primary process because only protons need to be present in the star. On the contrary, the CNO-bicycle is secondary because the proton fusion relies on, and is regulated by, the abundance of C, N, and O which act as catalyzers. This qualitative difference is very important, since it renders neutrino fluxes from the CNO-bicyle a very good diagnostic tool to study properties of the solar core, particularly its composition, as it will be discussed below. A general discussion on the production of solar neutrinos is out of the scope of the present paper, but can be found elsewhere [43].SSM calculations of neutrino fluxes have been affected by developments in the input physics discussed in previous sections. The two areas that have the strongest impact on the neutrino fluxes predicted by models are changes in nuclear cross-sections and the new solar composition. In Table4, we list the results for neutrino fluxes for the up-to-date SSMs SFII-GS98 and SFII-AGSS09. For comparison, we include, in the last column, results from the BP04 SSM [76].Table 4
SSM predictions for solar neutrino fluxes (second and third columns) and solar neutrino fluxes (fourth column) inferred from all available neutrino data. Units are, incm-2s-1, as usual: 1010(pp),109 (7Be), 108 (pep,13N, 15O) 106 (8B, 17F), and 103(hep). Note that the limit on the fluxes relative to the CNO cycle do not contain yet the information coming from recent Borexino result [74]. A revised analysis including these data is in progress.
Flux
SFII-GS98
SFII-AGSS09
Solar
BP04
pp
5.98
(
1
±
0.006
)
6.03
(
1
±
0.006
)
6.05
(
1
-
0.011
+
0.003
)
5.94
(
1
±
0.01
)
pep
1.44
(
1
±
0.012
)
1.47
(
1
±
0.012
)
1.46
(
1
-
0.014
+
0.010
)
1.40
(
1
±
0.02
)
hep
8.04
(
1
±
0.30
)
8.31
(
1
±
0.30
)
18
(
1
-
0.5
+
0.4
)
7.8
(
1
±
0.16
)
7
Be
5.00
(
1
±
0.07
)
4.56
(
1
±
0.07
)
4.82
(
1
-
0.04
+
0.05
)
4.86
(
1
±
0.12
)
8
B
5.58
(
1
±
0.13
)
4.59
(
1
±
0.13
)
5.00
(
1
±
0.03
)
5.79
(
1
±
0.23
)
13
N
2.96
(
1
±
0.15
)
2.17
(
1
±
0.13
)
≤6.7
5.71
(
1
±
0.36
)
15
O
2.23
(
1
±
0.16
)
1.56
(
1
±
0.15
)
≤3.2
5.03
(
1
±
0.41
)
17
F
5.52
(
1
±
0.18
)
3.40
(
1
±
0.16
)
≤5.9
5.91
(
1
±
0.44
)
χ
2
/
P
agr
3.5/90%
3.4/90%
—
—The most striking difference is the large reduction in the13N and 15O fluxes between the SFII-GS98 and BP04 models, which use the same solar composition. This reduction comes as a result of the new determination of S1,14, mostly by the LUNA experiment [77, 78], that has halved its value with respect to previous results (Table 2). If correct, the new expectation value of the combined 13N + 15O fluxes poses an even more challenging task for neutrino experiments to detect CNO fluxes. By comparing fluxes in Table 4 for models computed with the same solar composition (SFII-GS98 and BP04), it can be seen that in terms of flux values, those associated with the pp-chains have not changed much since 2004, despite improvements in the input physics entering solar model calculations. Few percent changes are present and are the result of changes in the nuclear cross-sections discussed before and also of the new OP radiative opacities. This is an encouraging situation; it implies that neutrino fluxes are robust predictions of solar models and, as experimental data on solar neutrinos accumulate, it will be possible to start fulfilling the initial goal posed by Davis and Bahcall: to use solar neutrinos to learn about the solar interior.In Figure2, we show the distribution of the solar neutrino fluxes as a function of solar radius. Together with the electron density profile, provided also by solar models (and neutron density profiles for sterile neutrino studies), these quantities are of fundamental importance for neutrino oscillation studies. It is worth noting that the 13N flux has two components. The larger one is associated with the operation in quasi-steady state of the CN-cycle in the innermost solar core (R<0.1R⊙), and for this reason coincides with the production region of the 15O flux (Figure 2(b), blue and black curves, resp.). This component of the 13N flux, as well as the total 15O flux, is linearly dependent on S1,14. The additional component of the 13N flux comes from the residual burning of 12C by the reactions 12C(p,γ)13N(β+)13C at temperatures not high enough to close the CN-cycle with a proton capture on 14N. This component is completely independent of S1,14. The careful reader will notice that the ratio of 13N and 15O fluxes is different in the SFII-GS98 and BP04 models, despite having the same solar composition. Whereas the added 13N +15O neutrino flux is linearly proportional to the C + N abundance in the solar core and also linearly proportional to S1,14, this degeneracy can be broken, at least theoretically, if the two fluxes can be experimentally isolated from one another.Normalized production profiles of solar neutrinos as a function of solar radius.
(a)
(b)The impact of thelow-Z solar composition on the production of solar neutrinos can be grasped by comparing results of models SFII-GS98 and SFII-AGSS09 shown in Table 4. As stated before, metals shape the solar structure through the radiative opacity. The lower abundance of metals in the AGSS09 composition is responsible for a reduction of the temperature in the solar core of about 1%. Because of the extreme temperature sensitivity of some of the neutrino fluxes this is enough to produce large changes in the total fluxes. The most extreme case is, of course, 8B, with the SFII-AGSS09 value being ~20% smaller. For 7Be the reduction is of ~9%.Given the small uncertainties in the experimental determination of these fluxes, it would be tempting to think these neutrino fluxes have the potential to discriminate between the two flavors of solar composition and contribute, in this way, to the solution of the solar abundance problem. As can be seen in Table4, unfortunately, the 7Be and 8B fluxes determined from experiments lie almost right in between the high-Z and low-Z models.In any case, since it is known thatlow-Z solar models do not reproduce well the solar structure as discussed in the previous section, it is dangerous to extract conclusions from comparing neutrino fluxes of this model to experimental results. Regardless of what the solution to the solar abundance problem is, since it will modify the solar interior structure, it will also change the expected values for the neutrino fluxes. In this regard, CNO fluxes are particularly interesting. Although they are of course affected by temperature variations to a comparable degree as the 8B flux is, they carry an extra linear dependence on the solar composition that is not related to temperature variations (The 17F flux is linearly dependent on O, but unfortunately the flux is too low to be detectable with current experimental capabilities.) Of particular interest is the linear dependence of the 13N and 15O fluxes on the combined C + N abundance. It is this dependence that enhances their capability as a diagnostic tool. In fact, differences between SFII-GS98 and SFII-AGSS09 models for these two fluxes are of the order of 30% (taking SFII-GS98 as reference) and, what is more important, a large contribution to these differences does not have an origin on temperature differences between the models.The last row in Table4 shows the results of an χ2 test for the two models against the solar fluxes also shown in the table. It is clear that both SSMs give a very good agreement with current data. We emphasize again, however, that the four fluxes that are currently well determined from data and the luminosity constraint, depending on the solar composition only in an indirect manner. Experimental determination of the combined 13N + 15O flux will therefore provide qualitatively new information on the solar structure and composition. In fact, one can take advantage of the similar response to temperature variations that CNO fluxes and the 8B flux has. This has been exploited [79] to develop a very simple method to determine the solar core C + N abundance that minimizes environmental uncertainties in solar models (i.e., sources of uncertainty that affect the solar core temperature). The idea is simple: the temperature dependences are cancelled out by using an appropriate ratio between the 8B and the combined 13N + 15O fluxes where SSM fluxes only act as normalization values and the overall scale is determined by an actual 8B flux measurement. The only additional requirement is that a measurement of the combined 13N + 15O flux becomes available. The current upper limit on this combined flux from Borexino [74] places an upper limit on the C + N central mass fraction of XC+N<0.072. Results for the SFII-GS98 and SFII-AGSS09 models are XC+N=0.048 and 0.039, respectively.


#### 3.3.2. Uncertainties

Uncertainties in the model predictions of solar neutrino fluxes are given in Table4. For deriving the total uncertainty basically two approaches can be used. On one hand, all contributions of uncertainty can be treated simultaneously by doing a Monte Carlo simulation [80]. The advantage is that intrinsic nonlinearities are captured in the total error. The disadvantage is that individual contributions to the total uncertainty are hardwired in the final result and cannot be disentangled. Fortunately, for the current level of uncertainties entering SSM calculations, nonlinearities seem to be negligible and the total uncertainty in neutrino fluxes can be obtained (adding quadratically) from individual contributions. To compute the latter, the expansion of fluxes as a product of power laws in the input parameters [43] around central values is a widely used, practical, insightful, and accurate approach. Uncertainties in the model fluxes listed in Table 4 have been obtained in this way.The most important change introduced in the estimation of uncertainties is related to the treatment of the solar composition. Up until the BP04 model [76], the uncertainty in the solar composition was taken into account by considering variations of the total solar metallicity (to be more precise, changes in the (Z/X)⊙ value used to construct SSMs). This leads to an overestimation of the neutrino uncertainties. The reason is that metals dominating the error budget in (Z/X)⊙ (C, N, O, and Ne) have, at most, a moderate impact on the neutrino fluxes because of their small contribution to the radiative opacity, and therefore a rather small impact on temperature, in the region where most neutrinos are produced. On the other hand, elements such as Fe, S, and Si are second-order in determining (Z/X)⊙ but play a fundamental role as sources of opacity in the solar core. It is important, therefore, to treat metal uncertainties individually [81]. Of course, in the case of the CNO fluxes the situation is different because CNO elements catalyze the CNO-bicycle and this overimposes an almost linear dependence of the 13N and 15O on the C + N content of the solar and a similar dependence of 17F on the O abundance. The uncertainties in the neutrino fluxes given for the SFII-GS98 and SFII-AGSS09 SSMs have been computed using the uncertainties for each relevant element given in the original publications [46, 50]. As a result, for either family of solar models, that is, high-Z or low-Z models, the solar composition is not the dominant source of uncertainty for any of the fluxes of the pp-chains. In the case of the CNO fluxes, the linear dependence mentioned above is the dominant source of uncertainty: the combined C + N abundance contributes to a 12% uncertainty for both the 13N and the 15O fluxes, and the O abundance to 15% in the 17F flux.In the case of the noncomposition uncertainties, the situation has improved in some cases thanks to more precise measurements of nuclear reaction rates. This is the case, in particular, for the3He(4He,γ)7Be reaction, which now contributes only 4.7% and 4.5% of the total uncertainty in the 7Be and 8B fluxes, respectively. For comparison, the analogous contributions in the BP04 model were 8.0% and 7.5% [76]. Significant progress has also been achieved regarding 14N(p,γ)15O, which now introduces uncertainties of only 5% and 7% in the 13N and 15O fluxes, half the amount it did in 2004. An important contribution to the uncertainty in the 8B flux now comes from 7Be(p,γ)8B because the uncertainty of this reaction has been revised upwards [55]. Even if the uncertainty in this rate is now smaller than in SFI (see Table 2), it is larger than that used for the BP04 model, which was taken considering only one experimental result for this reaction.While progress has been done in some cases, others have not seen much development, particularly diffusion and the delicate issue of radiative opacities. In Table5, we give the individual contributions to flux uncertainties for the most relevant sources. The reader can compare directly to the situation in 2004 [76].Table 5
Percentage contribution of selected individual sources of uncertainty to the neutrino fluxes.
S
11
S33
S34
S17
S1,14
Opac
Diff
pp
0.1
0.1
0.3
0.0
0.0
0.2
0.2
pep
0.2
0.2
0.5
0.0
0.0
0.7
0.2
hep
0.1
2.3
0.4
0.0
0.0
1.0
0.5
7
Be
1.1
2.2
4.7
0.0
0.0
3.2
1.9
8
B
2.7
2.1
4.5
7.7
0.0
6.9
4.0
13
N
2.1
0.1
0.3
0.0
5.1
3.6
4.9
15
O
2.9
0.1
0.2
0.0
7.2
5.2
5.7
17
F
3.1
0.1
0.2
0.0
0.0
5.8
6.0


## 3.1. Input Physics and Parameters

### 3.1.1. Solar Surface Composition

The constraint imposed by the surface metallicity of the Sun or, more precisely, the surface metal-to-hydrogen ratio(Z/X)⊙ is critical in the construction of solar models. The reason is that, aside from the 10 to 15% change in this value due to the action of gravitational settling, (Z/X)⊙ determines almost directly the metallicity of solar models. As for any other star, the metal content in the Sun has a fundamental role in its structure through its contribution to the radiative opacity κ, which determines, in turn, the temperature gradient in the radiative solar interior. It is important, in fact, that the abundance of individual metals are accurately determined, because different elements contribute to the radiative opacities in different regions of the Sun.The abundance of metals in the solar surface has to be determined or inferred from a variety of sources: photospheric abundances from solar spectra, chemical analysis of primitive meteorites, emission lines from the solar corona, and composition of the solar wind [44]. While meteoritic abundances are the most precisely determined, at 2/3 of the solar metallicity is composed by the volatile elements C, N, and O and can only be determined from the analysis of the solar spectrum.Over the last decade, the development of three-dimensional radiation hydrodynamic (3D RHD) models of the solar atmosphere has prompted a thorough revision of the solar composition determined from the solar spectrum. These 3D RHD models of the solar atmosphere capture the dynamics of convection and its interaction with the radiation field and are able to reproduce features such as the solar granulation pattern, observed limb-darkening, and asymmetries in the shapes of spectral lines [45]. The structure of the solar model atmospheres derived by different groups are nicely consistent with each other, adding to the credibility of the models. Newly derived spectroscopic abundances rely on the 3D atmosphere model or more appropriately on a one-dimensional model obtained from a suitably averaged 3D model, as the background on top of which detailed radiative transfer and line formation calculations are performed a posteriori. It is this second step that leads, finally, to the determination of the abundances of the different elements. The most thorough and consistent determination of the solar photospheric abundances based on 3D model atmospheres has been presented by Asplund and collaborators [46, 47], although the revision on key elements like oxygen was initially published already in 2001 [48]. In addition to using 3D RHD atmosphere models, nonlocal thermodynamic equilibrium has been taken into account when computing the line formation for some key elements such as C, N, and O. Also, and this is of particular importance for oxygen, blends in the solar spectrum that had been previously unnoticed were identified and taken into account in the determination of abundances. The most relevant result in the context of solar models and neutrinos is that abundances of CNO elements (also Ne, but this is mostly because its abundance ratio to oxygen is assumed fixed) have been revised down by 30% to 40%. Combining the abundance of all metals, the present-day metal-to-hydrogen ratio that has been obtained is (Z/X)⊙=0.0178 [46]. This represents a large decrease in comparison with previously accepted values, 0.0245 [49] and 0.0229 [50], that have been widely used in solar modeling. We note, however, that results by Asplund have not been unchallenged. In fact, also based on 3D RHD model solar atmospheres, larger CNO abundances have been derived [51] to yield (Z/X)⊙=0.0209, much closer to older determinations. Discrepancies between authors seem to have their origin at the preferred set of spectral lines each group uses and on using either a spectral synthesis or equivalent width techniques to determine the final abundances.In the last decade, there have been two flavors in SSM calculations. In one case, ahigh solar metallicity from older determinations [49, 50] is adopted; we will generically refer to these models as high-Z solar models. In the other case, a low(Z/X)⊙ [46, 47] is taken from and we refer to these, not surprisingly, as the low-Z solar models. Differences in the structure of high-Z and low-Z models are readily noticeable in quantities such as the internal sound speed and density profiles, the depth of the solar convective envelope, and the surface helium abundance among others. The deficit that low-Z models have in matching helioseismic constraints has been named the solar abundance problem in the literature, in clear analogy to the solar neutrino problem. We discuss it in some detail in Section 3.2.


### 3.1.2. Radiative Opacities

The most widely used calculations of atomic radiative opacities, appropriate for solar interiors, are those from OPAL [52]. However, the opacity project (OP) released in 2005 a completely independent set of atomic radiative opacities for stellar interiors [53]. In the case of the solar radiative interior, differences between OPAL and OP Rosseland mean opacities are of the order of a few percent, with OP being larger by about 3% at the base of the convective zone and 1% to 2% smaller in the central regions (see Figure 7 in [53]). At low temperatures neither OP nor OPAL atomic opacities are adequate, because the possible formation of molecules have to be taken into account and, therefore, they have to be complemented by low-temperature opacities [54]. However, due to the relatively high solar temperature, their influence in the properties of solar models is rather limited.


### 3.1.3. Nuclear Reactions Cross-Sections

Experimental and theoretical work on the determination of nuclear cross-sections have been very active fields with a strong impact on solar model predictions of solar neutrino fluxes (A nonresonant charged-particle induced reaction cross-section can be written asσ(E)=(S(E)/E)exp[-2πη(E)] where η(E)=Z1Z2α/v is the Sommerfeld parameters, v=(2E/μ), α the fine structure constant in natural units, and μ the reduced mass of the interacting nuclei. The nuclear physics is isolated in S(E), the astrophysical or S-factor, a slowly varying function of energy that can be more accurately extrapolated from experimental data down to the energy of the Gamow peak.) Recently, a set of recommended rates and uncertainties, expressed through the S-factor for all the reactions both in the pp-chains and CNO-bicycle that are relevant to solar modeling and neutrino production, has been published (Solar Fusion II, [55], hereafter SFII). The results presented in SFII reflect the progress made in laboratory and theoretical nuclear astrophysics over the last decade, since the publication of the seminal Solar Fusion I (SFI) article [56]. Unfortunately, for reasons of space, here we cannot review in detail every reaction. Instead, we provide in Table 2 the standard S-factors at zero energy, S(0), and the uncertainties recommended in SFII for the most relevant reactions. For comparison, with results from SFI are also shown. The impact of changes in key reactions on the production of neutrino fluxes is discussed in Section 3.3. The reader is referred to the SFII paper and references therein for details on the experimental and theoretical developments in nuclear astrophysics related to the Sun during the last decade.Table 2
Standard astrophysical factors and uncertainties for key nuclear reactions in thepp-chains and CNO-bicycle. SFII represents the state-of-the-art [55]; SFI [56] shows, for comparison, the situation around 1998.
Reaction
SFII
SFI
S
(
0
)
[
keV
b
]
S
(
0
)
[
keV
b
]
S
11
p
(
p
,
e
+
ν
e
)
d
4.01
×
1
0
-
22
(
1
±
0.010
)
4.00
×
1
0
-
22
(
1
±
0.005
)
S
33
3

He
(
3
He
,
2
p
)
4
He
5.21
×
1
0
3
(
1
±
0.052
)
5.4
×
1
0
3
(
1
±
0.074
)
S
34
3

He
(
4
He
,
γ
)
7
Be
5.6
×
1
0
-
1
(
1
±
0.054
)
5.3
×
1
0
-
1
(
1
±
0.094
)
Shep
3

He
(
p
,
e
+
ν
e
)
4
He
8.6
×
1
0
-
20
(
1
±
0.30
)
2.3
×
1
0
-
20
S
17
7

Be
(
p
,
γ
)
8
B
2.08
×
1
0
-
2
(
1
±
0.077
)
1.9
×
1
0
-
2
(
1
-
0.10
+
0.20
)
S
1,14
14

N
(
p
,
γ
)
15
O
1.66
(
1
±
0.072
)
3.5
(
1
-
0.46
+
0.11
)


## 3.1.1. Solar Surface Composition

The constraint imposed by the surface metallicity of the Sun or, more precisely, the surface metal-to-hydrogen ratio(Z/X)⊙ is critical in the construction of solar models. The reason is that, aside from the 10 to 15% change in this value due to the action of gravitational settling, (Z/X)⊙ determines almost directly the metallicity of solar models. As for any other star, the metal content in the Sun has a fundamental role in its structure through its contribution to the radiative opacity κ, which determines, in turn, the temperature gradient in the radiative solar interior. It is important, in fact, that the abundance of individual metals are accurately determined, because different elements contribute to the radiative opacities in different regions of the Sun.The abundance of metals in the solar surface has to be determined or inferred from a variety of sources: photospheric abundances from solar spectra, chemical analysis of primitive meteorites, emission lines from the solar corona, and composition of the solar wind [44]. While meteoritic abundances are the most precisely determined, at 2/3 of the solar metallicity is composed by the volatile elements C, N, and O and can only be determined from the analysis of the solar spectrum.Over the last decade, the development of three-dimensional radiation hydrodynamic (3D RHD) models of the solar atmosphere has prompted a thorough revision of the solar composition determined from the solar spectrum. These 3D RHD models of the solar atmosphere capture the dynamics of convection and its interaction with the radiation field and are able to reproduce features such as the solar granulation pattern, observed limb-darkening, and asymmetries in the shapes of spectral lines [45]. The structure of the solar model atmospheres derived by different groups are nicely consistent with each other, adding to the credibility of the models. Newly derived spectroscopic abundances rely on the 3D atmosphere model or more appropriately on a one-dimensional model obtained from a suitably averaged 3D model, as the background on top of which detailed radiative transfer and line formation calculations are performed a posteriori. It is this second step that leads, finally, to the determination of the abundances of the different elements. The most thorough and consistent determination of the solar photospheric abundances based on 3D model atmospheres has been presented by Asplund and collaborators [46, 47], although the revision on key elements like oxygen was initially published already in 2001 [48]. In addition to using 3D RHD atmosphere models, nonlocal thermodynamic equilibrium has been taken into account when computing the line formation for some key elements such as C, N, and O. Also, and this is of particular importance for oxygen, blends in the solar spectrum that had been previously unnoticed were identified and taken into account in the determination of abundances. The most relevant result in the context of solar models and neutrinos is that abundances of CNO elements (also Ne, but this is mostly because its abundance ratio to oxygen is assumed fixed) have been revised down by 30% to 40%. Combining the abundance of all metals, the present-day metal-to-hydrogen ratio that has been obtained is (Z/X)⊙=0.0178 [46]. This represents a large decrease in comparison with previously accepted values, 0.0245 [49] and 0.0229 [50], that have been widely used in solar modeling. We note, however, that results by Asplund have not been unchallenged. In fact, also based on 3D RHD model solar atmospheres, larger CNO abundances have been derived [51] to yield (Z/X)⊙=0.0209, much closer to older determinations. Discrepancies between authors seem to have their origin at the preferred set of spectral lines each group uses and on using either a spectral synthesis or equivalent width techniques to determine the final abundances.In the last decade, there have been two flavors in SSM calculations. In one case, ahigh solar metallicity from older determinations [49, 50] is adopted; we will generically refer to these models as high-Z solar models. In the other case, a low(Z/X)⊙ [46, 47] is taken from and we refer to these, not surprisingly, as the low-Z solar models. Differences in the structure of high-Z and low-Z models are readily noticeable in quantities such as the internal sound speed and density profiles, the depth of the solar convective envelope, and the surface helium abundance among others. The deficit that low-Z models have in matching helioseismic constraints has been named the solar abundance problem in the literature, in clear analogy to the solar neutrino problem. We discuss it in some detail in Section 3.2.


## 3.1.2. Radiative Opacities

The most widely used calculations of atomic radiative opacities, appropriate for solar interiors, are those from OPAL [52]. However, the opacity project (OP) released in 2005 a completely independent set of atomic radiative opacities for stellar interiors [53]. In the case of the solar radiative interior, differences between OPAL and OP Rosseland mean opacities are of the order of a few percent, with OP being larger by about 3% at the base of the convective zone and 1% to 2% smaller in the central regions (see Figure 7 in [53]). At low temperatures neither OP nor OPAL atomic opacities are adequate, because the possible formation of molecules have to be taken into account and, therefore, they have to be complemented by low-temperature opacities [54]. However, due to the relatively high solar temperature, their influence in the properties of solar models is rather limited.


## 3.1.3. Nuclear Reactions Cross-Sections

Experimental and theoretical work on the determination of nuclear cross-sections have been very active fields with a strong impact on solar model predictions of solar neutrino fluxes (A nonresonant charged-particle induced reaction cross-section can be written asσ(E)=(S(E)/E)exp[-2πη(E)] where η(E)=Z1Z2α/v is the Sommerfeld parameters, v=(2E/μ), α the fine structure constant in natural units, and μ the reduced mass of the interacting nuclei. The nuclear physics is isolated in S(E), the astrophysical or S-factor, a slowly varying function of energy that can be more accurately extrapolated from experimental data down to the energy of the Gamow peak.) Recently, a set of recommended rates and uncertainties, expressed through the S-factor for all the reactions both in the pp-chains and CNO-bicycle that are relevant to solar modeling and neutrino production, has been published (Solar Fusion II, [55], hereafter SFII). The results presented in SFII reflect the progress made in laboratory and theoretical nuclear astrophysics over the last decade, since the publication of the seminal Solar Fusion I (SFI) article [56]. Unfortunately, for reasons of space, here we cannot review in detail every reaction. Instead, we provide in Table 2 the standard S-factors at zero energy, S(0), and the uncertainties recommended in SFII for the most relevant reactions. For comparison, with results from SFI are also shown. The impact of changes in key reactions on the production of neutrino fluxes is discussed in Section 3.3. The reader is referred to the SFII paper and references therein for details on the experimental and theoretical developments in nuclear astrophysics related to the Sun during the last decade.Table 2
Standard astrophysical factors and uncertainties for key nuclear reactions in thepp-chains and CNO-bicycle. SFII represents the state-of-the-art [55]; SFI [56] shows, for comparison, the situation around 1998.
Reaction
SFII
SFI
S
(
0
)
[
keV
b
]
S
(
0
)
[
keV
b
]
S
11
p
(
p
,
e
+
ν
e
)
d
4.01
×
1
0
-
22
(
1
±
0.010
)
4.00
×
1
0
-
22
(
1
±
0.005
)
S
33
3

He
(
3
He
,
2
p
)
4
He
5.21
×
1
0
3
(
1
±
0.052
)
5.4
×
1
0
3
(
1
±
0.074
)
S
34
3

He
(
4
He
,
γ
)
7
Be
5.6
×
1
0
-
1
(
1
±
0.054
)
5.3
×
1
0
-
1
(
1
±
0.094
)
Shep
3

He
(
p
,
e
+
ν
e
)
4
He
8.6
×
1
0
-
20
(
1
±
0.30
)
2.3
×
1
0
-
20
S
17
7

Be
(
p
,
γ
)
8
B
2.08
×
1
0
-
2
(
1
±
0.077
)
1.9
×
1
0
-
2
(
1
-
0.10
+
0.20
)
S
1,14
14

N
(
p
,
γ
)
15
O
1.66
(
1
±
0.072
)
3.5
(
1
-
0.46
+
0.11
)


## 3.2. Solar Models: Helioseismology

Helioseismology, the study of the natural oscillations of the Sun, provides a unique tool to determine the structure of the solar interior. The 90s witnessed a rapid development of helioseismic observations and analysis techniques, which led, in very few years, to an accurate characterization of the solar interior [57]. The agreement between SSMs and helioseismic inferences of the solar structure [35, 58] provided a strong support to the accuracy with which SSMs could predict the 8B neutrino flux and, therefore, a strong indication, before Kamland and SNO results found evidence of neutrino flavor oscillations, that the solution to the solar neutrino problem had to be found in the realm of particle physics.In the context of the present paper, the most relevant results from helioseismology are the following (The Sun is characterized by an outer region where energy is transported by convection. The boundary between this region, located atRCZ, and the radiative interior can be accurately located by helioseismology because the discontinuity in the slope of the temperature gradient across this boundary leaves its imprint in the solar sound speed profile. The depth of the envelope can be located by helioseismology because properties of solar oscillations are sensitive to the derivative of the sound speed as a function of depth.) The depth of the convective envelope is RCZ=0.713±0.001 R⊙ [59] and the surface helium abundance YS=0.2485±0.0034 [60]. The sound speed differences between the Sun and a reference solar model can be obtained by inversion from the oscillation frequencies with a formal error of a few parts per 10-4 for most of the solar interior 0.07≲R/R⊙≲0.95 [61, 62]. Most recently, using a time series 4752 days long from the Birmingham Solar Oscillation Network, improved results on the sound speed in the solar core have been obtained [63]. The density profile can also be determined from the inversion of frequencies, but with worse precision than for the sound speed, and we therefore assign to it a secondary role in constraining the solar structure.As mentioned previously, metals determine to a large extent the radiative opacity in the solar interior and, in this way, define the temperature stratification from below of the convective envelope inwards, to the solar center. At the base of the convective zone, for example, metals are responsible for about 70% of the total radiative opacity with O, Fe, and Ne being the main contributors. In the solar core, where light metals are completely ionized, the contribution from Fe and, to a lesser extent Ni, Si, and S, is still above 30%. In view of this, it is not surprising that the low CNO and Ne abundances determined from 3D model atmospheres have a strong impact on the structure of the solar interior.It has been clear since initial works wherelow-Z SSMs were presented that low (Z/X)⊙ values posed a problem, later named the solar abundance problem, for solar modeling [60, 67–69]. In short, all helioseismic predictions of these models are in disagreement with observations. On the other hand, high-Z SSMs have consistently reproduced earlier success [58]. The solar abundance problem represents the incompatibility between the best solar atmosphere and interior models available [70]. In this paper, we will base the presentation and discussion of results on the most up-to-date standard solar models that we identify as SFII-GS98 and SFII-AGSS09 [64], representative of high-Z and low-Z SSM families defined in Section 3.1, respectively. With the exception made on small quantitative variations, results based on these models are extensible to results for all SSMs available in the literature corresponding to each of the two families.The most important characteristics of the SFII-GS98 and SFII-AGSS09 models are summarized in Table3. Helioseismic constraints are also included for comparison when appropriate. The disagreement between SFII-AGSS09 and helioseismic data is evident in the surface metallicity and helium abundances, ZS and YS, and in the depth of the convective envelope RCZ. A similar conclusion could be drawn from comparing Yini; however, the determination of the solar value of Yini [71] depends strongly on the seismic value for YS and, therefore, it is not an independent constraint. When model uncertainties are included, the discrepancy between SFII-AGSS09 and seismic results are, for each of the quantities mentioned above, of the order 3 to 4-σ [72]. On the contrary, the SFII-GS98 model performs very well, within 1-σ, when model uncertainties are accounted for.Table 3
Main characteristics of SSMs representative ofhigh-Z (GS98) and low-Z (AGSS09) solar compositions. Models have been computed including the most up-to-date input physics [64]. Helioseismic constraints are given when available. See text for details.
SFII-GS98
SFII-AGSS09
Helioseismology
(
Z
/
X
)
⨀
0.0229
0.0178
—
Z
S
0.0170
0.0134
0.0172
±
0.002 [65]
Y
S
0.2429
0.2319
0.2485
±
0.0034 [60]
R
CZ
/
R
⨀
0.7124
0.7231
0.713
±
0.001 [59]
〈
δ
c
/
c
〉
0.0009
0.0037
—
〈
δ
ρ
/
ρ
〉
0.011
0.040
—
Z
C
0.0200
0.0159
—
Y
C
0.6333
0.6222
—
〈
μ
C
〉
0.7200
0.7136
0.7225
±
0.0014 [66]
Z
ini
0.0187
0.0149
—
Y
ini
0.2724
0.2620
—Very explicit manifestations of the solar abundance problem are shown in the plots in Figure1, where degradation in the sound speed and density profiles found in low-Z SSMs are clearly evident. Particularly the peak in the sound speed profile differences found right below the convective zone is 4 times larger in the low-Z SFII-AGSS09 than in the high-Z SFII-GS98 model. The reason is the wrong location of RCZ in the model, caused by the lower opacity which, in turn, is due to the low abundance of metals. The density profile also shows very large discrepancies, but they are less telling. Density inversions include as a constraint the known value of the solar mass and for this reason small differences in the core, where density is large, translate into the large difference seen in the outer envelope. The average rms in the sound speed and density differences, 〈δc/c〉 and 〈δρ/ρ〉, also show that low-Z models are about 4 times worse than high-Z models.Figure 1
Sound speed and density relative differences between solar models and the Sun as determined from helioseismic inversions [72]. The convective envelope is depicted by the grey area.Low-degree helioseismology provides useful information about the solar innermost regions. Specific combinations of mode frequencies enhance the signal that the structure of the solar core imprints on the oscillation pattern [73]. This has been used to determine the mean molecular weight averaged over the innermost 20% solar core [66], 〈μC〉 in Table 3. Comparison with SSMs results shows that 〈μC〉 is too low in low-Z models as a result of the lower helium abundance (YC). This is due to the lower temperature in the solar core and the constraint imposed by the solar luminosity. The decreased nuclear energy production originated by a smaller core temperature has to be compensated by an increased hydrogen mass fraction, therefore leading to a lower molecular weight. It is interesting to note this puts a stringent constraint in the amount of rotational mixing that can take place in the solar core if the low-Z abundances are correct, since any mixing would lower the molecular weight even more, by bringing fresh hydrogen from outer regions, and make the agreement with helioseismic data worse.The current situation regarding SSMs and their performance against helioseismic inferences on the solar structure can be summarized as follows. SSMs that use solar abundances derived from 1D model atmospheres [49, 50], that is, high-Z models, reproduce overall the most important seismic constraints. Improvements in the input physics, for example, radiative opacities and nuclear reaction rates, that have occurred over the last 10 years introduce only small changes to the solar structure as seen by helioseismology. On the other hand, the solar abundance problem arises if the solar surface composition used to construct SSMs are derived from the most sophisticated 3D RHD solar model atmospheres. The family of low-Z SSMs does not match any helioseismic constraint.Have we reached the limit where the paradigm of the SSM is not good enough as a model of the solar interior? Are the 3D-based determinations of solar abundances systematically underestimating the metallicity of the solar surface? Does the microscopic input physics in solar models, for example, radiative opacities, need to be thoroughly revised? It is not possible to advance answers to these questions, but solar neutrino experiments can play an important role in guiding the research towards the solution of the solar abundance problem. In the next section, we discuss the current status on the theoretical predictions of solar neutrino fluxes and the prospects of using solar neutrinos to constraint the properties of the solar core.


## 3.3. Solar Models: Neutrino Fluxes

### 3.3.1. Production

Based on theoretical arguments and indirect evidence, it has long been believed that the source of energy of the Sun is the conversion of protons into helium,4p→He4+2e++2νe+γ. The original quest for solar neutrinos was indeed the search for the experimental confirmation of this hypothesis (Under peculiar conditions reached in advanced phases of stellar evolution, hydrogen can be converted into helium by other cycles like the NaMg-cycle. While important for nucleosynthesis or intermediate mass elements, these processes are not energetically relevant.) In more detail, hydrogen burning in the Sun (and in all other hydrogen-burning stars) takes place either through the pp-chains or the CNO-bicycle [43, 75]. Proton fusion through the pp-chains is a primary process because only protons need to be present in the star. On the contrary, the CNO-bicycle is secondary because the proton fusion relies on, and is regulated by, the abundance of C, N, and O which act as catalyzers. This qualitative difference is very important, since it renders neutrino fluxes from the CNO-bicyle a very good diagnostic tool to study properties of the solar core, particularly its composition, as it will be discussed below. A general discussion on the production of solar neutrinos is out of the scope of the present paper, but can be found elsewhere [43].SSM calculations of neutrino fluxes have been affected by developments in the input physics discussed in previous sections. The two areas that have the strongest impact on the neutrino fluxes predicted by models are changes in nuclear cross-sections and the new solar composition. In Table4, we list the results for neutrino fluxes for the up-to-date SSMs SFII-GS98 and SFII-AGSS09. For comparison, we include, in the last column, results from the BP04 SSM [76].Table 4
SSM predictions for solar neutrino fluxes (second and third columns) and solar neutrino fluxes (fourth column) inferred from all available neutrino data. Units are, incm-2s-1, as usual: 1010(pp),109 (7Be), 108 (pep,13N, 15O) 106 (8B, 17F), and 103(hep). Note that the limit on the fluxes relative to the CNO cycle do not contain yet the information coming from recent Borexino result [74]. A revised analysis including these data is in progress.
Flux
SFII-GS98
SFII-AGSS09
Solar
BP04
pp
5.98
(
1
±
0.006
)
6.03
(
1
±
0.006
)
6.05
(
1
-
0.011
+
0.003
)
5.94
(
1
±
0.01
)
pep
1.44
(
1
±
0.012
)
1.47
(
1
±
0.012
)
1.46
(
1
-
0.014
+
0.010
)
1.40
(
1
±
0.02
)
hep
8.04
(
1
±
0.30
)
8.31
(
1
±
0.30
)
18
(
1
-
0.5
+
0.4
)
7.8
(
1
±
0.16
)
7
Be
5.00
(
1
±
0.07
)
4.56
(
1
±
0.07
)
4.82
(
1
-
0.04
+
0.05
)
4.86
(
1
±
0.12
)
8
B
5.58
(
1
±
0.13
)
4.59
(
1
±
0.13
)
5.00
(
1
±
0.03
)
5.79
(
1
±
0.23
)
13
N
2.96
(
1
±
0.15
)
2.17
(
1
±
0.13
)
≤6.7
5.71
(
1
±
0.36
)
15
O
2.23
(
1
±
0.16
)
1.56
(
1
±
0.15
)
≤3.2
5.03
(
1
±
0.41
)
17
F
5.52
(
1
±
0.18
)
3.40
(
1
±
0.16
)
≤5.9
5.91
(
1
±
0.44
)
χ
2
/
P
agr
3.5/90%
3.4/90%
—
—The most striking difference is the large reduction in the13N and 15O fluxes between the SFII-GS98 and BP04 models, which use the same solar composition. This reduction comes as a result of the new determination of S1,14, mostly by the LUNA experiment [77, 78], that has halved its value with respect to previous results (Table 2). If correct, the new expectation value of the combined 13N + 15O fluxes poses an even more challenging task for neutrino experiments to detect CNO fluxes. By comparing fluxes in Table 4 for models computed with the same solar composition (SFII-GS98 and BP04), it can be seen that in terms of flux values, those associated with the pp-chains have not changed much since 2004, despite improvements in the input physics entering solar model calculations. Few percent changes are present and are the result of changes in the nuclear cross-sections discussed before and also of the new OP radiative opacities. This is an encouraging situation; it implies that neutrino fluxes are robust predictions of solar models and, as experimental data on solar neutrinos accumulate, it will be possible to start fulfilling the initial goal posed by Davis and Bahcall: to use solar neutrinos to learn about the solar interior.In Figure2, we show the distribution of the solar neutrino fluxes as a function of solar radius. Together with the electron density profile, provided also by solar models (and neutron density profiles for sterile neutrino studies), these quantities are of fundamental importance for neutrino oscillation studies. It is worth noting that the 13N flux has two components. The larger one is associated with the operation in quasi-steady state of the CN-cycle in the innermost solar core (R<0.1R⊙), and for this reason coincides with the production region of the 15O flux (Figure 2(b), blue and black curves, resp.). This component of the 13N flux, as well as the total 15O flux, is linearly dependent on S1,14. The additional component of the 13N flux comes from the residual burning of 12C by the reactions 12C(p,γ)13N(β+)13C at temperatures not high enough to close the CN-cycle with a proton capture on 14N. This component is completely independent of S1,14. The careful reader will notice that the ratio of 13N and 15O fluxes is different in the SFII-GS98 and BP04 models, despite having the same solar composition. Whereas the added 13N +15O neutrino flux is linearly proportional to the C + N abundance in the solar core and also linearly proportional to S1,14, this degeneracy can be broken, at least theoretically, if the two fluxes can be experimentally isolated from one another.Normalized production profiles of solar neutrinos as a function of solar radius.
(a)
(b)The impact of thelow-Z solar composition on the production of solar neutrinos can be grasped by comparing results of models SFII-GS98 and SFII-AGSS09 shown in Table 4. As stated before, metals shape the solar structure through the radiative opacity. The lower abundance of metals in the AGSS09 composition is responsible for a reduction of the temperature in the solar core of about 1%. Because of the extreme temperature sensitivity of some of the neutrino fluxes this is enough to produce large changes in the total fluxes. The most extreme case is, of course, 8B, with the SFII-AGSS09 value being ~20% smaller. For 7Be the reduction is of ~9%.Given the small uncertainties in the experimental determination of these fluxes, it would be tempting to think these neutrino fluxes have the potential to discriminate between the two flavors of solar composition and contribute, in this way, to the solution of the solar abundance problem. As can be seen in Table4, unfortunately, the 7Be and 8B fluxes determined from experiments lie almost right in between the high-Z and low-Z models.In any case, since it is known thatlow-Z solar models do not reproduce well the solar structure as discussed in the previous section, it is dangerous to extract conclusions from comparing neutrino fluxes of this model to experimental results. Regardless of what the solution to the solar abundance problem is, since it will modify the solar interior structure, it will also change the expected values for the neutrino fluxes. In this regard, CNO fluxes are particularly interesting. Although they are of course affected by temperature variations to a comparable degree as the 8B flux is, they carry an extra linear dependence on the solar composition that is not related to temperature variations (The 17F flux is linearly dependent on O, but unfortunately the flux is too low to be detectable with current experimental capabilities.) Of particular interest is the linear dependence of the 13N and 15O fluxes on the combined C + N abundance. It is this dependence that enhances their capability as a diagnostic tool. In fact, differences between SFII-GS98 and SFII-AGSS09 models for these two fluxes are of the order of 30% (taking SFII-GS98 as reference) and, what is more important, a large contribution to these differences does not have an origin on temperature differences between the models.The last row in Table4 shows the results of an χ2 test for the two models against the solar fluxes also shown in the table. It is clear that both SSMs give a very good agreement with current data. We emphasize again, however, that the four fluxes that are currently well determined from data and the luminosity constraint, depending on the solar composition only in an indirect manner. Experimental determination of the combined 13N + 15O flux will therefore provide qualitatively new information on the solar structure and composition. In fact, one can take advantage of the similar response to temperature variations that CNO fluxes and the 8B flux has. This has been exploited [79] to develop a very simple method to determine the solar core C + N abundance that minimizes environmental uncertainties in solar models (i.e., sources of uncertainty that affect the solar core temperature). The idea is simple: the temperature dependences are cancelled out by using an appropriate ratio between the 8B and the combined 13N + 15O fluxes where SSM fluxes only act as normalization values and the overall scale is determined by an actual 8B flux measurement. The only additional requirement is that a measurement of the combined 13N + 15O flux becomes available. The current upper limit on this combined flux from Borexino [74] places an upper limit on the C + N central mass fraction of XC+N<0.072. Results for the SFII-GS98 and SFII-AGSS09 models are XC+N=0.048 and 0.039, respectively.


### 3.3.2. Uncertainties

Uncertainties in the model predictions of solar neutrino fluxes are given in Table4. For deriving the total uncertainty basically two approaches can be used. On one hand, all contributions of uncertainty can be treated simultaneously by doing a Monte Carlo simulation [80]. The advantage is that intrinsic nonlinearities are captured in the total error. The disadvantage is that individual contributions to the total uncertainty are hardwired in the final result and cannot be disentangled. Fortunately, for the current level of uncertainties entering SSM calculations, nonlinearities seem to be negligible and the total uncertainty in neutrino fluxes can be obtained (adding quadratically) from individual contributions. To compute the latter, the expansion of fluxes as a product of power laws in the input parameters [43] around central values is a widely used, practical, insightful, and accurate approach. Uncertainties in the model fluxes listed in Table 4 have been obtained in this way.The most important change introduced in the estimation of uncertainties is related to the treatment of the solar composition. Up until the BP04 model [76], the uncertainty in the solar composition was taken into account by considering variations of the total solar metallicity (to be more precise, changes in the (Z/X)⊙ value used to construct SSMs). This leads to an overestimation of the neutrino uncertainties. The reason is that metals dominating the error budget in (Z/X)⊙ (C, N, O, and Ne) have, at most, a moderate impact on the neutrino fluxes because of their small contribution to the radiative opacity, and therefore a rather small impact on temperature, in the region where most neutrinos are produced. On the other hand, elements such as Fe, S, and Si are second-order in determining (Z/X)⊙ but play a fundamental role as sources of opacity in the solar core. It is important, therefore, to treat metal uncertainties individually [81]. Of course, in the case of the CNO fluxes the situation is different because CNO elements catalyze the CNO-bicycle and this overimposes an almost linear dependence of the 13N and 15O on the C + N content of the solar and a similar dependence of 17F on the O abundance. The uncertainties in the neutrino fluxes given for the SFII-GS98 and SFII-AGSS09 SSMs have been computed using the uncertainties for each relevant element given in the original publications [46, 50]. As a result, for either family of solar models, that is, high-Z or low-Z models, the solar composition is not the dominant source of uncertainty for any of the fluxes of the pp-chains. In the case of the CNO fluxes, the linear dependence mentioned above is the dominant source of uncertainty: the combined C + N abundance contributes to a 12% uncertainty for both the 13N and the 15O fluxes, and the O abundance to 15% in the 17F flux.In the case of the noncomposition uncertainties, the situation has improved in some cases thanks to more precise measurements of nuclear reaction rates. This is the case, in particular, for the3He(4He,γ)7Be reaction, which now contributes only 4.7% and 4.5% of the total uncertainty in the 7Be and 8B fluxes, respectively. For comparison, the analogous contributions in the BP04 model were 8.0% and 7.5% [76]. Significant progress has also been achieved regarding 14N(p,γ)15O, which now introduces uncertainties of only 5% and 7% in the 13N and 15O fluxes, half the amount it did in 2004. An important contribution to the uncertainty in the 8B flux now comes from 7Be(p,γ)8B because the uncertainty of this reaction has been revised upwards [55]. Even if the uncertainty in this rate is now smaller than in SFI (see Table 2), it is larger than that used for the BP04 model, which was taken considering only one experimental result for this reaction.While progress has been done in some cases, others have not seen much development, particularly diffusion and the delicate issue of radiative opacities. In Table5, we give the individual contributions to flux uncertainties for the most relevant sources. The reader can compare directly to the situation in 2004 [76].Table 5
Percentage contribution of selected individual sources of uncertainty to the neutrino fluxes.
S
11
S33
S34
S17
S1,14
Opac
Diff
pp
0.1
0.1
0.3
0.0
0.0
0.2
0.2
pep
0.2
0.2
0.5
0.0
0.0
0.7
0.2
hep
0.1
2.3
0.4
0.0
0.0
1.0
0.5
7
Be
1.1
2.2
4.7
0.0
0.0
3.2
1.9
8
B
2.7
2.1
4.5
7.7
0.0
6.9
4.0
13
N
2.1
0.1
0.3
0.0
5.1
3.6
4.9
15
O
2.9
0.1
0.2
0.0
7.2
5.2
5.7
17
F
3.1
0.1
0.2
0.0
0.0
5.8
6.0


## 3.3.1. Production

Based on theoretical arguments and indirect evidence, it has long been believed that the source of energy of the Sun is the conversion of protons into helium,4p→He4+2e++2νe+γ. The original quest for solar neutrinos was indeed the search for the experimental confirmation of this hypothesis (Under peculiar conditions reached in advanced phases of stellar evolution, hydrogen can be converted into helium by other cycles like the NaMg-cycle. While important for nucleosynthesis or intermediate mass elements, these processes are not energetically relevant.) In more detail, hydrogen burning in the Sun (and in all other hydrogen-burning stars) takes place either through the pp-chains or the CNO-bicycle [43, 75]. Proton fusion through the pp-chains is a primary process because only protons need to be present in the star. On the contrary, the CNO-bicycle is secondary because the proton fusion relies on, and is regulated by, the abundance of C, N, and O which act as catalyzers. This qualitative difference is very important, since it renders neutrino fluxes from the CNO-bicyle a very good diagnostic tool to study properties of the solar core, particularly its composition, as it will be discussed below. A general discussion on the production of solar neutrinos is out of the scope of the present paper, but can be found elsewhere [43].SSM calculations of neutrino fluxes have been affected by developments in the input physics discussed in previous sections. The two areas that have the strongest impact on the neutrino fluxes predicted by models are changes in nuclear cross-sections and the new solar composition. In Table4, we list the results for neutrino fluxes for the up-to-date SSMs SFII-GS98 and SFII-AGSS09. For comparison, we include, in the last column, results from the BP04 SSM [76].Table 4
SSM predictions for solar neutrino fluxes (second and third columns) and solar neutrino fluxes (fourth column) inferred from all available neutrino data. Units are, incm-2s-1, as usual: 1010(pp),109 (7Be), 108 (pep,13N, 15O) 106 (8B, 17F), and 103(hep). Note that the limit on the fluxes relative to the CNO cycle do not contain yet the information coming from recent Borexino result [74]. A revised analysis including these data is in progress.
Flux
SFII-GS98
SFII-AGSS09
Solar
BP04
pp
5.98
(
1
±
0.006
)
6.03
(
1
±
0.006
)
6.05
(
1
-
0.011
+
0.003
)
5.94
(
1
±
0.01
)
pep
1.44
(
1
±
0.012
)
1.47
(
1
±
0.012
)
1.46
(
1
-
0.014
+
0.010
)
1.40
(
1
±
0.02
)
hep
8.04
(
1
±
0.30
)
8.31
(
1
±
0.30
)
18
(
1
-
0.5
+
0.4
)
7.8
(
1
±
0.16
)
7
Be
5.00
(
1
±
0.07
)
4.56
(
1
±
0.07
)
4.82
(
1
-
0.04
+
0.05
)
4.86
(
1
±
0.12
)
8
B
5.58
(
1
±
0.13
)
4.59
(
1
±
0.13
)
5.00
(
1
±
0.03
)
5.79
(
1
±
0.23
)
13
N
2.96
(
1
±
0.15
)
2.17
(
1
±
0.13
)
≤6.7
5.71
(
1
±
0.36
)
15
O
2.23
(
1
±
0.16
)
1.56
(
1
±
0.15
)
≤3.2
5.03
(
1
±
0.41
)
17
F
5.52
(
1
±
0.18
)
3.40
(
1
±
0.16
)
≤5.9
5.91
(
1
±
0.44
)
χ
2
/
P
agr
3.5/90%
3.4/90%
—
—The most striking difference is the large reduction in the13N and 15O fluxes between the SFII-GS98 and BP04 models, which use the same solar composition. This reduction comes as a result of the new determination of S1,14, mostly by the LUNA experiment [77, 78], that has halved its value with respect to previous results (Table 2). If correct, the new expectation value of the combined 13N + 15O fluxes poses an even more challenging task for neutrino experiments to detect CNO fluxes. By comparing fluxes in Table 4 for models computed with the same solar composition (SFII-GS98 and BP04), it can be seen that in terms of flux values, those associated with the pp-chains have not changed much since 2004, despite improvements in the input physics entering solar model calculations. Few percent changes are present and are the result of changes in the nuclear cross-sections discussed before and also of the new OP radiative opacities. This is an encouraging situation; it implies that neutrino fluxes are robust predictions of solar models and, as experimental data on solar neutrinos accumulate, it will be possible to start fulfilling the initial goal posed by Davis and Bahcall: to use solar neutrinos to learn about the solar interior.In Figure2, we show the distribution of the solar neutrino fluxes as a function of solar radius. Together with the electron density profile, provided also by solar models (and neutron density profiles for sterile neutrino studies), these quantities are of fundamental importance for neutrino oscillation studies. It is worth noting that the 13N flux has two components. The larger one is associated with the operation in quasi-steady state of the CN-cycle in the innermost solar core (R<0.1R⊙), and for this reason coincides with the production region of the 15O flux (Figure 2(b), blue and black curves, resp.). This component of the 13N flux, as well as the total 15O flux, is linearly dependent on S1,14. The additional component of the 13N flux comes from the residual burning of 12C by the reactions 12C(p,γ)13N(β+)13C at temperatures not high enough to close the CN-cycle with a proton capture on 14N. This component is completely independent of S1,14. The careful reader will notice that the ratio of 13N and 15O fluxes is different in the SFII-GS98 and BP04 models, despite having the same solar composition. Whereas the added 13N +15O neutrino flux is linearly proportional to the C + N abundance in the solar core and also linearly proportional to S1,14, this degeneracy can be broken, at least theoretically, if the two fluxes can be experimentally isolated from one another.Normalized production profiles of solar neutrinos as a function of solar radius.
(a)
(b)The impact of thelow-Z solar composition on the production of solar neutrinos can be grasped by comparing results of models SFII-GS98 and SFII-AGSS09 shown in Table 4. As stated before, metals shape the solar structure through the radiative opacity. The lower abundance of metals in the AGSS09 composition is responsible for a reduction of the temperature in the solar core of about 1%. Because of the extreme temperature sensitivity of some of the neutrino fluxes this is enough to produce large changes in the total fluxes. The most extreme case is, of course, 8B, with the SFII-AGSS09 value being ~20% smaller. For 7Be the reduction is of ~9%.Given the small uncertainties in the experimental determination of these fluxes, it would be tempting to think these neutrino fluxes have the potential to discriminate between the two flavors of solar composition and contribute, in this way, to the solution of the solar abundance problem. As can be seen in Table4, unfortunately, the 7Be and 8B fluxes determined from experiments lie almost right in between the high-Z and low-Z models.In any case, since it is known thatlow-Z solar models do not reproduce well the solar structure as discussed in the previous section, it is dangerous to extract conclusions from comparing neutrino fluxes of this model to experimental results. Regardless of what the solution to the solar abundance problem is, since it will modify the solar interior structure, it will also change the expected values for the neutrino fluxes. In this regard, CNO fluxes are particularly interesting. Although they are of course affected by temperature variations to a comparable degree as the 8B flux is, they carry an extra linear dependence on the solar composition that is not related to temperature variations (The 17F flux is linearly dependent on O, but unfortunately the flux is too low to be detectable with current experimental capabilities.) Of particular interest is the linear dependence of the 13N and 15O fluxes on the combined C + N abundance. It is this dependence that enhances their capability as a diagnostic tool. In fact, differences between SFII-GS98 and SFII-AGSS09 models for these two fluxes are of the order of 30% (taking SFII-GS98 as reference) and, what is more important, a large contribution to these differences does not have an origin on temperature differences between the models.The last row in Table4 shows the results of an χ2 test for the two models against the solar fluxes also shown in the table. It is clear that both SSMs give a very good agreement with current data. We emphasize again, however, that the four fluxes that are currently well determined from data and the luminosity constraint, depending on the solar composition only in an indirect manner. Experimental determination of the combined 13N + 15O flux will therefore provide qualitatively new information on the solar structure and composition. In fact, one can take advantage of the similar response to temperature variations that CNO fluxes and the 8B flux has. This has been exploited [79] to develop a very simple method to determine the solar core C + N abundance that minimizes environmental uncertainties in solar models (i.e., sources of uncertainty that affect the solar core temperature). The idea is simple: the temperature dependences are cancelled out by using an appropriate ratio between the 8B and the combined 13N + 15O fluxes where SSM fluxes only act as normalization values and the overall scale is determined by an actual 8B flux measurement. The only additional requirement is that a measurement of the combined 13N + 15O flux becomes available. The current upper limit on this combined flux from Borexino [74] places an upper limit on the C + N central mass fraction of XC+N<0.072. Results for the SFII-GS98 and SFII-AGSS09 models are XC+N=0.048 and 0.039, respectively.


## 3.3.2. Uncertainties

Uncertainties in the model predictions of solar neutrino fluxes are given in Table4. For deriving the total uncertainty basically two approaches can be used. On one hand, all contributions of uncertainty can be treated simultaneously by doing a Monte Carlo simulation [80]. The advantage is that intrinsic nonlinearities are captured in the total error. The disadvantage is that individual contributions to the total uncertainty are hardwired in the final result and cannot be disentangled. Fortunately, for the current level of uncertainties entering SSM calculations, nonlinearities seem to be negligible and the total uncertainty in neutrino fluxes can be obtained (adding quadratically) from individual contributions. To compute the latter, the expansion of fluxes as a product of power laws in the input parameters [43] around central values is a widely used, practical, insightful, and accurate approach. Uncertainties in the model fluxes listed in Table 4 have been obtained in this way.The most important change introduced in the estimation of uncertainties is related to the treatment of the solar composition. Up until the BP04 model [76], the uncertainty in the solar composition was taken into account by considering variations of the total solar metallicity (to be more precise, changes in the (Z/X)⊙ value used to construct SSMs). This leads to an overestimation of the neutrino uncertainties. The reason is that metals dominating the error budget in (Z/X)⊙ (C, N, O, and Ne) have, at most, a moderate impact on the neutrino fluxes because of their small contribution to the radiative opacity, and therefore a rather small impact on temperature, in the region where most neutrinos are produced. On the other hand, elements such as Fe, S, and Si are second-order in determining (Z/X)⊙ but play a fundamental role as sources of opacity in the solar core. It is important, therefore, to treat metal uncertainties individually [81]. Of course, in the case of the CNO fluxes the situation is different because CNO elements catalyze the CNO-bicycle and this overimposes an almost linear dependence of the 13N and 15O on the C + N content of the solar and a similar dependence of 17F on the O abundance. The uncertainties in the neutrino fluxes given for the SFII-GS98 and SFII-AGSS09 SSMs have been computed using the uncertainties for each relevant element given in the original publications [46, 50]. As a result, for either family of solar models, that is, high-Z or low-Z models, the solar composition is not the dominant source of uncertainty for any of the fluxes of the pp-chains. In the case of the CNO fluxes, the linear dependence mentioned above is the dominant source of uncertainty: the combined C + N abundance contributes to a 12% uncertainty for both the 13N and the 15O fluxes, and the O abundance to 15% in the 17F flux.In the case of the noncomposition uncertainties, the situation has improved in some cases thanks to more precise measurements of nuclear reaction rates. This is the case, in particular, for the3He(4He,γ)7Be reaction, which now contributes only 4.7% and 4.5% of the total uncertainty in the 7Be and 8B fluxes, respectively. For comparison, the analogous contributions in the BP04 model were 8.0% and 7.5% [76]. Significant progress has also been achieved regarding 14N(p,γ)15O, which now introduces uncertainties of only 5% and 7% in the 13N and 15O fluxes, half the amount it did in 2004. An important contribution to the uncertainty in the 8B flux now comes from 7Be(p,γ)8B because the uncertainty of this reaction has been revised upwards [55]. Even if the uncertainty in this rate is now smaller than in SFI (see Table 2), it is larger than that used for the BP04 model, which was taken considering only one experimental result for this reaction.While progress has been done in some cases, others have not seen much development, particularly diffusion and the delicate issue of radiative opacities. In Table5, we give the individual contributions to flux uncertainties for the most relevant sources. The reader can compare directly to the situation in 2004 [76].Table 5
Percentage contribution of selected individual sources of uncertainty to the neutrino fluxes.
S
11
S33
S34
S17
S1,14
Opac
Diff
pp
0.1
0.1
0.3
0.0
0.0
0.2
0.2
pep
0.2
0.2
0.5
0.0
0.0
0.7
0.2
hep
0.1
2.3
0.4
0.0
0.0
1.0
0.5
7
Be
1.1
2.2
4.7
0.0
0.0
3.2
1.9
8
B
2.7
2.1
4.5
7.7
0.0
6.9
4.0
13
N
2.1
0.1
0.3
0.0
5.1
3.6
4.9
15
O
2.9
0.1
0.2
0.0
7.2
5.2
5.7
17
F
3.1
0.1
0.2
0.0
0.0
5.8
6.0


## 4. Neutrino Flavor Conversion in Vacuum and Matter

Neutrino flavor conversion has been reviewed by Yu. Smirnov in this volume and we refer the reader for a detailed physics discussion and references to his article. Here we just summarize the basic features and formulae of flavor conversion relevant to solar neutrinos.We consider mixing of the three flavor neutrinos. The description of flavor conversion of solar neutrinos traveling through a medium is simplified because (a) the hierarchy in mass splittings determined by solar and atmospheric data leads to a reduction of the three neutrino flavor conversion to an effective two-flavor problem and (b) the neutrino parameters, the mixings, and solar mass splitting lead to adiabatic flavor conversion in solar matter and to cancel the interference term by averaging out. Therefore, the physics of the flavor conversion of solar neutrinos is described by simple expressions with a very good accuracy. In practice, the survival probability is computed numerically to correctly include the number density of scatterers along the trajectory of neutrinos from the production to the detection and to average over the neutrino production region. In solar neutrino flavor conversion,νμ and ντ are indistinguishable and therefore the survival probability of electron neutrinos is the only function needed to describe the flavor composition of the solar neutrino flux.Solar neutrino survival or appearance probabilities can be expressed in terms of three oscillation parameters (that can be called the solar oscillation parameters), namely, the mixing angles between the first neutrino mass eigenstate and the two other active mass eigenstates (θ12 and θ13) and the difference of the squares of the first and second generation mass eigenvalues (Δm212). The survival probability in the absence of Earth-matter effects, that is, during the day, is well described by
(5)PeeD=cos4θ13(12+12·cos2θS·cos2θ12)+sin4θ13.
Here, θS is the mixing angle at the production point inside the Sun:
(6)cos2θS≡cos2θm(ρS),
where θm(ρ) is the mixing angle in matter of density ρS,
(7)cos2θS=cos2θ12-ξS(1-2ξScos2θ12+ξS2)1/2.
In (7), ξS is defined as the ratio of the neutrino oscillation length in vacuum, lν, to the refraction length in matter, l0:
(8)ξS≡lνl0=22GFρSYecos2θ13mNEΔm2=0.203×cos2θ13(E1MeV)(ρSYe100gcm-3),
where
(9)lν≡4πEΔm2,l0≡2πmN2GFρSYecos2θ13.
In (8) and (9), ρS is the solar matter density, YeS is the number of electrons per nucleon, and mN is the nucleon mass. The electron solar density and neutrino production distribution of the neutrino fluxes are derived from solar models as discussed in the previous section. In the last line in (8), we have used the best fit values of the global analysis Δm2=7.5×10-5 eV2. The ratio of the parameter ρS to cos2θ12 separates the region where the flavor conversion corresponds to vacuum averaged oscillations from the one of matter dominated conversion.Theνe survival probability at night during which solar neutrinos pass through the Earth can be written as
(10)PeeN=PeeD-cos2θScos2θ13〈freg〉zenith,
where PeeD is the one given in (5). freg denotes the regeneration effect in the Earth and is given as freg=P2e-sin2θ12cos2θ13, where P2e is the transition probability of the second mass eigenstate to νe. Under the constant density approximation in the Earth, freg is given by
(11)freg=ξEcos2θ13sin22θE×sin2[aEcos2θ13(1-2ξE-1cos2θ12+ξE-2)1/2(L2)],
for passage of distance L, where we have introduced aE≡2GFneEarth=2GFρEYeE/mN.In (11), θE and ξE stand for the mixing angle and the ξ parameter (see (8)) with matter density ρE in the Earth. Within the range of neutrino parameters allowed by the solar neutrino data, the oscillatory term averages to 1/2 in a good approximation when integrated over zenith angle. Then, the equation simplifies to
(12)〈freg〉zenith=12cos2θ13ξEsin22θE.
At E=7MeV, which is a typical energy for 8B neutrinos, ξE=3.98×10-2 and sin2θE=0.940 for the average density ρ-E=5.6g/cm3 and the electron fraction YeE=0.5 in the Earth. Then, 〈freg〉zenith is given as 〈freg〉zenith=1.76×10-2 for the best fit neutrino parameters. This result is in a reasonable agreement with the computed Earth-matter factor using the best estimates on the Earth-matter density.


## 5. Recent Solar Neutrino Measurements

### 5.1. The SNO and SK Legacy

After the results and analyses from 2002, it was clear that the LMA oscillation was the right solution of the long standing solar neutrino puzzle [82–93], but the activity of the SNO and SK experiments continued in the following years. The data obtained from these experiments were very important in making the LMA solution more robust and in improving the accuracy and precision of the mixing parameters determination.The so-called SNO II experiment began in June of 2001 with the addition of 2000 kg of NaCl to the 1000 metric tons ofD2O and ended in October 2003 when the NaCl was removed. The addition of salt significantly increased SNO’s efficiency (by a factor ~3 with respect to the pure D2O phase) in the detection of neutrons produced in the neutral current (NC) disintegration of deuterons by solar neutrinos and, by enhancing the energy of the γ-ray coming from neutron capture, allowed a more precise measurement of this interaction channel, well above the low-energy radioactive background. Moreover, the isotropy of the multiple γ-ray emission by neutron capture on 35Cl is different from the one of the Cˇerenkov light emitted by the single electron of the charged current interaction; therefore, by studying the event isotropy, it has been possible to separate the neutral from the charged current events without any additional assumption on the neutrino energy spectrum. The salt phase results have been reported in two main publications. In [30], referring to the first 254 live days, a global analysis including all the solar and reactor neutrino results rejected the maximal mixing hypothesis at a 5.4σ level and gave a value of the 8B neutrino flux in agreement with previous measurements and with SSMs. These results were essentially confirmed (even if with a small shift towards larger values of the mixing angle) by the second publication [94], which included the full data of the salt phase (391 live days), analyzed in terms of the CC spectra (starting from 5.5MeV kinetic energy), and NC and ES integrated fluxes separately for day and night. The day-night asymmetry in the neutral current rate, which would be an indication of oscillation to sterile neutrinos or nonstandard interaction with matter in the earth, came out to be consistent with zero.This result confirmed also the outcome of the study performed for elastic scattering (ES) interaction above5MeV by the Super-Kamiokande collaboration [95]. The full SK-I low energy data, corresponding to 1496 live days until July 2001, were investigated analyzing the time variations of the ES rates and fitting them to the variations expected from active two neutrino oscillations. In this kind of study, the zenith angle of the solar neutrinos arriving on the detector is associated to the time variable and the full data are divided in two different time samples from which the day and night rates (D) and (N) are derived. The day-night asymmetry turned out to be ADN=2(D-N)/(D+N)=-0.021±0.020(stat.)-0.012+0.013(syst.), which is consistent with zero within 0.9σ. This value was in a good agreement also with the LMA oscillation solution, which (for the best fit parameter) predicted [95] ADN=-0.018±0.016(stat.)-0.012+0.013(syst.). The impact of Earth-matter effects on solar neutrino oscillations is an important topic, which has been widely studied in the literature with different techniques (analytical and semianalytical studies and fully numerical analyses)[96–109].The SK analysis [95, 110] also showed that the energy spectrum of the recoiling electron was consistent with an undistorted solar 8B neutrino spectrum and did not find any anomalous periodic time variation of the rates, apart from the expected seasonal variation due to the Earth’s orbit eccentricity. The SK best fit point was in quite a good agreement with the SNO results, even if SK would favor slightly larger values of tan2θ. A SNO-only analysis gave the following best fit parameters [94]: Δm122=5.0×10-5eV2, tan2θ12=0.45. Including all the other solar neutrino and the KamLAND results, the best fit was obtained for Δm122=8.0-0.4+0.6×10-5eV2, tan2θ12=0.452-0.070+0.088. The effect of KamLAND data was mainly to increase the value of Δm2 and to restrict the allowed region in the mixing parameter plane. The main difference of the global analysis done with the SNO salt phase data with respect to previous studies was the possibility to exclude at 95% CL the secondary region at even larger values of the mass differences (the so-called LMA II solution, with Δm122>10-4eV2).In the third SNO phase (November 2004–November 2006), the neutral current signal neutrons were mainly detected by means of an array of3He proportional counters deployed in the D2O and looking at the gas ionization induced by neutron capture on 3He. In this way, the fluxes correlation was reduced and the accuracy in the mixing angle determination was improved. The total active 8B neutrino flux was found [31] to be 5.54-0.31+0.33(stat)-0.34+0.36(syst)×106cm-2s-1, in agreement with previous measurements and SSMs. The ratio of the 8B neutrino flux measured with CC and NC reaction was ΦCCSNO/ΦNCSNO=0.301±0.033. The global solar neutrino experiment analysis included, in this case, also the first results coming from the Borexino experiment [111], that we discuss in Section 5.3. The best fit point moved to Δm122=4.90×10-5eV2, tan2θ12=0.437 and the uncertainty in the mixing parameter plane was still quite large. Adding the KamLAND data, the allowed region was significantly restricted (mainly for Δm2) and the marginalized 1σ regions were Δm122=7.59-0.21+0.19×10-5eV2, tan2θ12=0.469-0.041+0.047.A subsequent joint reanalysis of SNO I and SNO II data, known as LETA (low energy threshold analysis) [112], succeeded, with improved calibration and analysis techniques, in lowering the energy threshold, with respect to previous analyses [94, 113], down to an effective electron kinetic energy of Teff=3.5 MeV. The main effect was to increase the statistics of CC and ES and, above all, of NC events and to increase significantly the precision on both the total 8B neutrino flux and the neutrino mixing parameters. The value for the total 8B neutrino flux extracted from neutral current was ΦNC=5.14-0.20+0.21×106cm-2s-1, where the error, obtained by summing in quadrature the statistic and systematic contributions, was reduced by more than a factor of two with respect to previous publications. For SNO data alone (LETA plus SNO III), the best fit point moved to the LOW region of parameter space, but the significance level was very similar to the one of the usual LMA solution. A global fit, including all the solar and the KamLAND data, essentially confirmed, instead, the previous results [31] for Δm122 and it made possible a further improvement in the angle determination, giving, in a 2-flavor analysis, tan2θ12=0.457-0.028+0.041.In the last five years, also the Super-Kamiokande collaboration presented new analyses, including the data of the different working phases of this experiment: Super-Kamiokande II [114] (from December 2002 to October 2005) and Super-Kamiokande III (from July 2006 to August 2008) [115]. Due to the 2001 accident, which damaged some of the photomultiplier tubes, the detector sensitivity was reduced with respect to SK-I and therefore it was important to improve the methods adopted for data collection (particularly for vertex event reconstruction, angular resolution, and background reduction) and analysis. In this way, during the 548 days of SK-III a 2.1% systematic uncertainty on the total flux (corresponding roughly to two-thirds of the SK-I value) was reached. The second and third Super-Kamiokande phases essentially confirmed the SK-I results, for what concerns the absence of significant spectral distortion, the total 8B measured flux and the day-night asymmetry.Since September 2008, Super-Kamiokande is running with modernized data acquisition system (DAQ) and electronics, which allow a wider dynamic range in the measured charge and is read out via Ethernet. This phase of the experiment is denoted as Super-Kamiokande IV [116]. Thanks to the fast DAQ every hit can be recorded and the resulting data stream analyzed by an online computer system that finds timing coincidences which are saved as triggers. As a consequence, Super-Kamiokande’s energy threshold is now only limited by computing speed and the event reconstruction. The present event reconstruction is able to reconstruct electrons with a total energy of 3 MeV or more. The computing speed limits the energy threshold to 4.2 MeV which is just below the threshold of Super-Kamiokande I and III (4.5 MeV). The same water flow techniques developed during Super-Kamiokande III result in an observed solar neutrino elastic scattering peak between 4 and 4.5 MeV total recoil electron energy. Special techniques are developed to discriminate the signal from the background, taking advantage from the fact that the background is mainly due to β emission from 214Bi and it is characterized by a larger Coulomb multiple scattering. This makes possible a reduction of about 10–15% of the statistical uncertainty and this method can also be applied to previous phases of the experiment. The additional systematic uncertainty of this method is under investigation.


### 5.2. The Impact of KamLAND Results on Solar Neutrino Physics

Even if it is based on the analysis of a reactor antineutrino beam, the KamLAND experiment played a fundamental role in the solution of the long standing solar neutrino puzzle. In fact, the first KamLAND data [34] were determinant, in conjunction with the previous solar neutrino experiments (and mainly with SNO) and assuming CPT invariance, to prove the validity of the oscillation hypothesis and to select the LMA solution as the correct one.Between March 2002 and January 2004, a new set of data were collected and the KamLAND collaboration performed a study including also a reanalysis of the previous data. During the 2002–2004 campaign, important upgrades were done both on the central detector (increasing the photocatode coverage and improving the energy resolution) and in the analysis techniques (reduction of the background with better techniques in the event selection cuts based on the time, position, and geometry of the events). The number of antineutrino events above2.6 MeV expected in absence of antineutrino disappearance was 365.2±23.7(syst) and the 258 observed events corresponded to a ν-e survival probability equal to 0.658±0.044(stat)±0.047(syst). The energy spectrum analysis was in disagreement with the no oscillation hypothesis at 99.6% statistical significance. In [39], the KamLAND collaboration, looking at the L0/E spectrum dependence (where L0 is the source-detector distance and E the ν-e energy), performed also an interesting study of other alternative hypotheses (like decoherence and decay) for neutrino disappearance. The oscillation hypothesis offered by far the best explanation of the spectrum shape, as one can see from Figure 3.Figure 3
Ratio of the observedν-e spectrum to the expectation for nooscillation versus L0/E. The curves show the expectation for the best-fit oscillation, best-fit decay, and best-fit decoherence models, taking into account the individual time-dependent flux variations of all reactors and detector effects. Taken from [39].As shown in Figure4(a), the best fit obtained from the data analysis was in the so-called LMAI region (with values of Δm122 around 8·10-5eV2) and the alternative solution at higher Δm122 (around 2·10-4eV2) was strongly disfavoured, at 98% CL, mainly due to the spectrum distortions. The KamLAND data alone were not sufficient to solve completely the ambiguity on the mixing angle values and to exclude maximal mixing. However, including in the analysis also the results coming from solar neutrino experiments, the allowed values of the angle were significantly restricted (see Figure 4(b)) and the two-flavor combined analysis gave Δm122=7.9-0.5+0.6·10-5eV2, tan2θ12=0.40-0.07+0.10 at a 1σ level.(a) Allowed region of the neutrino oscillation parameter from KamLAND antineutrino data (colored regions) and solar neutrino experiments (lines) [30]. (b) the result of a combined two-neutrino oscillation analysis of KamLAND and the observed solar neutrino fluxes under the assumption of CPT invariance. Taken from [39].
(a)
(b)The next KamLAND analysis [40] included also, in addition to the one of [34, 39], the new data collected up to May 2007. The increase in data collection was significant (also thanks to enlarging the radius of the fiducial volume from 5.5 to 6 m) and there was a reduction of systematic uncertainties, in the number of target protons and the background. The total uncertainty on Δm212 was around 2%, mainly due to the distortion of the energy scale in the detector. The total uncertainty, 4.1%, on the expected event rate was due to different sources (above all the definition of the detector fiducial volume and energy threshold, the ν-e spectra, and the reactor power) and it affected primarily the mixing angle determination. The different background sources were studied and reduced further. The most important one was the 13C(α,n)16O reaction made possible by the α decay of 210Po (a daughter of 222Rn) introduced in the liquid scintillator during the construction, which produces neutrons with energies up to 7.3MeV.The results of the statistical analysis are reported in Figure5, taken from [40]. The allowed oscillation parameter values were Δm212=7.58-0.13+0.14(stat)-0.15+0.15(syst)·10-5eV2 for the mass eigenvalues and tan2θ12=0.56-0.07+0.10(stat)-0.06+0.10(syst), for tan2θ12<1 and the no oscillation hypothesis was excluded at 5σ. The extension to the three-neutrino oscillation analysis had the main effect to enlarge the uncertainty on θ12, leaving Δm122 substantially unchanged. Figure 5, taken from [40], shows that the effect of the inclusion in the analysis of the data from SNO [94] and previous solar neutrino experiments was essential to reduce the interval of allowed θ12 values and also to move the best-fit point towards slightly lower values of the mixing angle.Figure 5
Allowed region for neutrino oscillation parameters from KamLAND and solar neutrino experiments. The side-panels show theΔχ2-profiles for KamLAND (dashed) and solar experiments (dotted) individually, as well as the combination of the two (solid). Taken from [40].Figure6 (taken from [40]) illustrates, instead, the ν-e survival probability, as a function of the ratio L0/E between the average baseline and the antineutrino energies. One can notice that the observed spectrum (after subtraction of background and geoneutrino signals), reproduces correctly the general shape of the expected oscillation cycle, with a slight excess of low energy antineutrinos, that could be interpreted as geoneutrinos.Figure 6
Ratio of the background and geo-neutrino-subtractedν-e spectrum to the expectation for no oscillation as a function of L0/E. L0 is the effective baseline taken as a flux-weighted average (L0 = 180 km). The energy bins are equal probability bins of the best fit including all backgrounds. The histogram and curve show the expectation accounting for the distances to the individual reactors, time-dependent flux variations, and efficiencies. The error bars are statistical only and do not include, for example, correlated systematic uncertainties in the energy scale. Taken from [40].


### 5.3. Toward the Sub-MeV Analysis: The Borexino Detector and Its Measurements

In the last decade, significant steps forward have been done in the knowledge of solar neutrino properties, thanks mainly to the results obtained by the kiloton scaleCˇerenkov detectors (SK and SNO) and by advent of the reactor neutrino experiment KamLAND. However, these experiments investigated only the energy part of solar neutrino spectrum above 5 MeV, which represents a small fraction of the full spectrum. The single components of the neutrino spectrum cannot be determined by such techniques at low energies and, therefore, up to the last four years, low energy neutrinos had been observed only via radiochemical methods. A significant change took place with the advent of Borexino, a real-time experiment which opened the way to the investigation of the sub-MeV region and isolated for the first time the neutrinos corresponding to the monochromatic beryllium line.


#### 5.3.1. The Borexino Detector

Borexino is an ultrahigh radiopure large volume liquid scintillator detector (using pseudocumene—PC (1,2,4-trimethylbenzene)—as aromatic scintillation solvent, and PPO (2,5-diphenyloxazole) as solute at a concentration of 1.5 g/L) located underground at the italian Gran Sasso National Laboratories (LNGS), under about 1400 m of rock (3800 mwe) [117]. The employment of a liquid scintillator as target mass assures a light production sufficient to observe low energy neutrino events via elastic scattering by electrons. This reaction is sensitive to all neutrino flavors, through the neutral current interaction, but the cross-section for νe is larger than νμ and ντ by a factor of 5-6, due to the combination of charged and neutral currents. The main goal of Borexino is the measurement of the monoenergetic (0.862MeV) 7Be neutrinos, which have the basic signature of the Compton-like edge of the recoil electrons at 665 keV (see Figure 7).Figure 7
Neutrino spectra expected in Borexino (accounting for the detector’s energy resolution). The upper line represents the neutrino signal rate in Borexino according to the most recent predictions of the standard solar model [118] including neutrino oscillations with the LMA-MSW parameters. The lower line illustrates the contribution due to 7Be neutrinos. The pp neutrinos contribute to the spectrum below 0.3 MeV and the edge at 1.2 MeV is due to pep neutrinos (from [119]).The high light yield typical of a liquid scintillator makes it possible to reach a low energy threshold, a good energy resolution of about5% at 1 MeV, and a pulse shape discrimination between α and β decays. On the other hand, no directionality is possible and it is also not possible to distinguish neutrino scattered electrons from electrons due to natural radioactivity. For this reason, an extremely low level of radioactive contamination is compulsory and this has been one of the main tasks and technological achievements of the experiment. The background due to the presence of β decay of 14C (βend-point 156 keV), intrinsic to the scintillator, limits neutrino observation to energies above 200 keV. Techniques for the scintillator purification are based mainly on methods developed and tested in earlier studies with the counting test facility (CTF), a 4-ton prototype of Borexino which demonstrated for the first time the feasibility of achieving the low backgrounds needed to detect solar neutrinos in a large-scale scintillator [120–122]. For Borexino, a larger purification plant was developed similar to the CTF system, but with several improved features including the use of high vacuum and precision cleaning techniques.The design of Borexino is based on the principle of graded shielding (onion-like structure—see Figure8).Figure 8
Schematic view of the Borexino detector.The scintillator (≈300 tons) is contained in a thin nylon inner vessel (IV), of radius 4.25 m, at the center of a set of concentric shells of increasing radiopurity and it is surrounded by an outer vessel (OV), filled with PC and 5.0 g/L DMP (dimethyl phthalate), a material which is able to quench the residual scintillation of PC and acts as a passive shield against radon and other background contaminations originating from the external parts. A third more external vessel is composed of a stainless steel sphere (SSS), enclosing the passive shield (PC-DMP), and the entire detector is contained in a dome-shape structure 16.9 m high with a radius of 9 m, filled with ultrapure water, denominated water tank (WT). The scintillation light is recorded by 2212 8-inches photomultipliers distributed on the inner part of the SSS [123, 124]; 1828 of them are equipped with aluminum light concentrators designed to increase the light collection efficiency [125]. Čerenkov’s light and residual background scintillation in the buffer are thus reduced. The others 384 photomultipliers without concentrators are used to study this background and to identify muons that cross the buffer and not the inner vessel. The water tank is equipped with 208 8-inches photomultipliers and acts as a Čerenkov muon detector. Although the muon flux is reduced by a six-order of magnitude by the 3800 mwe depth of the Gran Sasso Laboratory is still significant (1.1 μm-2 h-1). An additional reduction, of the order of about 104, has been necessary; for more details see [126].In order to remove contaminants from dust (U, Th, K), air (Ar39, Kr85), and cosmogenically produced isotopes (Be7), different purification techniques were applied, such as distillation, water extraction, nitrogen stripping, and ultrafine filtration. The pseudocumene was distilled in-line during the detector filling at 80 mbar and at a temperature of about 90–95°C. Distilled pseudocumene was stripped in an 8 m high (15 cm in diameter) packed column with specially prepared ultralow Ar/Kr nitrogen (0.005 ppm Ar and 0.06 ppt Kr, see [127]). Position reconstruction of the events, as obtained from the photomultipliers timing data via a time-of-flight algorithm, allowed to define a fiducial spherical volume, corresponding approximately to 1/3 (i.e., about 100 tons) of the scintillator volume in order to reject external γ background. The others 2/3 of the scintillator act as an active shield.


#### 5.3.2. The Measurement of the7Be Line

The Borexino collaboration started taking data in May 2007 and after only 3 months (47.4 live days) it was able to extract the7Be signal from the background. The best value estimate for the rate was 47±7(stat)±12(syst) counts/(day · 100 ton), where the systematic error is mainly due to the fiducial mass determination [119]. An update of the 7Be signal was reported after 9 months from an analysis of 192 live days (from May 16 2007 to April 12 2008), corresponding to 41.3 ton · yr fiducial exposure to solar neutrinos.The severe cuts that had to be passed by the events in order to be selected and enter the analysis were mainly designed to avoid pile up of multiple events and reject the events originated by muons and their daughters and the ones due to radon daughters preceding theα-β Bi-Po delayed coincidences. Moreover, severe cuts (radial and based on the z-coordinates) were finalized to reduce the external γ background. The remaining fiducial mass was of about 79 metric tons. Important background sources were the fast coincidence decays from the 238U chain (contamination level of (1.6±0.1)10-17 g/g) and the 232Th chain (contamination level of (6.8 ± 1.5) 10−18 g/g) and the 85Kr contained in the scintillator that produces the rare decay sequence 85Kr→85mRb+e-+ν-e,85mRb→85Rb+γ. The total estimated systematic error was 8.5% [111], mainly determined by two sources, introducing an uncertainty of 6% each: the total uncertainty on the fiducial mass and the one on the response function. The best value for the interaction rate of the 0.862 MeV 7Be solar neutrinos was 49±3(stat)±4(syst) counts/(day · 100 ton). This result excludes at the 4σ CL the no oscillation hypothesis for 7Be solar neutrinos, which in the high metallicity SSM [118, 128] would imply 74±4 counts/(day · 100 ton). The Borexino result is, instead, in a very good agreement with the predictions of the LMA oscillation solution: 48±4 counts/(day · 100 ton).In order to reduce the systematic uncertainties and to tune the reconstruction algorithm and Monte Carlo simulations, a calibration campaign was performed in 2009 introducing inside the Borexino detector several internal radio sourcesα’s, β’s, γ’s, and neutrons, at different energies and in hundreds of different positions, which were determined with a precision better than 2 cm. The previous systematic error on 7Be solar neutrino flux was estimated to be [111] at the level of 6% for both the fiducial volume and the energy scale (when thermal neutrons are captured by protons a 2.2 MeV γ-ray is generated.) In the calibration campaign, the detector energy response was studied with eight γ sources and Am-Be neutron source and comparing the calibration data and Monte Carlo simulations at different energies within the solar neutrinos energy region. The energy scale uncertainty, obtained with these studies, was determined to be less than 1.5%.The inaccuracy of the position (reduced by means of studies withα and β events) was less than 3 cm, equivalent to a systematic error of 1.3% for the overall fiducial volume in the 7Be solar neutrino energy region. The analyzed data set run from May 2007 to May 2010, with a fiducial exposure equivalent to 153.6 ton · year. In order to extract the 7Be solar neutrino signal, the spectral fit was applied assuming all the intrinsic background components such as 85Kr, 210Bi, 14C, and 11C. The 7Be solar neutrino rate was evaluated to be 46.0±1.5(stat)-1.6+1.5(syst) counts/day · 100 ton [129]. Thanks to the calibration campaign, the systematic error was reduced to 2.7% and the total uncertainty to 4.3%.


### 5.4. Thepep and CNO Neutrinos Measurement in Borexino

In the SSM, due to the solar luminosity constraint and their intimate link to thepp neutrinos [43, 56], the monoenergetic 1.44 MeV pep neutrinos have one of the smallest uncertainties (1.2%) [64]. For this reason, after the pp neutrinos, they constitute the ideal probe to test SSM hypotheses. On the other hand, the detection of neutrinos within the CNO-bicycle is central to probe the solar core metallicity and contribute in this way to the solution of the solar metallicity problem [64, 130]. Also, they are believed to fuel massive stars with mass greater than ~1.2M⊙ during the main sequence evolution and also stars with lower masses in more advanced stages of evolution. The energy spectrum of neutrinos from the CNO-bicycle is the result of three continuous spectra with end point energies of 1.19 MeV (13N), 1.73 MeV (15O), and 1.74 MeV (17F). Despite their relevance, until 2011, no pep and CNO neutrinos had been detected directly.The electron recoil energy spectrum frompep neutrino interactions in Borexino is a Compton-like shoulder with end point of 1.22 MeV, as one can see from Figures 9 and 10, showing the pep and CNO contribution in Borexino.Examples of fitted spectra; the fit results in the legends have units [counts/(day· 100 ton)]. (a): A Monte Carlo based fit over the energy region 270–1600 keV to a spectrum from which some, but not all, of the α events have been removed using a PSA cut, and in which the event energies were estimated using the number of photons detected by the PMT array. (b): An analytic fit over the 290–1270 keV energy region to a spectrum obtained with statistical α subtraction and in which the event energies were estimated using the total charge collected by the PMT array. In all cases the fitted event rates refer to the total rate of each species, independently from the fit energy window (from [129]).
(a)
(b)Figure 10
The neutrino-induced electron recoil spectra expected in Borexino. The total rates are those predicted by the latesthigh-Z solar model [64]. The pep and CNO neutrinos recoil spectra with end points in the region 1.2–1.5 MeV are shown. Also the 7Be neutrinos (measured in [129]), with a count rate about 10 times larger, are shown for comparison. Note that the variable on the x-axis is not directly the energy value. Taken from [131].As already mentioned, very low background levels [111, 119] are required to detect 7Be neutrinos; the detection of pep and CNO neutrinos is even more challenging, as their expected interaction rates are ~10 times lower. The expected rate is on the order of a few counts per day in a 100-ton target. To detect pep and CNO neutrinos, the Borexino collaboration adopted a novel analysis procedure to suppress the dominant background in the 1-2 MeV energy range, due to the cosmogenic β+-emitter 11C produced within the scintillator by muon interactions with 12C nuclei. The muon flux crossing the Borexino detector, ~4300 μ/day, yields a 11C production rate of ~27 counts/(day · 100 ton) (In 95% of the cases at least one free neutron is spalled in the 11C production process [132], and then captured in the scintillator with a mean time of 255 μs [133].) This background can be reduced by performing a space and time veto following coincidences between signals from the muons and the cosmogenic neutrons [134, 135], discarding exposure that is more likely to contain 11C due to the correlation between the parent muon, the neutron, and the subsequent 11C decay (the three-fold coincidence, TFC). The TFC technique is based on the reconstructed track of the muon and the reconstructed position of the neutron-capture γ-ray [133]. The criteria of rejection were applied to obtain the best compromise between 11C rejection and preservation of fiducial exposure, resulting in a 11C rate of (2.5±0.3) count per day and (9±1)% of the original rate, while preserving 48.5% of the initial exposure.Figure11 shows the resulting spectrum obtained with data collected between January 2008 and May 2010, corresponding to a fiducial exposure of 20409 ton · day [74]. Despite the TFC veto, the number of 11C surviving events still constituted a significant background.Figure 11
Energy spectra of the events in the FV before and after the TFC veto is applied. The solid and dashed blue lines show the data and estimated11C rate before any veto is applied. The solid black line shows the data after the procedure, in which the 11C contribution (dashed) has been greatly suppressed. The next largest background, 210Bi, and the electron recoil spectra of the best estimate of the pep neutrino rate and of the upper limit of CNO neutrino rate are shown for reference. Rate values in the legend are quoted in counts/(day · 100 ton) from [74].To discriminate11C β+ decays from neutrino-induced e- recoils and β- decays, the pulse shape differences between e- and e+ interactions in organic liquid scintillators [136, 137] were exploited. In fact a small difference in the time distribution of the scintillation signal arises from the finite lifetime of orthopositronium as well as from the presence of annihilation γ-rays, which present a distributed, multisite event topology and a larger average ionization density than electron interactions. The Borexino collaboration employed an optimized pulse shape parameter using a boosted-decision-tree algorithm [138] and trained with a TFC-selected set of 11C events (e+) and 214Bi events (e-) selected by the fast 214Bi-214Po α-β decay sequence (less than 2.8 m from the detector center and with a vertical position relative to the detector center between −1.8 m and 2.2 m.) In a work published in 2012 [74], the Borexino collaboration presented the results of an analysis based on a binned likelihood multivariate fit performed on the energy, pulse shape, and spatial distributions of selected scintillation events whose reconstructed position is within the fiducial volume.The energy spectra and spatial distribution of the externalγ-ray backgrounds have been obtained from a full, Geant4-based Monte Carlo simulation and validated with calibration data from a high-activity 228Th source [139] deployed in the outermost buffer region, outside the active volume. α events were removed from the energy spectrum by the statistical subtraction method [119]. In the energy region of interest of the fit procedure all background species whose rates were estimated to be less than 5% of the predicted rate from pep neutrinos have been excluded (electron recoils from 7Be, pep, and CNO solar neutrinos, internal radioactive backgrounds 210Bi, 11C, 10C, 6He, 40K, 85Kr, and 234mPa, and external γ-rays from 208Tl, 214Bi, and 40K.) All rates were constrained to positive values and thirteen species were left free in the fit. The rate of the radon daughter 214Pb was fixed using the measured rate of 214Bi-214Po delayed coincidence events. The contribution from pp solar neutrinos was fixed to the SSM assuming MSW-LMA [140–145] with tan2θ12=0.47-0.04+0.05, Δm122=(7.6±0.2)·10-5 eV2 [146], and the contribution from 8B neutrinos to the rate from the measured flux [112, 147].In Table6, the results for the pep and CNO neutrino interaction rates are shown. The absence of a pep neutrino signal was rejected at 98% CL. Concerning the CNO neutrinos flux, its electron-recoil spectrum is similar to the spectral shape of 210Bi, but the last one is about 10 times greater; therefore, it has only been possible to provide an upper limit on the CNO neutrino interaction rate. The 95% CL limit reported in Table 6 has been obtained from a likelihood ratio test with the pp neutrino rate fixed to the SSM prediction [64] under the assumption of MSW-LMA, (2.80±0.04) counts/(day · 100 ton).Table 6
Best estimates for thepep and CNO solar neutrino interaction rates. For the results in the last two columns both statistical and systematic uncertainties are considered. Total fluxes have been obtained assuming MSW-LMA and using the scattering cross-sections from [146, 148, 149] and a scintillator e- density of (3.307±0.003)·1029ton-1. The last column gives the ratio between our measurement and the high-Z (GS98) SSM [64]. Table taken from [74].
ν
Interaction rate
Solar-ν flux
Data/SSM
[counts/(day · 100 ton)]
[108cm-2s-1]
ratio
pep
3.1
±
0
.
6
stat
±
0.3
syst
1.6
±
0.3
1.1
±
0.2
CNO
<7.9 (<7.1statonly)
<7.7
<1.5


## 5.1. The SNO and SK Legacy

After the results and analyses from 2002, it was clear that the LMA oscillation was the right solution of the long standing solar neutrino puzzle [82–93], but the activity of the SNO and SK experiments continued in the following years. The data obtained from these experiments were very important in making the LMA solution more robust and in improving the accuracy and precision of the mixing parameters determination.The so-called SNO II experiment began in June of 2001 with the addition of 2000 kg of NaCl to the 1000 metric tons ofD2O and ended in October 2003 when the NaCl was removed. The addition of salt significantly increased SNO’s efficiency (by a factor ~3 with respect to the pure D2O phase) in the detection of neutrons produced in the neutral current (NC) disintegration of deuterons by solar neutrinos and, by enhancing the energy of the γ-ray coming from neutron capture, allowed a more precise measurement of this interaction channel, well above the low-energy radioactive background. Moreover, the isotropy of the multiple γ-ray emission by neutron capture on 35Cl is different from the one of the Cˇerenkov light emitted by the single electron of the charged current interaction; therefore, by studying the event isotropy, it has been possible to separate the neutral from the charged current events without any additional assumption on the neutrino energy spectrum. The salt phase results have been reported in two main publications. In [30], referring to the first 254 live days, a global analysis including all the solar and reactor neutrino results rejected the maximal mixing hypothesis at a 5.4σ level and gave a value of the 8B neutrino flux in agreement with previous measurements and with SSMs. These results were essentially confirmed (even if with a small shift towards larger values of the mixing angle) by the second publication [94], which included the full data of the salt phase (391 live days), analyzed in terms of the CC spectra (starting from 5.5MeV kinetic energy), and NC and ES integrated fluxes separately for day and night. The day-night asymmetry in the neutral current rate, which would be an indication of oscillation to sterile neutrinos or nonstandard interaction with matter in the earth, came out to be consistent with zero.This result confirmed also the outcome of the study performed for elastic scattering (ES) interaction above5MeV by the Super-Kamiokande collaboration [95]. The full SK-I low energy data, corresponding to 1496 live days until July 2001, were investigated analyzing the time variations of the ES rates and fitting them to the variations expected from active two neutrino oscillations. In this kind of study, the zenith angle of the solar neutrinos arriving on the detector is associated to the time variable and the full data are divided in two different time samples from which the day and night rates (D) and (N) are derived. The day-night asymmetry turned out to be ADN=2(D-N)/(D+N)=-0.021±0.020(stat.)-0.012+0.013(syst.), which is consistent with zero within 0.9σ. This value was in a good agreement also with the LMA oscillation solution, which (for the best fit parameter) predicted [95] ADN=-0.018±0.016(stat.)-0.012+0.013(syst.). The impact of Earth-matter effects on solar neutrino oscillations is an important topic, which has been widely studied in the literature with different techniques (analytical and semianalytical studies and fully numerical analyses)[96–109].The SK analysis [95, 110] also showed that the energy spectrum of the recoiling electron was consistent with an undistorted solar 8B neutrino spectrum and did not find any anomalous periodic time variation of the rates, apart from the expected seasonal variation due to the Earth’s orbit eccentricity. The SK best fit point was in quite a good agreement with the SNO results, even if SK would favor slightly larger values of tan2θ. A SNO-only analysis gave the following best fit parameters [94]: Δm122=5.0×10-5eV2, tan2θ12=0.45. Including all the other solar neutrino and the KamLAND results, the best fit was obtained for Δm122=8.0-0.4+0.6×10-5eV2, tan2θ12=0.452-0.070+0.088. The effect of KamLAND data was mainly to increase the value of Δm2 and to restrict the allowed region in the mixing parameter plane. The main difference of the global analysis done with the SNO salt phase data with respect to previous studies was the possibility to exclude at 95% CL the secondary region at even larger values of the mass differences (the so-called LMA II solution, with Δm122>10-4eV2).In the third SNO phase (November 2004–November 2006), the neutral current signal neutrons were mainly detected by means of an array of3He proportional counters deployed in the D2O and looking at the gas ionization induced by neutron capture on 3He. In this way, the fluxes correlation was reduced and the accuracy in the mixing angle determination was improved. The total active 8B neutrino flux was found [31] to be 5.54-0.31+0.33(stat)-0.34+0.36(syst)×106cm-2s-1, in agreement with previous measurements and SSMs. The ratio of the 8B neutrino flux measured with CC and NC reaction was ΦCCSNO/ΦNCSNO=0.301±0.033. The global solar neutrino experiment analysis included, in this case, also the first results coming from the Borexino experiment [111], that we discuss in Section 5.3. The best fit point moved to Δm122=4.90×10-5eV2, tan2θ12=0.437 and the uncertainty in the mixing parameter plane was still quite large. Adding the KamLAND data, the allowed region was significantly restricted (mainly for Δm2) and the marginalized 1σ regions were Δm122=7.59-0.21+0.19×10-5eV2, tan2θ12=0.469-0.041+0.047.A subsequent joint reanalysis of SNO I and SNO II data, known as LETA (low energy threshold analysis) [112], succeeded, with improved calibration and analysis techniques, in lowering the energy threshold, with respect to previous analyses [94, 113], down to an effective electron kinetic energy of Teff=3.5 MeV. The main effect was to increase the statistics of CC and ES and, above all, of NC events and to increase significantly the precision on both the total 8B neutrino flux and the neutrino mixing parameters. The value for the total 8B neutrino flux extracted from neutral current was ΦNC=5.14-0.20+0.21×106cm-2s-1, where the error, obtained by summing in quadrature the statistic and systematic contributions, was reduced by more than a factor of two with respect to previous publications. For SNO data alone (LETA plus SNO III), the best fit point moved to the LOW region of parameter space, but the significance level was very similar to the one of the usual LMA solution. A global fit, including all the solar and the KamLAND data, essentially confirmed, instead, the previous results [31] for Δm122 and it made possible a further improvement in the angle determination, giving, in a 2-flavor analysis, tan2θ12=0.457-0.028+0.041.In the last five years, also the Super-Kamiokande collaboration presented new analyses, including the data of the different working phases of this experiment: Super-Kamiokande II [114] (from December 2002 to October 2005) and Super-Kamiokande III (from July 2006 to August 2008) [115]. Due to the 2001 accident, which damaged some of the photomultiplier tubes, the detector sensitivity was reduced with respect to SK-I and therefore it was important to improve the methods adopted for data collection (particularly for vertex event reconstruction, angular resolution, and background reduction) and analysis. In this way, during the 548 days of SK-III a 2.1% systematic uncertainty on the total flux (corresponding roughly to two-thirds of the SK-I value) was reached. The second and third Super-Kamiokande phases essentially confirmed the SK-I results, for what concerns the absence of significant spectral distortion, the total 8B measured flux and the day-night asymmetry.Since September 2008, Super-Kamiokande is running with modernized data acquisition system (DAQ) and electronics, which allow a wider dynamic range in the measured charge and is read out via Ethernet. This phase of the experiment is denoted as Super-Kamiokande IV [116]. Thanks to the fast DAQ every hit can be recorded and the resulting data stream analyzed by an online computer system that finds timing coincidences which are saved as triggers. As a consequence, Super-Kamiokande’s energy threshold is now only limited by computing speed and the event reconstruction. The present event reconstruction is able to reconstruct electrons with a total energy of 3 MeV or more. The computing speed limits the energy threshold to 4.2 MeV which is just below the threshold of Super-Kamiokande I and III (4.5 MeV). The same water flow techniques developed during Super-Kamiokande III result in an observed solar neutrino elastic scattering peak between 4 and 4.5 MeV total recoil electron energy. Special techniques are developed to discriminate the signal from the background, taking advantage from the fact that the background is mainly due to β emission from 214Bi and it is characterized by a larger Coulomb multiple scattering. This makes possible a reduction of about 10–15% of the statistical uncertainty and this method can also be applied to previous phases of the experiment. The additional systematic uncertainty of this method is under investigation.


## 5.2. The Impact of KamLAND Results on Solar Neutrino Physics

Even if it is based on the analysis of a reactor antineutrino beam, the KamLAND experiment played a fundamental role in the solution of the long standing solar neutrino puzzle. In fact, the first KamLAND data [34] were determinant, in conjunction with the previous solar neutrino experiments (and mainly with SNO) and assuming CPT invariance, to prove the validity of the oscillation hypothesis and to select the LMA solution as the correct one.Between March 2002 and January 2004, a new set of data were collected and the KamLAND collaboration performed a study including also a reanalysis of the previous data. During the 2002–2004 campaign, important upgrades were done both on the central detector (increasing the photocatode coverage and improving the energy resolution) and in the analysis techniques (reduction of the background with better techniques in the event selection cuts based on the time, position, and geometry of the events). The number of antineutrino events above2.6 MeV expected in absence of antineutrino disappearance was 365.2±23.7(syst) and the 258 observed events corresponded to a ν-e survival probability equal to 0.658±0.044(stat)±0.047(syst). The energy spectrum analysis was in disagreement with the no oscillation hypothesis at 99.6% statistical significance. In [39], the KamLAND collaboration, looking at the L0/E spectrum dependence (where L0 is the source-detector distance and E the ν-e energy), performed also an interesting study of other alternative hypotheses (like decoherence and decay) for neutrino disappearance. The oscillation hypothesis offered by far the best explanation of the spectrum shape, as one can see from Figure 3.Figure 3
Ratio of the observedν-e spectrum to the expectation for nooscillation versus L0/E. The curves show the expectation for the best-fit oscillation, best-fit decay, and best-fit decoherence models, taking into account the individual time-dependent flux variations of all reactors and detector effects. Taken from [39].As shown in Figure4(a), the best fit obtained from the data analysis was in the so-called LMAI region (with values of Δm122 around 8·10-5eV2) and the alternative solution at higher Δm122 (around 2·10-4eV2) was strongly disfavoured, at 98% CL, mainly due to the spectrum distortions. The KamLAND data alone were not sufficient to solve completely the ambiguity on the mixing angle values and to exclude maximal mixing. However, including in the analysis also the results coming from solar neutrino experiments, the allowed values of the angle were significantly restricted (see Figure 4(b)) and the two-flavor combined analysis gave Δm122=7.9-0.5+0.6·10-5eV2, tan2θ12=0.40-0.07+0.10 at a 1σ level.(a) Allowed region of the neutrino oscillation parameter from KamLAND antineutrino data (colored regions) and solar neutrino experiments (lines) [30]. (b) the result of a combined two-neutrino oscillation analysis of KamLAND and the observed solar neutrino fluxes under the assumption of CPT invariance. Taken from [39].
(a)
(b)The next KamLAND analysis [40] included also, in addition to the one of [34, 39], the new data collected up to May 2007. The increase in data collection was significant (also thanks to enlarging the radius of the fiducial volume from 5.5 to 6 m) and there was a reduction of systematic uncertainties, in the number of target protons and the background. The total uncertainty on Δm212 was around 2%, mainly due to the distortion of the energy scale in the detector. The total uncertainty, 4.1%, on the expected event rate was due to different sources (above all the definition of the detector fiducial volume and energy threshold, the ν-e spectra, and the reactor power) and it affected primarily the mixing angle determination. The different background sources were studied and reduced further. The most important one was the 13C(α,n)16O reaction made possible by the α decay of 210Po (a daughter of 222Rn) introduced in the liquid scintillator during the construction, which produces neutrons with energies up to 7.3MeV.The results of the statistical analysis are reported in Figure5, taken from [40]. The allowed oscillation parameter values were Δm212=7.58-0.13+0.14(stat)-0.15+0.15(syst)·10-5eV2 for the mass eigenvalues and tan2θ12=0.56-0.07+0.10(stat)-0.06+0.10(syst), for tan2θ12<1 and the no oscillation hypothesis was excluded at 5σ. The extension to the three-neutrino oscillation analysis had the main effect to enlarge the uncertainty on θ12, leaving Δm122 substantially unchanged. Figure 5, taken from [40], shows that the effect of the inclusion in the analysis of the data from SNO [94] and previous solar neutrino experiments was essential to reduce the interval of allowed θ12 values and also to move the best-fit point towards slightly lower values of the mixing angle.Figure 5
Allowed region for neutrino oscillation parameters from KamLAND and solar neutrino experiments. The side-panels show theΔχ2-profiles for KamLAND (dashed) and solar experiments (dotted) individually, as well as the combination of the two (solid). Taken from [40].Figure6 (taken from [40]) illustrates, instead, the ν-e survival probability, as a function of the ratio L0/E between the average baseline and the antineutrino energies. One can notice that the observed spectrum (after subtraction of background and geoneutrino signals), reproduces correctly the general shape of the expected oscillation cycle, with a slight excess of low energy antineutrinos, that could be interpreted as geoneutrinos.Figure 6
Ratio of the background and geo-neutrino-subtractedν-e spectrum to the expectation for no oscillation as a function of L0/E. L0 is the effective baseline taken as a flux-weighted average (L0 = 180 km). The energy bins are equal probability bins of the best fit including all backgrounds. The histogram and curve show the expectation accounting for the distances to the individual reactors, time-dependent flux variations, and efficiencies. The error bars are statistical only and do not include, for example, correlated systematic uncertainties in the energy scale. Taken from [40].


## 5.3. Toward the Sub-MeV Analysis: The Borexino Detector and Its Measurements

In the last decade, significant steps forward have been done in the knowledge of solar neutrino properties, thanks mainly to the results obtained by the kiloton scaleCˇerenkov detectors (SK and SNO) and by advent of the reactor neutrino experiment KamLAND. However, these experiments investigated only the energy part of solar neutrino spectrum above 5 MeV, which represents a small fraction of the full spectrum. The single components of the neutrino spectrum cannot be determined by such techniques at low energies and, therefore, up to the last four years, low energy neutrinos had been observed only via radiochemical methods. A significant change took place with the advent of Borexino, a real-time experiment which opened the way to the investigation of the sub-MeV region and isolated for the first time the neutrinos corresponding to the monochromatic beryllium line.


### 5.3.1. The Borexino Detector

Borexino is an ultrahigh radiopure large volume liquid scintillator detector (using pseudocumene—PC (1,2,4-trimethylbenzene)—as aromatic scintillation solvent, and PPO (2,5-diphenyloxazole) as solute at a concentration of 1.5 g/L) located underground at the italian Gran Sasso National Laboratories (LNGS), under about 1400 m of rock (3800 mwe) [117]. The employment of a liquid scintillator as target mass assures a light production sufficient to observe low energy neutrino events via elastic scattering by electrons. This reaction is sensitive to all neutrino flavors, through the neutral current interaction, but the cross-section for νe is larger than νμ and ντ by a factor of 5-6, due to the combination of charged and neutral currents. The main goal of Borexino is the measurement of the monoenergetic (0.862MeV) 7Be neutrinos, which have the basic signature of the Compton-like edge of the recoil electrons at 665 keV (see Figure 7).Figure 7
Neutrino spectra expected in Borexino (accounting for the detector’s energy resolution). The upper line represents the neutrino signal rate in Borexino according to the most recent predictions of the standard solar model [118] including neutrino oscillations with the LMA-MSW parameters. The lower line illustrates the contribution due to 7Be neutrinos. The pp neutrinos contribute to the spectrum below 0.3 MeV and the edge at 1.2 MeV is due to pep neutrinos (from [119]).The high light yield typical of a liquid scintillator makes it possible to reach a low energy threshold, a good energy resolution of about5% at 1 MeV, and a pulse shape discrimination between α and β decays. On the other hand, no directionality is possible and it is also not possible to distinguish neutrino scattered electrons from electrons due to natural radioactivity. For this reason, an extremely low level of radioactive contamination is compulsory and this has been one of the main tasks and technological achievements of the experiment. The background due to the presence of β decay of 14C (βend-point 156 keV), intrinsic to the scintillator, limits neutrino observation to energies above 200 keV. Techniques for the scintillator purification are based mainly on methods developed and tested in earlier studies with the counting test facility (CTF), a 4-ton prototype of Borexino which demonstrated for the first time the feasibility of achieving the low backgrounds needed to detect solar neutrinos in a large-scale scintillator [120–122]. For Borexino, a larger purification plant was developed similar to the CTF system, but with several improved features including the use of high vacuum and precision cleaning techniques.The design of Borexino is based on the principle of graded shielding (onion-like structure—see Figure8).Figure 8
Schematic view of the Borexino detector.The scintillator (≈300 tons) is contained in a thin nylon inner vessel (IV), of radius 4.25 m, at the center of a set of concentric shells of increasing radiopurity and it is surrounded by an outer vessel (OV), filled with PC and 5.0 g/L DMP (dimethyl phthalate), a material which is able to quench the residual scintillation of PC and acts as a passive shield against radon and other background contaminations originating from the external parts. A third more external vessel is composed of a stainless steel sphere (SSS), enclosing the passive shield (PC-DMP), and the entire detector is contained in a dome-shape structure 16.9 m high with a radius of 9 m, filled with ultrapure water, denominated water tank (WT). The scintillation light is recorded by 2212 8-inches photomultipliers distributed on the inner part of the SSS [123, 124]; 1828 of them are equipped with aluminum light concentrators designed to increase the light collection efficiency [125]. Čerenkov’s light and residual background scintillation in the buffer are thus reduced. The others 384 photomultipliers without concentrators are used to study this background and to identify muons that cross the buffer and not the inner vessel. The water tank is equipped with 208 8-inches photomultipliers and acts as a Čerenkov muon detector. Although the muon flux is reduced by a six-order of magnitude by the 3800 mwe depth of the Gran Sasso Laboratory is still significant (1.1 μm-2 h-1). An additional reduction, of the order of about 104, has been necessary; for more details see [126].In order to remove contaminants from dust (U, Th, K), air (Ar39, Kr85), and cosmogenically produced isotopes (Be7), different purification techniques were applied, such as distillation, water extraction, nitrogen stripping, and ultrafine filtration. The pseudocumene was distilled in-line during the detector filling at 80 mbar and at a temperature of about 90–95°C. Distilled pseudocumene was stripped in an 8 m high (15 cm in diameter) packed column with specially prepared ultralow Ar/Kr nitrogen (0.005 ppm Ar and 0.06 ppt Kr, see [127]). Position reconstruction of the events, as obtained from the photomultipliers timing data via a time-of-flight algorithm, allowed to define a fiducial spherical volume, corresponding approximately to 1/3 (i.e., about 100 tons) of the scintillator volume in order to reject external γ background. The others 2/3 of the scintillator act as an active shield.


### 5.3.2. The Measurement of the7Be Line

The Borexino collaboration started taking data in May 2007 and after only 3 months (47.4 live days) it was able to extract the7Be signal from the background. The best value estimate for the rate was 47±7(stat)±12(syst) counts/(day · 100 ton), where the systematic error is mainly due to the fiducial mass determination [119]. An update of the 7Be signal was reported after 9 months from an analysis of 192 live days (from May 16 2007 to April 12 2008), corresponding to 41.3 ton · yr fiducial exposure to solar neutrinos.The severe cuts that had to be passed by the events in order to be selected and enter the analysis were mainly designed to avoid pile up of multiple events and reject the events originated by muons and their daughters and the ones due to radon daughters preceding theα-β Bi-Po delayed coincidences. Moreover, severe cuts (radial and based on the z-coordinates) were finalized to reduce the external γ background. The remaining fiducial mass was of about 79 metric tons. Important background sources were the fast coincidence decays from the 238U chain (contamination level of (1.6±0.1)10-17 g/g) and the 232Th chain (contamination level of (6.8 ± 1.5) 10−18 g/g) and the 85Kr contained in the scintillator that produces the rare decay sequence 85Kr→85mRb+e-+ν-e,85mRb→85Rb+γ. The total estimated systematic error was 8.5% [111], mainly determined by two sources, introducing an uncertainty of 6% each: the total uncertainty on the fiducial mass and the one on the response function. The best value for the interaction rate of the 0.862 MeV 7Be solar neutrinos was 49±3(stat)±4(syst) counts/(day · 100 ton). This result excludes at the 4σ CL the no oscillation hypothesis for 7Be solar neutrinos, which in the high metallicity SSM [118, 128] would imply 74±4 counts/(day · 100 ton). The Borexino result is, instead, in a very good agreement with the predictions of the LMA oscillation solution: 48±4 counts/(day · 100 ton).In order to reduce the systematic uncertainties and to tune the reconstruction algorithm and Monte Carlo simulations, a calibration campaign was performed in 2009 introducing inside the Borexino detector several internal radio sourcesα’s, β’s, γ’s, and neutrons, at different energies and in hundreds of different positions, which were determined with a precision better than 2 cm. The previous systematic error on 7Be solar neutrino flux was estimated to be [111] at the level of 6% for both the fiducial volume and the energy scale (when thermal neutrons are captured by protons a 2.2 MeV γ-ray is generated.) In the calibration campaign, the detector energy response was studied with eight γ sources and Am-Be neutron source and comparing the calibration data and Monte Carlo simulations at different energies within the solar neutrinos energy region. The energy scale uncertainty, obtained with these studies, was determined to be less than 1.5%.The inaccuracy of the position (reduced by means of studies withα and β events) was less than 3 cm, equivalent to a systematic error of 1.3% for the overall fiducial volume in the 7Be solar neutrino energy region. The analyzed data set run from May 2007 to May 2010, with a fiducial exposure equivalent to 153.6 ton · year. In order to extract the 7Be solar neutrino signal, the spectral fit was applied assuming all the intrinsic background components such as 85Kr, 210Bi, 14C, and 11C. The 7Be solar neutrino rate was evaluated to be 46.0±1.5(stat)-1.6+1.5(syst) counts/day · 100 ton [129]. Thanks to the calibration campaign, the systematic error was reduced to 2.7% and the total uncertainty to 4.3%.


## 5.3.1. The Borexino Detector

Borexino is an ultrahigh radiopure large volume liquid scintillator detector (using pseudocumene—PC (1,2,4-trimethylbenzene)—as aromatic scintillation solvent, and PPO (2,5-diphenyloxazole) as solute at a concentration of 1.5 g/L) located underground at the italian Gran Sasso National Laboratories (LNGS), under about 1400 m of rock (3800 mwe) [117]. The employment of a liquid scintillator as target mass assures a light production sufficient to observe low energy neutrino events via elastic scattering by electrons. This reaction is sensitive to all neutrino flavors, through the neutral current interaction, but the cross-section for νe is larger than νμ and ντ by a factor of 5-6, due to the combination of charged and neutral currents. The main goal of Borexino is the measurement of the monoenergetic (0.862MeV) 7Be neutrinos, which have the basic signature of the Compton-like edge of the recoil electrons at 665 keV (see Figure 7).Figure 7
Neutrino spectra expected in Borexino (accounting for the detector’s energy resolution). The upper line represents the neutrino signal rate in Borexino according to the most recent predictions of the standard solar model [118] including neutrino oscillations with the LMA-MSW parameters. The lower line illustrates the contribution due to 7Be neutrinos. The pp neutrinos contribute to the spectrum below 0.3 MeV and the edge at 1.2 MeV is due to pep neutrinos (from [119]).The high light yield typical of a liquid scintillator makes it possible to reach a low energy threshold, a good energy resolution of about5% at 1 MeV, and a pulse shape discrimination between α and β decays. On the other hand, no directionality is possible and it is also not possible to distinguish neutrino scattered electrons from electrons due to natural radioactivity. For this reason, an extremely low level of radioactive contamination is compulsory and this has been one of the main tasks and technological achievements of the experiment. The background due to the presence of β decay of 14C (βend-point 156 keV), intrinsic to the scintillator, limits neutrino observation to energies above 200 keV. Techniques for the scintillator purification are based mainly on methods developed and tested in earlier studies with the counting test facility (CTF), a 4-ton prototype of Borexino which demonstrated for the first time the feasibility of achieving the low backgrounds needed to detect solar neutrinos in a large-scale scintillator [120–122]. For Borexino, a larger purification plant was developed similar to the CTF system, but with several improved features including the use of high vacuum and precision cleaning techniques.The design of Borexino is based on the principle of graded shielding (onion-like structure—see Figure8).Figure 8
Schematic view of the Borexino detector.The scintillator (≈300 tons) is contained in a thin nylon inner vessel (IV), of radius 4.25 m, at the center of a set of concentric shells of increasing radiopurity and it is surrounded by an outer vessel (OV), filled with PC and 5.0 g/L DMP (dimethyl phthalate), a material which is able to quench the residual scintillation of PC and acts as a passive shield against radon and other background contaminations originating from the external parts. A third more external vessel is composed of a stainless steel sphere (SSS), enclosing the passive shield (PC-DMP), and the entire detector is contained in a dome-shape structure 16.9 m high with a radius of 9 m, filled with ultrapure water, denominated water tank (WT). The scintillation light is recorded by 2212 8-inches photomultipliers distributed on the inner part of the SSS [123, 124]; 1828 of them are equipped with aluminum light concentrators designed to increase the light collection efficiency [125]. Čerenkov’s light and residual background scintillation in the buffer are thus reduced. The others 384 photomultipliers without concentrators are used to study this background and to identify muons that cross the buffer and not the inner vessel. The water tank is equipped with 208 8-inches photomultipliers and acts as a Čerenkov muon detector. Although the muon flux is reduced by a six-order of magnitude by the 3800 mwe depth of the Gran Sasso Laboratory is still significant (1.1 μm-2 h-1). An additional reduction, of the order of about 104, has been necessary; for more details see [126].In order to remove contaminants from dust (U, Th, K), air (Ar39, Kr85), and cosmogenically produced isotopes (Be7), different purification techniques were applied, such as distillation, water extraction, nitrogen stripping, and ultrafine filtration. The pseudocumene was distilled in-line during the detector filling at 80 mbar and at a temperature of about 90–95°C. Distilled pseudocumene was stripped in an 8 m high (15 cm in diameter) packed column with specially prepared ultralow Ar/Kr nitrogen (0.005 ppm Ar and 0.06 ppt Kr, see [127]). Position reconstruction of the events, as obtained from the photomultipliers timing data via a time-of-flight algorithm, allowed to define a fiducial spherical volume, corresponding approximately to 1/3 (i.e., about 100 tons) of the scintillator volume in order to reject external γ background. The others 2/3 of the scintillator act as an active shield.


## 5.3.2. The Measurement of the7Be Line

The Borexino collaboration started taking data in May 2007 and after only 3 months (47.4 live days) it was able to extract the7Be signal from the background. The best value estimate for the rate was 47±7(stat)±12(syst) counts/(day · 100 ton), where the systematic error is mainly due to the fiducial mass determination [119]. An update of the 7Be signal was reported after 9 months from an analysis of 192 live days (from May 16 2007 to April 12 2008), corresponding to 41.3 ton · yr fiducial exposure to solar neutrinos.The severe cuts that had to be passed by the events in order to be selected and enter the analysis were mainly designed to avoid pile up of multiple events and reject the events originated by muons and their daughters and the ones due to radon daughters preceding theα-β Bi-Po delayed coincidences. Moreover, severe cuts (radial and based on the z-coordinates) were finalized to reduce the external γ background. The remaining fiducial mass was of about 79 metric tons. Important background sources were the fast coincidence decays from the 238U chain (contamination level of (1.6±0.1)10-17 g/g) and the 232Th chain (contamination level of (6.8 ± 1.5) 10−18 g/g) and the 85Kr contained in the scintillator that produces the rare decay sequence 85Kr→85mRb+e-+ν-e,85mRb→85Rb+γ. The total estimated systematic error was 8.5% [111], mainly determined by two sources, introducing an uncertainty of 6% each: the total uncertainty on the fiducial mass and the one on the response function. The best value for the interaction rate of the 0.862 MeV 7Be solar neutrinos was 49±3(stat)±4(syst) counts/(day · 100 ton). This result excludes at the 4σ CL the no oscillation hypothesis for 7Be solar neutrinos, which in the high metallicity SSM [118, 128] would imply 74±4 counts/(day · 100 ton). The Borexino result is, instead, in a very good agreement with the predictions of the LMA oscillation solution: 48±4 counts/(day · 100 ton).In order to reduce the systematic uncertainties and to tune the reconstruction algorithm and Monte Carlo simulations, a calibration campaign was performed in 2009 introducing inside the Borexino detector several internal radio sourcesα’s, β’s, γ’s, and neutrons, at different energies and in hundreds of different positions, which were determined with a precision better than 2 cm. The previous systematic error on 7Be solar neutrino flux was estimated to be [111] at the level of 6% for both the fiducial volume and the energy scale (when thermal neutrons are captured by protons a 2.2 MeV γ-ray is generated.) In the calibration campaign, the detector energy response was studied with eight γ sources and Am-Be neutron source and comparing the calibration data and Monte Carlo simulations at different energies within the solar neutrinos energy region. The energy scale uncertainty, obtained with these studies, was determined to be less than 1.5%.The inaccuracy of the position (reduced by means of studies withα and β events) was less than 3 cm, equivalent to a systematic error of 1.3% for the overall fiducial volume in the 7Be solar neutrino energy region. The analyzed data set run from May 2007 to May 2010, with a fiducial exposure equivalent to 153.6 ton · year. In order to extract the 7Be solar neutrino signal, the spectral fit was applied assuming all the intrinsic background components such as 85Kr, 210Bi, 14C, and 11C. The 7Be solar neutrino rate was evaluated to be 46.0±1.5(stat)-1.6+1.5(syst) counts/day · 100 ton [129]. Thanks to the calibration campaign, the systematic error was reduced to 2.7% and the total uncertainty to 4.3%.


## 5.4. Thepep and CNO Neutrinos Measurement in Borexino

In the SSM, due to the solar luminosity constraint and their intimate link to thepp neutrinos [43, 56], the monoenergetic 1.44 MeV pep neutrinos have one of the smallest uncertainties (1.2%) [64]. For this reason, after the pp neutrinos, they constitute the ideal probe to test SSM hypotheses. On the other hand, the detection of neutrinos within the CNO-bicycle is central to probe the solar core metallicity and contribute in this way to the solution of the solar metallicity problem [64, 130]. Also, they are believed to fuel massive stars with mass greater than ~1.2M⊙ during the main sequence evolution and also stars with lower masses in more advanced stages of evolution. The energy spectrum of neutrinos from the CNO-bicycle is the result of three continuous spectra with end point energies of 1.19 MeV (13N), 1.73 MeV (15O), and 1.74 MeV (17F). Despite their relevance, until 2011, no pep and CNO neutrinos had been detected directly.The electron recoil energy spectrum frompep neutrino interactions in Borexino is a Compton-like shoulder with end point of 1.22 MeV, as one can see from Figures 9 and 10, showing the pep and CNO contribution in Borexino.Examples of fitted spectra; the fit results in the legends have units [counts/(day· 100 ton)]. (a): A Monte Carlo based fit over the energy region 270–1600 keV to a spectrum from which some, but not all, of the α events have been removed using a PSA cut, and in which the event energies were estimated using the number of photons detected by the PMT array. (b): An analytic fit over the 290–1270 keV energy region to a spectrum obtained with statistical α subtraction and in which the event energies were estimated using the total charge collected by the PMT array. In all cases the fitted event rates refer to the total rate of each species, independently from the fit energy window (from [129]).
(a)
(b)Figure 10
The neutrino-induced electron recoil spectra expected in Borexino. The total rates are those predicted by the latesthigh-Z solar model [64]. The pep and CNO neutrinos recoil spectra with end points in the region 1.2–1.5 MeV are shown. Also the 7Be neutrinos (measured in [129]), with a count rate about 10 times larger, are shown for comparison. Note that the variable on the x-axis is not directly the energy value. Taken from [131].As already mentioned, very low background levels [111, 119] are required to detect 7Be neutrinos; the detection of pep and CNO neutrinos is even more challenging, as their expected interaction rates are ~10 times lower. The expected rate is on the order of a few counts per day in a 100-ton target. To detect pep and CNO neutrinos, the Borexino collaboration adopted a novel analysis procedure to suppress the dominant background in the 1-2 MeV energy range, due to the cosmogenic β+-emitter 11C produced within the scintillator by muon interactions with 12C nuclei. The muon flux crossing the Borexino detector, ~4300 μ/day, yields a 11C production rate of ~27 counts/(day · 100 ton) (In 95% of the cases at least one free neutron is spalled in the 11C production process [132], and then captured in the scintillator with a mean time of 255 μs [133].) This background can be reduced by performing a space and time veto following coincidences between signals from the muons and the cosmogenic neutrons [134, 135], discarding exposure that is more likely to contain 11C due to the correlation between the parent muon, the neutron, and the subsequent 11C decay (the three-fold coincidence, TFC). The TFC technique is based on the reconstructed track of the muon and the reconstructed position of the neutron-capture γ-ray [133]. The criteria of rejection were applied to obtain the best compromise between 11C rejection and preservation of fiducial exposure, resulting in a 11C rate of (2.5±0.3) count per day and (9±1)% of the original rate, while preserving 48.5% of the initial exposure.Figure11 shows the resulting spectrum obtained with data collected between January 2008 and May 2010, corresponding to a fiducial exposure of 20409 ton · day [74]. Despite the TFC veto, the number of 11C surviving events still constituted a significant background.Figure 11
Energy spectra of the events in the FV before and after the TFC veto is applied. The solid and dashed blue lines show the data and estimated11C rate before any veto is applied. The solid black line shows the data after the procedure, in which the 11C contribution (dashed) has been greatly suppressed. The next largest background, 210Bi, and the electron recoil spectra of the best estimate of the pep neutrino rate and of the upper limit of CNO neutrino rate are shown for reference. Rate values in the legend are quoted in counts/(day · 100 ton) from [74].To discriminate11C β+ decays from neutrino-induced e- recoils and β- decays, the pulse shape differences between e- and e+ interactions in organic liquid scintillators [136, 137] were exploited. In fact a small difference in the time distribution of the scintillation signal arises from the finite lifetime of orthopositronium as well as from the presence of annihilation γ-rays, which present a distributed, multisite event topology and a larger average ionization density than electron interactions. The Borexino collaboration employed an optimized pulse shape parameter using a boosted-decision-tree algorithm [138] and trained with a TFC-selected set of 11C events (e+) and 214Bi events (e-) selected by the fast 214Bi-214Po α-β decay sequence (less than 2.8 m from the detector center and with a vertical position relative to the detector center between −1.8 m and 2.2 m.) In a work published in 2012 [74], the Borexino collaboration presented the results of an analysis based on a binned likelihood multivariate fit performed on the energy, pulse shape, and spatial distributions of selected scintillation events whose reconstructed position is within the fiducial volume.The energy spectra and spatial distribution of the externalγ-ray backgrounds have been obtained from a full, Geant4-based Monte Carlo simulation and validated with calibration data from a high-activity 228Th source [139] deployed in the outermost buffer region, outside the active volume. α events were removed from the energy spectrum by the statistical subtraction method [119]. In the energy region of interest of the fit procedure all background species whose rates were estimated to be less than 5% of the predicted rate from pep neutrinos have been excluded (electron recoils from 7Be, pep, and CNO solar neutrinos, internal radioactive backgrounds 210Bi, 11C, 10C, 6He, 40K, 85Kr, and 234mPa, and external γ-rays from 208Tl, 214Bi, and 40K.) All rates were constrained to positive values and thirteen species were left free in the fit. The rate of the radon daughter 214Pb was fixed using the measured rate of 214Bi-214Po delayed coincidence events. The contribution from pp solar neutrinos was fixed to the SSM assuming MSW-LMA [140–145] with tan2θ12=0.47-0.04+0.05, Δm122=(7.6±0.2)·10-5 eV2 [146], and the contribution from 8B neutrinos to the rate from the measured flux [112, 147].In Table6, the results for the pep and CNO neutrino interaction rates are shown. The absence of a pep neutrino signal was rejected at 98% CL. Concerning the CNO neutrinos flux, its electron-recoil spectrum is similar to the spectral shape of 210Bi, but the last one is about 10 times greater; therefore, it has only been possible to provide an upper limit on the CNO neutrino interaction rate. The 95% CL limit reported in Table 6 has been obtained from a likelihood ratio test with the pp neutrino rate fixed to the SSM prediction [64] under the assumption of MSW-LMA, (2.80±0.04) counts/(day · 100 ton).Table 6
Best estimates for thepep and CNO solar neutrino interaction rates. For the results in the last two columns both statistical and systematic uncertainties are considered. Total fluxes have been obtained assuming MSW-LMA and using the scattering cross-sections from [146, 148, 149] and a scintillator e- density of (3.307±0.003)·1029ton-1. The last column gives the ratio between our measurement and the high-Z (GS98) SSM [64]. Table taken from [74].
ν
Interaction rate
Solar-ν flux
Data/SSM
[counts/(day · 100 ton)]
[108cm-2s-1]
ratio
pep
3.1
±
0
.
6
stat
±
0.3
syst
1.6
±
0.3
1.1
±
0.2
CNO
<7.9 (<7.1statonly)
<7.7
<1.5


## 6. Phenomenological Analysis

### 6.1. Status of the Determination of the Mixing Parameters in a 3-Flavor Analysis

Recently, the SNO collaboration performed a combined analysis of all the three working phases of the experiment [147] based on a fit to Monte Carlo derived probability density functions (PDFs) for each of the possible signals and backgrounds, and also introduced a new way to parametrize the 8B neutrino signal. Figure 12, reporting the results of the two-flavour (with the assumption θ13=0) SNO only analysis, shows the further improvement in the mixing parameters accuracy, but, at the same time, it confirms that the SNO results alone would not be sufficient to completely exclude the LOW solution.Figure 12
Two-flavor neutrino oscillation analysis contour using only SNO data  (taken from [147]).This ambiguity was definitely removed, as shown in Figure13, by including in the analysis the results of all previous solar neutrino experiments [110, 114, 115, 150–153], the 7Be solar neutrino rate measured by Borexino [129], the 8B neutrino spectra [154], and the KamLAND data [41] (The KamLAND data were obtained in a completely independent experiment and, therefore, the corresponding χ2 values, as functions of the mixing parameters, were directly summed to the χ2 values computed by direct solar neutrino analysis.)Figure 13
Two-flavor neutrino oscillation analysis contour using both solar neutrino and KamLAND results (taken from [147]).The higher values ofΔm122 in the LMA region were excluded, together with the full LOW solution, thanks mainly to the large discrimination power of KamLAND. This experiment, however, did not contribute significantly to improve the mixing angle determination and the accuracy on this parameter remained quite high. The results of the two-flavor analysis are reported in Table 7 (taken from [147]).Table 7
Best-fit neutrino oscillation parameters from a two-flavor neutrino oscillation analysis. Uncertainties listed are1σ after the χ2 was minimized with respect to all other parameters (taken from [147]).
Analysis
tan
2
θ
12
Δ
m
21
2
[
e
V
2
]
χ
2
/
NDF
SNO only (LMA)
0.42
7
-
0.029
+
0.033
5.6
2
-
1.36
+
1.92
×
1
0
-
5
1.39
/
3
SNO only (LOW)
0.42
7
-
0.035
+
0.043
1.3
5
-
0.14
+
0.35
×
1
0
-
7
1.41
/
3
Solar
0.42
7
-
0.028
+
0.028
5.1
3
-
0.96
+
1.29
×
1
0
-
5
108.07
/
129
Solar + KamLAND
0.42
7
-
0.024
+
0.027
7.4
6
-
0.19
+
0.20
×
1
0
-
5The slight tension between the solar neutrino experiments and KamLAND was significantly reduced by extending the analysis to the 3 flavor oscillation case as shown in Figure14, from which it is clear that the best global fit is obtained for values of θ13 different from zero.Figure 14
Three-flavor neutrino oscillation analysis contour using both solar neutrino and KamLAND results. Taken from [147].A detailed analysis of theχ2 behavior proved also that the combination of solar experiments and KamLAND enables the significant improve of the discriminating power on the θ13 mixing parameter (see Figure 15 and Table 8).Table 8
Best-fit neutrino oscillation parameters from a three-flavor neutrino oscillation analysis. Uncertainties listed are±1σ after the χ2 was minimized with respect to all other parameters. The global analysis includes Solar + KL + ATM + LBL + CHOOZ.
Analysis
tan
2
θ
12
2
Δ
m
12
2
[
e
V
2
]
sin
2
θ
13
×
1
0
-
2
Solar
0.43
6
-
0.036
+
0.048
5.1
3
-
0.98
+
1.49
×
1
0
-
5
<5.8 (95% C.L.)
Solar + KL
0.44
6
-
0.029
+
0.030
7.4
1
-
0.19
+
0.21
×
1
0
-
5
2
.
5
-
1.5
+
1.8
<5.3 (95% C.L.)
Global
2.0
2
-
0.55
+
0.88Figure 15
Projections of the three-flavor neutrino oscillation parameters. The horizontal lines represent theΔχ2 for a particular confidence level. Taken from [147].The indication in favor ofθ13 being different from zero was in agreement with the recent results from the long-baseline experiments T2 K [155] and MINOS [156], and with the combined analysis performed in [157], including also the atmospheric neutrino and the CHOOZ [158] data. Moreover, the validity of this hint has been corroborated by the data obtained this year by the short baseline neutrino reactor experiments [159–162], which established that θ13>0 at about 5σ (and even more in the Daya Bay case [163]). These experiments found values of sin2θ13 centered between 0.020 and 0.030, very promising results for future experiments looking for leptonic CP violation [164]. The impact and the possible consequences of these recent results have been discussed, among the others, in the following papers [164–167]. The different accuracy that can be reached in the determination of the mixing angle between the first and third generation, according to the different kind of neutrino experiments included in the analysis, is represented in Figure 16.Figure 16
Projection oversin2θ13 combining the projections obtained by analyzing data from all neutrino sources. The data from atmospheric, short-baseline experiments, and long-baseline experiments (ATM + LBL + CHOOZ) was determined from Figure 2 (left panel) in [157] which already includes the latest T2 K [155] and MINOS [156] results.The combined analysis of the different SNO phases was also very useful to obtain a precise determination of the8B solar neutrino flux, ΦB8=5.25±0.16(stat)-0.13+0.11(syst)×106cm-2s-1, with an important reduction of the systematic uncertainty. This result was consistent with, but more precise than, both the high-Z BPS09 (GS), Φ=(5.88±0.65)×106cm-2s-1, and low-Z BPS09(AGSS09), Φ=(4.85±0.58)×106cm-2s-1, and solar model predictions [72].The combination of the LETA analysis by the SNO collaboration [112] and of the Borexino measurements [154] made possible a detailed study of the low energy part of the 8B solar neutrino spectrum. Even if characterized by a larger uncertainty (mainly due to a more limited statistics), Borexino data confirm the LETA indication of low energy data points lower than the theoretical expectations based on matter enhanced oscillation and solar models as shown in Figure 17 (taken from [154]). These results agreed also with the Super-Kamiokande observation [110] of flat spectrum, consistent with the undistorted spectrum hypothesis. The emergence of this slight tension between theory and experiments seems to indicate the presence of new subdominant effects and also suggests the possibility of nonstandard neutrino interactions (like those studied in [168]) or the mixing with a very light sterile neutrino [169]. Future solar neutrino experiments, like SNO+, could shed more light on this subject, by performing precision measurements of lower energies solar neutrinos (like the pep neutrinos).Figure 17
In this picture, taken from [154], the final energy spectrum derived from Borexino’s analysis (red points) is represented and compared with the Monte Carlo predictions (blue and purple bands) obtained using the MSW-LMA neutrino oscillation model and the standard solar models in the versions corresponding, respectively, to the high metallicity (BPS09(GS98)) and the low metallicity (BPS09 (AGS05)) cases.


### 6.2. Free Flux Analyses

The increasing data of solar neutrinos allow to independently test the astrophysics of the solar interior and the physics of neutrino propagation. The analysis discussed in previous sections can be modified by also varying the solar neutrino fluxes in order to accommodate all neutrino data, while all the functional dependences are maintained as predicted by the standard model dependences. A key step in this kind of analysis is the imposition of the luminosity constraint [170, 171], which implements in a global way for the Sun the constraint of conservation of energy for nuclear fusion among light elements. Each neutrino flux is associated with a specific amount of energy released to the star and therefore a particular linear combination of the solar neutrino fluxes is equal to the solar luminosity (in appropriate units). One can write the luminosity constraint as
(13)L⊙4π(A.U.)2=∑i‍αiΦi,
where L⊙ is the solar luminosity measured at the Earth’s surface, 1 AU is the average Earth-Sun distance, and the coefficient αi is the amount of energy provided to the star by nuclear fusion reactions associated with each of the important solar neutrino fluxes, Φi. The coefficients αi are calculated accurately in [171].The model independent determination of the solar neutrino fluxes [172, 173] shows that present solar neutrino data leads to accurate results for four fluxes and also the correlations between them. This information allows for a consistent global comparison of SSM fluxes with the inferred fluxes by neutrino data. Present data lead to the values for the inferred solar neutrino fluxes reported in the fourth column (labelled as “Solar”) of Table 4 in Section 3. The precision of the 7Be and 8B neutrino fluxes is driven by the Borexino and SNO (SK) neutrino experiments, while the precision of the pp and pep neutrino fluxes mainly comes by the imposition of the luminosity constraint. The neutrino data directly demonstrates that the Sun shines by the pp chain. The CNO cycle only contributes to the total luminosity at the percent level.The reader may wonder how much these inferences are affected by the luminosity constraint. The idea that the Sun shines because of nuclear fusion reactions can be tested accurately by comparing the observed photon luminosity of the Sun with the luminosity inferred from measurements of solar neutrino fluxes. Moreover, this same comparison will test a basic result of the standard solar model, namely, that the Sun is in a quasi-steady state in which the current energy generation in the interior equals the current luminosity at the solar surface. The free flux analysis, without imposing luminosity constraint, permits an estimation of the solar luminosity inferred by neutrino data, which agrees with the directly measured one within 15% (1σ).


## 6.1. Status of the Determination of the Mixing Parameters in a 3-Flavor Analysis

Recently, the SNO collaboration performed a combined analysis of all the three working phases of the experiment [147] based on a fit to Monte Carlo derived probability density functions (PDFs) for each of the possible signals and backgrounds, and also introduced a new way to parametrize the 8B neutrino signal. Figure 12, reporting the results of the two-flavour (with the assumption θ13=0) SNO only analysis, shows the further improvement in the mixing parameters accuracy, but, at the same time, it confirms that the SNO results alone would not be sufficient to completely exclude the LOW solution.Figure 12
Two-flavor neutrino oscillation analysis contour using only SNO data  (taken from [147]).This ambiguity was definitely removed, as shown in Figure13, by including in the analysis the results of all previous solar neutrino experiments [110, 114, 115, 150–153], the 7Be solar neutrino rate measured by Borexino [129], the 8B neutrino spectra [154], and the KamLAND data [41] (The KamLAND data were obtained in a completely independent experiment and, therefore, the corresponding χ2 values, as functions of the mixing parameters, were directly summed to the χ2 values computed by direct solar neutrino analysis.)Figure 13
Two-flavor neutrino oscillation analysis contour using both solar neutrino and KamLAND results (taken from [147]).The higher values ofΔm122 in the LMA region were excluded, together with the full LOW solution, thanks mainly to the large discrimination power of KamLAND. This experiment, however, did not contribute significantly to improve the mixing angle determination and the accuracy on this parameter remained quite high. The results of the two-flavor analysis are reported in Table 7 (taken from [147]).Table 7
Best-fit neutrino oscillation parameters from a two-flavor neutrino oscillation analysis. Uncertainties listed are1σ after the χ2 was minimized with respect to all other parameters (taken from [147]).
Analysis
tan
2
θ
12
Δ
m
21
2
[
e
V
2
]
χ
2
/
NDF
SNO only (LMA)
0.42
7
-
0.029
+
0.033
5.6
2
-
1.36
+
1.92
×
1
0
-
5
1.39
/
3
SNO only (LOW)
0.42
7
-
0.035
+
0.043
1.3
5
-
0.14
+
0.35
×
1
0
-
7
1.41
/
3
Solar
0.42
7
-
0.028
+
0.028
5.1
3
-
0.96
+
1.29
×
1
0
-
5
108.07
/
129
Solar + KamLAND
0.42
7
-
0.024
+
0.027
7.4
6
-
0.19
+
0.20
×
1
0
-
5The slight tension between the solar neutrino experiments and KamLAND was significantly reduced by extending the analysis to the 3 flavor oscillation case as shown in Figure14, from which it is clear that the best global fit is obtained for values of θ13 different from zero.Figure 14
Three-flavor neutrino oscillation analysis contour using both solar neutrino and KamLAND results. Taken from [147].A detailed analysis of theχ2 behavior proved also that the combination of solar experiments and KamLAND enables the significant improve of the discriminating power on the θ13 mixing parameter (see Figure 15 and Table 8).Table 8
Best-fit neutrino oscillation parameters from a three-flavor neutrino oscillation analysis. Uncertainties listed are±1σ after the χ2 was minimized with respect to all other parameters. The global analysis includes Solar + KL + ATM + LBL + CHOOZ.
Analysis
tan
2
θ
12
2
Δ
m
12
2
[
e
V
2
]
sin
2
θ
13
×
1
0
-
2
Solar
0.43
6
-
0.036
+
0.048
5.1
3
-
0.98
+
1.49
×
1
0
-
5
<5.8 (95% C.L.)
Solar + KL
0.44
6
-
0.029
+
0.030
7.4
1
-
0.19
+
0.21
×
1
0
-
5
2
.
5
-
1.5
+
1.8
<5.3 (95% C.L.)
Global
2.0
2
-
0.55
+
0.88Figure 15
Projections of the three-flavor neutrino oscillation parameters. The horizontal lines represent theΔχ2 for a particular confidence level. Taken from [147].The indication in favor ofθ13 being different from zero was in agreement with the recent results from the long-baseline experiments T2 K [155] and MINOS [156], and with the combined analysis performed in [157], including also the atmospheric neutrino and the CHOOZ [158] data. Moreover, the validity of this hint has been corroborated by the data obtained this year by the short baseline neutrino reactor experiments [159–162], which established that θ13>0 at about 5σ (and even more in the Daya Bay case [163]). These experiments found values of sin2θ13 centered between 0.020 and 0.030, very promising results for future experiments looking for leptonic CP violation [164]. The impact and the possible consequences of these recent results have been discussed, among the others, in the following papers [164–167]. The different accuracy that can be reached in the determination of the mixing angle between the first and third generation, according to the different kind of neutrino experiments included in the analysis, is represented in Figure 16.Figure 16
Projection oversin2θ13 combining the projections obtained by analyzing data from all neutrino sources. The data from atmospheric, short-baseline experiments, and long-baseline experiments (ATM + LBL + CHOOZ) was determined from Figure 2 (left panel) in [157] which already includes the latest T2 K [155] and MINOS [156] results.The combined analysis of the different SNO phases was also very useful to obtain a precise determination of the8B solar neutrino flux, ΦB8=5.25±0.16(stat)-0.13+0.11(syst)×106cm-2s-1, with an important reduction of the systematic uncertainty. This result was consistent with, but more precise than, both the high-Z BPS09 (GS), Φ=(5.88±0.65)×106cm-2s-1, and low-Z BPS09(AGSS09), Φ=(4.85±0.58)×106cm-2s-1, and solar model predictions [72].The combination of the LETA analysis by the SNO collaboration [112] and of the Borexino measurements [154] made possible a detailed study of the low energy part of the 8B solar neutrino spectrum. Even if characterized by a larger uncertainty (mainly due to a more limited statistics), Borexino data confirm the LETA indication of low energy data points lower than the theoretical expectations based on matter enhanced oscillation and solar models as shown in Figure 17 (taken from [154]). These results agreed also with the Super-Kamiokande observation [110] of flat spectrum, consistent with the undistorted spectrum hypothesis. The emergence of this slight tension between theory and experiments seems to indicate the presence of new subdominant effects and also suggests the possibility of nonstandard neutrino interactions (like those studied in [168]) or the mixing with a very light sterile neutrino [169]. Future solar neutrino experiments, like SNO+, could shed more light on this subject, by performing precision measurements of lower energies solar neutrinos (like the pep neutrinos).Figure 17
In this picture, taken from [154], the final energy spectrum derived from Borexino’s analysis (red points) is represented and compared with the Monte Carlo predictions (blue and purple bands) obtained using the MSW-LMA neutrino oscillation model and the standard solar models in the versions corresponding, respectively, to the high metallicity (BPS09(GS98)) and the low metallicity (BPS09 (AGS05)) cases.


## 6.2. Free Flux Analyses

The increasing data of solar neutrinos allow to independently test the astrophysics of the solar interior and the physics of neutrino propagation. The analysis discussed in previous sections can be modified by also varying the solar neutrino fluxes in order to accommodate all neutrino data, while all the functional dependences are maintained as predicted by the standard model dependences. A key step in this kind of analysis is the imposition of the luminosity constraint [170, 171], which implements in a global way for the Sun the constraint of conservation of energy for nuclear fusion among light elements. Each neutrino flux is associated with a specific amount of energy released to the star and therefore a particular linear combination of the solar neutrino fluxes is equal to the solar luminosity (in appropriate units). One can write the luminosity constraint as
(13)L⊙4π(A.U.)2=∑i‍αiΦi,
where L⊙ is the solar luminosity measured at the Earth’s surface, 1 AU is the average Earth-Sun distance, and the coefficient αi is the amount of energy provided to the star by nuclear fusion reactions associated with each of the important solar neutrino fluxes, Φi. The coefficients αi are calculated accurately in [171].The model independent determination of the solar neutrino fluxes [172, 173] shows that present solar neutrino data leads to accurate results for four fluxes and also the correlations between them. This information allows for a consistent global comparison of SSM fluxes with the inferred fluxes by neutrino data. Present data lead to the values for the inferred solar neutrino fluxes reported in the fourth column (labelled as “Solar”) of Table 4 in Section 3. The precision of the 7Be and 8B neutrino fluxes is driven by the Borexino and SNO (SK) neutrino experiments, while the precision of the pp and pep neutrino fluxes mainly comes by the imposition of the luminosity constraint. The neutrino data directly demonstrates that the Sun shines by the pp chain. The CNO cycle only contributes to the total luminosity at the percent level.The reader may wonder how much these inferences are affected by the luminosity constraint. The idea that the Sun shines because of nuclear fusion reactions can be tested accurately by comparing the observed photon luminosity of the Sun with the luminosity inferred from measurements of solar neutrino fluxes. Moreover, this same comparison will test a basic result of the standard solar model, namely, that the Sun is in a quasi-steady state in which the current energy generation in the interior equals the current luminosity at the solar surface. The free flux analysis, without imposing luminosity constraint, permits an estimation of the solar luminosity inferred by neutrino data, which agrees with the directly measured one within 15% (1σ).


## 7. Future Solar Neutrino Experiments

### 7.1. The Near Future: Improvement ofpep Measurements and CNO Detection

In the last decades, the intensive study of8B and, more recently, 7Be solar neutrinos made possible fundamental steps forward in the solution of the solar neutrino puzzle and the determination of the neutrino mixing parameters. Nevertheless, many key features of the oscillation models (like the transition between the vacuum dominated sub-MeV region and the spectral region between 1 and 3 MeV, where matter effects become relevant) still have to be tested or verified with better accuracy and precision (see Figure 18, taken from [174]).Figure 18
Theνe survival probability is represented as a function of neutrino energy. The gray band represent the MSW-LMA prediction. The higher survival probability region at low energies is where vacuum-dominated oscillations occur. As the neutrino energy increases, matter effects become important and the lower survival probability at high energies is due to matter-enhanced oscillations. The reported data correspond to solar neutrino flux measurements performed by different experiments. Taken from [174].The apparent partial deficit of events in the low energy part of the8B spectrum suggested the introduction of new theoretical models (as discussed in Section 6). Also for these reasons, the experimental efforts in the last years focused on the detection of neutrinos of ever decreasing energies, to fully confirm the validity of the MSW-LMA solution and verify the fluxes predicted by SSMs, discriminating between different versions of these models. The fluxes of the medium and high energy neutrinos of the pp chains (7Be, 8B, and hep) are predicted with quite large uncertainties, mainly due to the uncertainties in nuclear cross-sections and solar opacity (Table 5). The pp and pep fluxes, instead, are strongly correlated between themselves and their values are predicted with the highest precision because SSMs predict that pp chain reactions are responsible for more than 99% of the energy powering the Sun [80]. Therefore, the measurements of these components would be the most stringent test of the SSM. The tight correlation between pep and pp neutrinos is theoretically well established and, therefore, even in the pessimistic hypothesis that pp neutrinos could not be measured with the desired accuracy, a significant improvement in the pep neutrinos measurement with respect to data presently available would make it possible to reduce significantly the 15% indetermination on the solar luminosity (see Section 6.2) and to test indirectly the SSM’s predictions that almost 100% of solar energy is produced by nuclear burning.As already mentioned, water Čerenkov detectors, which played a fundamental role in the solution of the solar neutrino problem, are characterized by a low photon yield [175, 176] and therefore can detect only the higher part of the spectrum (hep and 8B neutrinos with a threshold around 3.5MeV). The radiochemical experiments [153, 177] are limited, instead, by their ability to measure only the integrated neutrino rate above the charge-current interaction threshold (down to 0.23MeV for the Gallium experiments), without the possibility to discriminate between the different spectrum components. Therefore, an important contribution should come from the present and future organic liquid scintillator detectors, planned to perform low energy solar neutrino spectroscopy. To reach this goal, they will take advantage from the high values of light yield (about 104 photons per MeV of deposited energy) and from the possibility to assemble very large masses of high purity materials. The excellent levels of radiopurity, reached, for instance, at Borexino, and the typical geometry of these detectors (which are unsegmented and can be easily adapted to the definition of a fiducial volume) are fundamental to reduce the impact of the background, that is so critical due to the feebleness of the low energy signal.In the near future, significant contributions are expected from Borexino and SNO+ [178] experiments (the main problem still surviving seems to be the reduction of 210Pb.) Borexino has already proved its importance in this kind of analysis performing the first measurements of pep and CNO neutrinos (even if the level accuracy is not yet the desired one) and further reducing, with the purification campaign started since July 2010, the level of contamination from almost all of the main radioactive background sources. The purification efforts are still ongoing and should make possible a further improvement on the accuracy of the signal extraction. Also, a novel technique [179] would allow to determine the 210Bi background. Preliminary calculations show that the CNO signal could be extracted from the 210Bi background with one year of data taking. The SNO+ experiment, that should start taking data soon in the SNOLAB, should take advantage from the location (about two times deeper underground than the Gran Sasso laboratory), with the consequent lower muon flux and a strongly reduced 11C rate. Moreover, thanks to the detector mass (about three times larger than in Borexino), it should be able to reach a higher counting rate. This could determine a fundamental improvement at least in the case of the pep neutrino measurement, where a 5% uncertainty is expected, to a level that should make possible a significant test of the MSW transition region.In the more optimistic scenarios, it may be also possible to attack the main problem of measuring the lowest energy parts of the solar neutrino spectrum, that is, thepp neutrinos and the 0.38MeV Berillium line. In any case, the presence in organic scintillators of an intrinsic 14C background will make this very low energy measurements an extremely hard task and they may require the introduction of new techniques, like the ones we are going to describe in the next subsections.


### 7.2. The Far Future: Experimental Challenges

The challenge for all future experiments aimed at measuring the low energy part of solar neutrino spectrum is that of assembling experimental devices with low energy thresholds suitable to detect a low rate signal in a region characterized by different potential sources of radioactive background. This difficult experimental task is common also to the experiments looking for neutrinoless doubleβ decay or for dark matter signals (search for signatures of WIMPs, a stable or long-lived weakly interacting elementary particle, produced in the early Universe, whose existence is predicted in extensions of the standard model). In fact, some of the solar neutrino experiments planned for the future are multipurpose experiments designed also for the other above-quoted topics.They are all characterized by a very large detector target mass and by the need to reach very high levels of radiopurity. The common feature is that of using scintillator detectors, but they differ for the chosen active scintillator material, which can vary from traditional organic scintillators (developed with the use of innovative technological devices) to new materials, like the noble gases.


#### 7.2.1. Noble Liquid Detectors: CLEAN and XMASS

One of the possible future frontiers is the idea to use scintillation detectors with liquid noble gases, like xenon, argon, and neon. These materials have the advantage of being relatively inexpensive, easy to obtain, and dense and it is not too difficult to build large homogeneous detectors of this kind; moreover, they can be quite easily purified, offer very high scintillation yields (about 30–40 photons/keV), and do not absorb their own scintillation light.A first example is offered by the CLEAN/DEAP family, a series of detectors based entirely on scintillation in liquid neon (LNe) and liquid argon (LAr). They have been realized using a scaleable technology in order to reach increasing sensitivities in the different prototypes realized and installed in the SNOLAB (Pico-CLEAN, Micro-CLEAN, DEAP-I, Mini-CLEAN and CLEAN/DEAP) with the aim to search for dark matter and to perform (through the analysis of elastic neutrino-electron and neutrino-nucleus scattering) a real-time measurement of thepp solar neutrino flux. The final detector CLEAN (cryogenic low energy astrophysics with noble gases) [180] (see Figure 19) will be made by a stainless steel tank, of about 6 meters of diameter, filled with 135 metric tons of cryogenic liquid neon; only the central part of it, surrounded isotropically by a series of photomultipliers, will constitute the detector fiducial volume. An external tank of water, 10 metres wide and 12 metres high, will act as γ-ray shielding, neutron shielding, and muon veto. According to Monte Carlo simulations, there should be a production of 15000 photons/MeV and it should be possible to reach a 100% photon wavelength shifter efficiency and a statistical uncertainty on the pp measurements of the order of 1%.Figure 19
Scheme of the CLEAN detector. Taken from [180].A precise measurement of thepp component and of the ratio between pp and 7Be fluxes would be essential to test the predictions of SSMs. A high accuracy on the pp neutrino flux would also make possible a better determination of the θ12 mixing angle, which, complemented with the results from previous solar neutrino experiments and from KamLAND (essential for the Δm122 measurement), would be fundamental to test the consistency of the LMA solution also in the region of transition between vacuum dominated and matter enhanced oscillations. Finally, CLEAN could in principle try to measure also the CNO neutrino flux, through the analysis of neutrino spectrum from 0.7 to 1.0 MeV, with an estimated accuracy between 10% and 15%.An interesting alternative to the use of neon is offered by liquid xenon scintillator detectors [181], which take advantage of the fact that among liquid rare gases xenon has the highest stopping power for penetrating radiation (thanks to its high atomic number, A≃131, and density, ρ=3g/cm3) and also the highest ionization and scintillation yield. The technological improvements of the last twenty to thirty years made possible significant improvements in the cooling and purification techniques of this kind of detectors and in the possibility of assembling large mass detectors, of the order of some tons (like in the case of MEG [182] experiment, studying the μ→eγ decay).The XMASS experiment (see Figure20) is a multipurpose low background and low energy threshold experiment that will use a large massive liquid xenon detector and has been designed to look for WIMPs (dark matter candidates), search for neutrinoless double β decay, and study the pp and the 7Be solar neutrinos. After two preliminary phases, during which smaller prototypes have been realized and installed in the Kamioka mine [183], and the first data on double beta decay and dark matter have been taken, the full XMASS detector (that will measure also solar neutrinos) will have a total mass of 20 metric tons,with a fiducial volume of 10 metric tons. Special efforts are required mainly to lower the background, by reducing the radioactive contamination in the parts used for detector construction (with special attention to the photomultipliers and the copper material used for PMT holder), constructing a larger pure water active shield (for muons and mainly neutrons and γ rays), and, above all, developing a distillation system for xenon in order to reduce the contamination by 85Kr, the major source of radioactive background inside the detector.Schematic view of the full XMASS facility (a) and details of the inner detector (b) from which one can see the particular configuration of the hexagonal photomultiplier tubes. Taken from [183, 184].
(a)
(b)Another interesting experimental project based on the noble gases liquid scintillator technique is that of DARWIN (dark matter wimp search with noble liquids) [185], which brings together different European and US research groups working on existing experiments and on the study for a future multiton scale LAr and LXe dark matter search facility in Europe. The main goal of the experiment is to look for a WIMP signal and to demonstrate its dark matter nature, taking advantage from the fact of performing the measurement with multiple different targets operating under similar conditions. In this way, it should be possible to estimate the dependence of the rate with the target material and, therefore, to better determine the WIMP candidate mass and to distinguish between spin independent and spin dependent couplings. The energy region of the nuclear recoil spectrum, below 200 keV, that should be investigated by this future experiment is of particular interest also for the study of the pp solar neutrinos and, in fact, the elastic scattering on electrons by the low energy component of the neutrino spectrum would be one of the main background sources for WIMP searches in liquid xenon detectors, as shown in Figure 21.Figure 21
Expected nuclear recoil spectrum from WIMP scatters in LXe for a spin-independent WIMP-nucleon cross-section of10-47cm2 (red solid) and 10-48 cm2 (red dashed) and a WIMP mass of 100 GeV/c2, along with the differential energy spectrum for pp (blue) and 7Be (cyan) neutrinos, and the electron recoil spectrum from the double beta decay of 136Xe (green). Assumptions are 99.5% discrimination of electronic recoils, 50% acceptance of nuclear recoils, and 80% flat analysis cuts acceptance. Taken from [185].DARWIN officially started in 2010; a technical design study should be ready in Spring 2013 and the start of the first physics run is expected by mid-2017.


#### 7.2.2. Multikiloton Scale Liquid Scintillators: Example LENA

The Borexino experiment demonstrated the great potential of the liquid-scintillator technique for the detection of low energy solar neutrinos. Thanks to this experience, a next-generation neutrino detector has been proposed: LENA (low energy neutrino astronomy) [186]. LENA is a multipurpose detector aiming to study supernova neutrinos, diffuse supernova neutrino background, proton decay, atmospheric neutrinos, long-baseline neutrino beams, geoneutrinos, and, last but not least, solar neutrinos. The LENA project foresees a cylindrical detector with a diameter of 30 m and a length of about 100 m. Inside the detector is foreseen an internal part (with a diameter of about 26 m) containing about 50 kilotons of liquid scintillator, separated from a nonscintillating buffer region by a nylon barrier. Outside, a tank (made in steel or concrete) separates the inner detector from an outer water tank; it is used both for shielding and as an active muon veto. To collect the scintillation light, about 45,000 photomultipliers (with a diameter of 20 cm) are mounted to the internal walls of the detector. To increase the optically active area, the photomultipliers tubes are equipped with conic mirrors, the corresponding surface coverage is about 30%. Figure 22 shows a schematic overview of the current LENA design.Figure 22
Schematical view of the LENA detector. From [186].Among the favored solvent for the liquid scintillator in LENA, the LAB (linear alkylbenzene) is currently the preferred one. It has a high light yield and large attenuation length and it has also the advantage of being a nonhazardous liquid. The attenuation lengths is on the order of 10 to 20 m (at a wavelength of 430 nm) and the photoelectron yield could be greater than 200 photoelectrons per MeV (with a scintillator mixture containing 2 g/L PPO and 20 mg/L bisMSB as wavelength shifters). Studies have been carried out to test the large-scale light transport and the differences in scintillator response forα, β, and γ particles. An alternative solvent option is the well-studied PXE [187] or a mixture of PXE and dodecane.As already pointed out, Borexino has splendidly demonstrated the potential of the detection technique with liquid scintillator based detectors for the solar neutrino detection. This technique offers the opportunity for a spectrally resolved measurement of the solar neutrino spectrum in the all energy range.Because the smaller ratio of surface to volume compared to the Borexino detector in LENA it is very likely to reach the excellent background conditions of Borexino (A smaller ratio of surface to volume decreases the chance that the scintillator is contaminated with radioimpurities.) Monte Carlo simulations of the gamma background due to the uranium, thorium, and potassium from the photomultipliers glass show that a fiducial volume of the order of 30 ktons is achievable for solar neutrino studies; LENA will be able to address topics both in neutrino oscillations and in solar physics thanks to its unprecedented statistics. A high statistics can be obtained in short times and in both Pyhsalmi and Frejus underground laboratories, where the detector could be hosted and where the cosmogenic background of11C will be significantly lower than in Borexino.Monte Carlo simulations show that forpep, CNO, and low-energy 8B-νs detection a fiducial mass of ~30 kton is necessary, while the fiducial mass for 7Be-νs and high-energy (E>5MeV) 8B-νs could be enlarged to 35 kton or more.In Table9 the expected rates in 30 kton for the neutrinos emitted in the pp chain and the CNO-bicycle are reported, using the most recent solar model predictions. This evaluation refers to a detection threshold set at about 250 keV.Table 9
Expected solar neutrino rates in LENA (channelνe→eν). The estimates are derived from the existing Borexino analyses [154, 188] as well as expectation values for the respective energy windows (EW) of observation [189–191]. The quoted fiducial masses, mfid, in LAB are based on a Monte Carlo simulation of the external γ-ray background in LENA. Table taken and adapted from [186].
Source
EW [MeV]
m
fid [kt]
Rate [cpd]
pp
>0.25
30
40
pep
0.8−1.4
30
2.8
×
10
2
7
Be
>0.25
35
1.0
×
10
4
8
B
>2.8
35
79
CNO
0.8–1.4
30
1.9
×
10
2


#### 7.2.3. New Techniques with Organic Scintillators: LENS

The main goal of the Low Energy Neutrino Spectroscopy (LENS) detector is the real-time measurement of solar neutrinos as a function of their energy, focusing, on particular, in the analysis of the lowest energy neutrinos coming from the proton-proton fusion (i.e., thepp neutrinos), which represent the main contribution and the less known component of the pp-chain of fusion reactions inside the Sun.In order to make an energy spectrum measurement on low energy neutrinos, it is necessary to reach a low threshold for the charged current (CC) process and to be able to discriminate the background from radioactive decays. The CC process employed in LENS is the neutrino induced transition of115In to an excited state of 115Sn:
(14)νe+In115→Sn115*+e-(E=Eν-114keV),Sn115*(τ=4.76μs)→Sn115+γ(498keV)+γ(116keV).Thanks to that it is possible to detect low energy neutrinos with a threshold of 114 keV and measure their energy, following an idea that has been investigated since the 1970s [192].The primary interaction and the secondary cascade enable a triple coincidence, correlated in space and time. LENS employs as detection medium a liquid scintillator chemically doped with natural indium (In115 = 95.7%). In order to exploit the spatial correlation, the volume of the detector is segmented into cubic cells (7.5 cm) by clear foils (Teflon FEP) that have a lower index of refraction than the liquid scintillator. By internal reflection, the scintillation light produced in a cell is channeled in the directions of the 6-cell faces. The collected channeled light is read out at the edge of the detector by photomultiplier tubes.LENS should be able to determine the low energy solar neutrino fluxes with an accuracy ≤4%, testing neutrino and solar physics with a global precision better than the present one and also looking for any inconsistency in the LMA conversion mechanism [193].


## 7.1. The Near Future: Improvement ofpep Measurements and CNO Detection

In the last decades, the intensive study of8B and, more recently, 7Be solar neutrinos made possible fundamental steps forward in the solution of the solar neutrino puzzle and the determination of the neutrino mixing parameters. Nevertheless, many key features of the oscillation models (like the transition between the vacuum dominated sub-MeV region and the spectral region between 1 and 3 MeV, where matter effects become relevant) still have to be tested or verified with better accuracy and precision (see Figure 18, taken from [174]).Figure 18
Theνe survival probability is represented as a function of neutrino energy. The gray band represent the MSW-LMA prediction. The higher survival probability region at low energies is where vacuum-dominated oscillations occur. As the neutrino energy increases, matter effects become important and the lower survival probability at high energies is due to matter-enhanced oscillations. The reported data correspond to solar neutrino flux measurements performed by different experiments. Taken from [174].The apparent partial deficit of events in the low energy part of the8B spectrum suggested the introduction of new theoretical models (as discussed in Section 6). Also for these reasons, the experimental efforts in the last years focused on the detection of neutrinos of ever decreasing energies, to fully confirm the validity of the MSW-LMA solution and verify the fluxes predicted by SSMs, discriminating between different versions of these models. The fluxes of the medium and high energy neutrinos of the pp chains (7Be, 8B, and hep) are predicted with quite large uncertainties, mainly due to the uncertainties in nuclear cross-sections and solar opacity (Table 5). The pp and pep fluxes, instead, are strongly correlated between themselves and their values are predicted with the highest precision because SSMs predict that pp chain reactions are responsible for more than 99% of the energy powering the Sun [80]. Therefore, the measurements of these components would be the most stringent test of the SSM. The tight correlation between pep and pp neutrinos is theoretically well established and, therefore, even in the pessimistic hypothesis that pp neutrinos could not be measured with the desired accuracy, a significant improvement in the pep neutrinos measurement with respect to data presently available would make it possible to reduce significantly the 15% indetermination on the solar luminosity (see Section 6.2) and to test indirectly the SSM’s predictions that almost 100% of solar energy is produced by nuclear burning.As already mentioned, water Čerenkov detectors, which played a fundamental role in the solution of the solar neutrino problem, are characterized by a low photon yield [175, 176] and therefore can detect only the higher part of the spectrum (hep and 8B neutrinos with a threshold around 3.5MeV). The radiochemical experiments [153, 177] are limited, instead, by their ability to measure only the integrated neutrino rate above the charge-current interaction threshold (down to 0.23MeV for the Gallium experiments), without the possibility to discriminate between the different spectrum components. Therefore, an important contribution should come from the present and future organic liquid scintillator detectors, planned to perform low energy solar neutrino spectroscopy. To reach this goal, they will take advantage from the high values of light yield (about 104 photons per MeV of deposited energy) and from the possibility to assemble very large masses of high purity materials. The excellent levels of radiopurity, reached, for instance, at Borexino, and the typical geometry of these detectors (which are unsegmented and can be easily adapted to the definition of a fiducial volume) are fundamental to reduce the impact of the background, that is so critical due to the feebleness of the low energy signal.In the near future, significant contributions are expected from Borexino and SNO+ [178] experiments (the main problem still surviving seems to be the reduction of 210Pb.) Borexino has already proved its importance in this kind of analysis performing the first measurements of pep and CNO neutrinos (even if the level accuracy is not yet the desired one) and further reducing, with the purification campaign started since July 2010, the level of contamination from almost all of the main radioactive background sources. The purification efforts are still ongoing and should make possible a further improvement on the accuracy of the signal extraction. Also, a novel technique [179] would allow to determine the 210Bi background. Preliminary calculations show that the CNO signal could be extracted from the 210Bi background with one year of data taking. The SNO+ experiment, that should start taking data soon in the SNOLAB, should take advantage from the location (about two times deeper underground than the Gran Sasso laboratory), with the consequent lower muon flux and a strongly reduced 11C rate. Moreover, thanks to the detector mass (about three times larger than in Borexino), it should be able to reach a higher counting rate. This could determine a fundamental improvement at least in the case of the pep neutrino measurement, where a 5% uncertainty is expected, to a level that should make possible a significant test of the MSW transition region.In the more optimistic scenarios, it may be also possible to attack the main problem of measuring the lowest energy parts of the solar neutrino spectrum, that is, thepp neutrinos and the 0.38MeV Berillium line. In any case, the presence in organic scintillators of an intrinsic 14C background will make this very low energy measurements an extremely hard task and they may require the introduction of new techniques, like the ones we are going to describe in the next subsections.


## 7.2. The Far Future: Experimental Challenges

The challenge for all future experiments aimed at measuring the low energy part of solar neutrino spectrum is that of assembling experimental devices with low energy thresholds suitable to detect a low rate signal in a region characterized by different potential sources of radioactive background. This difficult experimental task is common also to the experiments looking for neutrinoless doubleβ decay or for dark matter signals (search for signatures of WIMPs, a stable or long-lived weakly interacting elementary particle, produced in the early Universe, whose existence is predicted in extensions of the standard model). In fact, some of the solar neutrino experiments planned for the future are multipurpose experiments designed also for the other above-quoted topics.They are all characterized by a very large detector target mass and by the need to reach very high levels of radiopurity. The common feature is that of using scintillator detectors, but they differ for the chosen active scintillator material, which can vary from traditional organic scintillators (developed with the use of innovative technological devices) to new materials, like the noble gases.


### 7.2.1. Noble Liquid Detectors: CLEAN and XMASS

One of the possible future frontiers is the idea to use scintillation detectors with liquid noble gases, like xenon, argon, and neon. These materials have the advantage of being relatively inexpensive, easy to obtain, and dense and it is not too difficult to build large homogeneous detectors of this kind; moreover, they can be quite easily purified, offer very high scintillation yields (about 30–40 photons/keV), and do not absorb their own scintillation light.A first example is offered by the CLEAN/DEAP family, a series of detectors based entirely on scintillation in liquid neon (LNe) and liquid argon (LAr). They have been realized using a scaleable technology in order to reach increasing sensitivities in the different prototypes realized and installed in the SNOLAB (Pico-CLEAN, Micro-CLEAN, DEAP-I, Mini-CLEAN and CLEAN/DEAP) with the aim to search for dark matter and to perform (through the analysis of elastic neutrino-electron and neutrino-nucleus scattering) a real-time measurement of thepp solar neutrino flux. The final detector CLEAN (cryogenic low energy astrophysics with noble gases) [180] (see Figure 19) will be made by a stainless steel tank, of about 6 meters of diameter, filled with 135 metric tons of cryogenic liquid neon; only the central part of it, surrounded isotropically by a series of photomultipliers, will constitute the detector fiducial volume. An external tank of water, 10 metres wide and 12 metres high, will act as γ-ray shielding, neutron shielding, and muon veto. According to Monte Carlo simulations, there should be a production of 15000 photons/MeV and it should be possible to reach a 100% photon wavelength shifter efficiency and a statistical uncertainty on the pp measurements of the order of 1%.Figure 19
Scheme of the CLEAN detector. Taken from [180].A precise measurement of thepp component and of the ratio between pp and 7Be fluxes would be essential to test the predictions of SSMs. A high accuracy on the pp neutrino flux would also make possible a better determination of the θ12 mixing angle, which, complemented with the results from previous solar neutrino experiments and from KamLAND (essential for the Δm122 measurement), would be fundamental to test the consistency of the LMA solution also in the region of transition between vacuum dominated and matter enhanced oscillations. Finally, CLEAN could in principle try to measure also the CNO neutrino flux, through the analysis of neutrino spectrum from 0.7 to 1.0 MeV, with an estimated accuracy between 10% and 15%.An interesting alternative to the use of neon is offered by liquid xenon scintillator detectors [181], which take advantage of the fact that among liquid rare gases xenon has the highest stopping power for penetrating radiation (thanks to its high atomic number, A≃131, and density, ρ=3g/cm3) and also the highest ionization and scintillation yield. The technological improvements of the last twenty to thirty years made possible significant improvements in the cooling and purification techniques of this kind of detectors and in the possibility of assembling large mass detectors, of the order of some tons (like in the case of MEG [182] experiment, studying the μ→eγ decay).The XMASS experiment (see Figure20) is a multipurpose low background and low energy threshold experiment that will use a large massive liquid xenon detector and has been designed to look for WIMPs (dark matter candidates), search for neutrinoless double β decay, and study the pp and the 7Be solar neutrinos. After two preliminary phases, during which smaller prototypes have been realized and installed in the Kamioka mine [183], and the first data on double beta decay and dark matter have been taken, the full XMASS detector (that will measure also solar neutrinos) will have a total mass of 20 metric tons,with a fiducial volume of 10 metric tons. Special efforts are required mainly to lower the background, by reducing the radioactive contamination in the parts used for detector construction (with special attention to the photomultipliers and the copper material used for PMT holder), constructing a larger pure water active shield (for muons and mainly neutrons and γ rays), and, above all, developing a distillation system for xenon in order to reduce the contamination by 85Kr, the major source of radioactive background inside the detector.Schematic view of the full XMASS facility (a) and details of the inner detector (b) from which one can see the particular configuration of the hexagonal photomultiplier tubes. Taken from [183, 184].
(a)
(b)Another interesting experimental project based on the noble gases liquid scintillator technique is that of DARWIN (dark matter wimp search with noble liquids) [185], which brings together different European and US research groups working on existing experiments and on the study for a future multiton scale LAr and LXe dark matter search facility in Europe. The main goal of the experiment is to look for a WIMP signal and to demonstrate its dark matter nature, taking advantage from the fact of performing the measurement with multiple different targets operating under similar conditions. In this way, it should be possible to estimate the dependence of the rate with the target material and, therefore, to better determine the WIMP candidate mass and to distinguish between spin independent and spin dependent couplings. The energy region of the nuclear recoil spectrum, below 200 keV, that should be investigated by this future experiment is of particular interest also for the study of the pp solar neutrinos and, in fact, the elastic scattering on electrons by the low energy component of the neutrino spectrum would be one of the main background sources for WIMP searches in liquid xenon detectors, as shown in Figure 21.Figure 21
Expected nuclear recoil spectrum from WIMP scatters in LXe for a spin-independent WIMP-nucleon cross-section of10-47cm2 (red solid) and 10-48 cm2 (red dashed) and a WIMP mass of 100 GeV/c2, along with the differential energy spectrum for pp (blue) and 7Be (cyan) neutrinos, and the electron recoil spectrum from the double beta decay of 136Xe (green). Assumptions are 99.5% discrimination of electronic recoils, 50% acceptance of nuclear recoils, and 80% flat analysis cuts acceptance. Taken from [185].DARWIN officially started in 2010; a technical design study should be ready in Spring 2013 and the start of the first physics run is expected by mid-2017.


### 7.2.2. Multikiloton Scale Liquid Scintillators: Example LENA

The Borexino experiment demonstrated the great potential of the liquid-scintillator technique for the detection of low energy solar neutrinos. Thanks to this experience, a next-generation neutrino detector has been proposed: LENA (low energy neutrino astronomy) [186]. LENA is a multipurpose detector aiming to study supernova neutrinos, diffuse supernova neutrino background, proton decay, atmospheric neutrinos, long-baseline neutrino beams, geoneutrinos, and, last but not least, solar neutrinos. The LENA project foresees a cylindrical detector with a diameter of 30 m and a length of about 100 m. Inside the detector is foreseen an internal part (with a diameter of about 26 m) containing about 50 kilotons of liquid scintillator, separated from a nonscintillating buffer region by a nylon barrier. Outside, a tank (made in steel or concrete) separates the inner detector from an outer water tank; it is used both for shielding and as an active muon veto. To collect the scintillation light, about 45,000 photomultipliers (with a diameter of 20 cm) are mounted to the internal walls of the detector. To increase the optically active area, the photomultipliers tubes are equipped with conic mirrors, the corresponding surface coverage is about 30%. Figure 22 shows a schematic overview of the current LENA design.Figure 22
Schematical view of the LENA detector. From [186].Among the favored solvent for the liquid scintillator in LENA, the LAB (linear alkylbenzene) is currently the preferred one. It has a high light yield and large attenuation length and it has also the advantage of being a nonhazardous liquid. The attenuation lengths is on the order of 10 to 20 m (at a wavelength of 430 nm) and the photoelectron yield could be greater than 200 photoelectrons per MeV (with a scintillator mixture containing 2 g/L PPO and 20 mg/L bisMSB as wavelength shifters). Studies have been carried out to test the large-scale light transport and the differences in scintillator response forα, β, and γ particles. An alternative solvent option is the well-studied PXE [187] or a mixture of PXE and dodecane.As already pointed out, Borexino has splendidly demonstrated the potential of the detection technique with liquid scintillator based detectors for the solar neutrino detection. This technique offers the opportunity for a spectrally resolved measurement of the solar neutrino spectrum in the all energy range.Because the smaller ratio of surface to volume compared to the Borexino detector in LENA it is very likely to reach the excellent background conditions of Borexino (A smaller ratio of surface to volume decreases the chance that the scintillator is contaminated with radioimpurities.) Monte Carlo simulations of the gamma background due to the uranium, thorium, and potassium from the photomultipliers glass show that a fiducial volume of the order of 30 ktons is achievable for solar neutrino studies; LENA will be able to address topics both in neutrino oscillations and in solar physics thanks to its unprecedented statistics. A high statistics can be obtained in short times and in both Pyhsalmi and Frejus underground laboratories, where the detector could be hosted and where the cosmogenic background of11C will be significantly lower than in Borexino.Monte Carlo simulations show that forpep, CNO, and low-energy 8B-νs detection a fiducial mass of ~30 kton is necessary, while the fiducial mass for 7Be-νs and high-energy (E>5MeV) 8B-νs could be enlarged to 35 kton or more.In Table9 the expected rates in 30 kton for the neutrinos emitted in the pp chain and the CNO-bicycle are reported, using the most recent solar model predictions. This evaluation refers to a detection threshold set at about 250 keV.Table 9
Expected solar neutrino rates in LENA (channelνe→eν). The estimates are derived from the existing Borexino analyses [154, 188] as well as expectation values for the respective energy windows (EW) of observation [189–191]. The quoted fiducial masses, mfid, in LAB are based on a Monte Carlo simulation of the external γ-ray background in LENA. Table taken and adapted from [186].
Source
EW [MeV]
m
fid [kt]
Rate [cpd]
pp
>0.25
30
40
pep
0.8−1.4
30
2.8
×
10
2
7
Be
>0.25
35
1.0
×
10
4
8
B
>2.8
35
79
CNO
0.8–1.4
30
1.9
×
10
2


### 7.2.3. New Techniques with Organic Scintillators: LENS

The main goal of the Low Energy Neutrino Spectroscopy (LENS) detector is the real-time measurement of solar neutrinos as a function of their energy, focusing, on particular, in the analysis of the lowest energy neutrinos coming from the proton-proton fusion (i.e., thepp neutrinos), which represent the main contribution and the less known component of the pp-chain of fusion reactions inside the Sun.In order to make an energy spectrum measurement on low energy neutrinos, it is necessary to reach a low threshold for the charged current (CC) process and to be able to discriminate the background from radioactive decays. The CC process employed in LENS is the neutrino induced transition of115In to an excited state of 115Sn:
(14)νe+In115→Sn115*+e-(E=Eν-114keV),Sn115*(τ=4.76μs)→Sn115+γ(498keV)+γ(116keV).Thanks to that it is possible to detect low energy neutrinos with a threshold of 114 keV and measure their energy, following an idea that has been investigated since the 1970s [192].The primary interaction and the secondary cascade enable a triple coincidence, correlated in space and time. LENS employs as detection medium a liquid scintillator chemically doped with natural indium (In115 = 95.7%). In order to exploit the spatial correlation, the volume of the detector is segmented into cubic cells (7.5 cm) by clear foils (Teflon FEP) that have a lower index of refraction than the liquid scintillator. By internal reflection, the scintillation light produced in a cell is channeled in the directions of the 6-cell faces. The collected channeled light is read out at the edge of the detector by photomultiplier tubes.LENS should be able to determine the low energy solar neutrino fluxes with an accuracy ≤4%, testing neutrino and solar physics with a global precision better than the present one and also looking for any inconsistency in the LMA conversion mechanism [193].


## 7.2.1. Noble Liquid Detectors: CLEAN and XMASS

One of the possible future frontiers is the idea to use scintillation detectors with liquid noble gases, like xenon, argon, and neon. These materials have the advantage of being relatively inexpensive, easy to obtain, and dense and it is not too difficult to build large homogeneous detectors of this kind; moreover, they can be quite easily purified, offer very high scintillation yields (about 30–40 photons/keV), and do not absorb their own scintillation light.A first example is offered by the CLEAN/DEAP family, a series of detectors based entirely on scintillation in liquid neon (LNe) and liquid argon (LAr). They have been realized using a scaleable technology in order to reach increasing sensitivities in the different prototypes realized and installed in the SNOLAB (Pico-CLEAN, Micro-CLEAN, DEAP-I, Mini-CLEAN and CLEAN/DEAP) with the aim to search for dark matter and to perform (through the analysis of elastic neutrino-electron and neutrino-nucleus scattering) a real-time measurement of thepp solar neutrino flux. The final detector CLEAN (cryogenic low energy astrophysics with noble gases) [180] (see Figure 19) will be made by a stainless steel tank, of about 6 meters of diameter, filled with 135 metric tons of cryogenic liquid neon; only the central part of it, surrounded isotropically by a series of photomultipliers, will constitute the detector fiducial volume. An external tank of water, 10 metres wide and 12 metres high, will act as γ-ray shielding, neutron shielding, and muon veto. According to Monte Carlo simulations, there should be a production of 15000 photons/MeV and it should be possible to reach a 100% photon wavelength shifter efficiency and a statistical uncertainty on the pp measurements of the order of 1%.Figure 19
Scheme of the CLEAN detector. Taken from [180].A precise measurement of thepp component and of the ratio between pp and 7Be fluxes would be essential to test the predictions of SSMs. A high accuracy on the pp neutrino flux would also make possible a better determination of the θ12 mixing angle, which, complemented with the results from previous solar neutrino experiments and from KamLAND (essential for the Δm122 measurement), would be fundamental to test the consistency of the LMA solution also in the region of transition between vacuum dominated and matter enhanced oscillations. Finally, CLEAN could in principle try to measure also the CNO neutrino flux, through the analysis of neutrino spectrum from 0.7 to 1.0 MeV, with an estimated accuracy between 10% and 15%.An interesting alternative to the use of neon is offered by liquid xenon scintillator detectors [181], which take advantage of the fact that among liquid rare gases xenon has the highest stopping power for penetrating radiation (thanks to its high atomic number, A≃131, and density, ρ=3g/cm3) and also the highest ionization and scintillation yield. The technological improvements of the last twenty to thirty years made possible significant improvements in the cooling and purification techniques of this kind of detectors and in the possibility of assembling large mass detectors, of the order of some tons (like in the case of MEG [182] experiment, studying the μ→eγ decay).The XMASS experiment (see Figure20) is a multipurpose low background and low energy threshold experiment that will use a large massive liquid xenon detector and has been designed to look for WIMPs (dark matter candidates), search for neutrinoless double β decay, and study the pp and the 7Be solar neutrinos. After two preliminary phases, during which smaller prototypes have been realized and installed in the Kamioka mine [183], and the first data on double beta decay and dark matter have been taken, the full XMASS detector (that will measure also solar neutrinos) will have a total mass of 20 metric tons,with a fiducial volume of 10 metric tons. Special efforts are required mainly to lower the background, by reducing the radioactive contamination in the parts used for detector construction (with special attention to the photomultipliers and the copper material used for PMT holder), constructing a larger pure water active shield (for muons and mainly neutrons and γ rays), and, above all, developing a distillation system for xenon in order to reduce the contamination by 85Kr, the major source of radioactive background inside the detector.Schematic view of the full XMASS facility (a) and details of the inner detector (b) from which one can see the particular configuration of the hexagonal photomultiplier tubes. Taken from [183, 184].
(a)
(b)Another interesting experimental project based on the noble gases liquid scintillator technique is that of DARWIN (dark matter wimp search with noble liquids) [185], which brings together different European and US research groups working on existing experiments and on the study for a future multiton scale LAr and LXe dark matter search facility in Europe. The main goal of the experiment is to look for a WIMP signal and to demonstrate its dark matter nature, taking advantage from the fact of performing the measurement with multiple different targets operating under similar conditions. In this way, it should be possible to estimate the dependence of the rate with the target material and, therefore, to better determine the WIMP candidate mass and to distinguish between spin independent and spin dependent couplings. The energy region of the nuclear recoil spectrum, below 200 keV, that should be investigated by this future experiment is of particular interest also for the study of the pp solar neutrinos and, in fact, the elastic scattering on electrons by the low energy component of the neutrino spectrum would be one of the main background sources for WIMP searches in liquid xenon detectors, as shown in Figure 21.Figure 21
Expected nuclear recoil spectrum from WIMP scatters in LXe for a spin-independent WIMP-nucleon cross-section of10-47cm2 (red solid) and 10-48 cm2 (red dashed) and a WIMP mass of 100 GeV/c2, along with the differential energy spectrum for pp (blue) and 7Be (cyan) neutrinos, and the electron recoil spectrum from the double beta decay of 136Xe (green). Assumptions are 99.5% discrimination of electronic recoils, 50% acceptance of nuclear recoils, and 80% flat analysis cuts acceptance. Taken from [185].DARWIN officially started in 2010; a technical design study should be ready in Spring 2013 and the start of the first physics run is expected by mid-2017.


## 7.2.2. Multikiloton Scale Liquid Scintillators: Example LENA

The Borexino experiment demonstrated the great potential of the liquid-scintillator technique for the detection of low energy solar neutrinos. Thanks to this experience, a next-generation neutrino detector has been proposed: LENA (low energy neutrino astronomy) [186]. LENA is a multipurpose detector aiming to study supernova neutrinos, diffuse supernova neutrino background, proton decay, atmospheric neutrinos, long-baseline neutrino beams, geoneutrinos, and, last but not least, solar neutrinos. The LENA project foresees a cylindrical detector with a diameter of 30 m and a length of about 100 m. Inside the detector is foreseen an internal part (with a diameter of about 26 m) containing about 50 kilotons of liquid scintillator, separated from a nonscintillating buffer region by a nylon barrier. Outside, a tank (made in steel or concrete) separates the inner detector from an outer water tank; it is used both for shielding and as an active muon veto. To collect the scintillation light, about 45,000 photomultipliers (with a diameter of 20 cm) are mounted to the internal walls of the detector. To increase the optically active area, the photomultipliers tubes are equipped with conic mirrors, the corresponding surface coverage is about 30%. Figure 22 shows a schematic overview of the current LENA design.Figure 22
Schematical view of the LENA detector. From [186].Among the favored solvent for the liquid scintillator in LENA, the LAB (linear alkylbenzene) is currently the preferred one. It has a high light yield and large attenuation length and it has also the advantage of being a nonhazardous liquid. The attenuation lengths is on the order of 10 to 20 m (at a wavelength of 430 nm) and the photoelectron yield could be greater than 200 photoelectrons per MeV (with a scintillator mixture containing 2 g/L PPO and 20 mg/L bisMSB as wavelength shifters). Studies have been carried out to test the large-scale light transport and the differences in scintillator response forα, β, and γ particles. An alternative solvent option is the well-studied PXE [187] or a mixture of PXE and dodecane.As already pointed out, Borexino has splendidly demonstrated the potential of the detection technique with liquid scintillator based detectors for the solar neutrino detection. This technique offers the opportunity for a spectrally resolved measurement of the solar neutrino spectrum in the all energy range.Because the smaller ratio of surface to volume compared to the Borexino detector in LENA it is very likely to reach the excellent background conditions of Borexino (A smaller ratio of surface to volume decreases the chance that the scintillator is contaminated with radioimpurities.) Monte Carlo simulations of the gamma background due to the uranium, thorium, and potassium from the photomultipliers glass show that a fiducial volume of the order of 30 ktons is achievable for solar neutrino studies; LENA will be able to address topics both in neutrino oscillations and in solar physics thanks to its unprecedented statistics. A high statistics can be obtained in short times and in both Pyhsalmi and Frejus underground laboratories, where the detector could be hosted and where the cosmogenic background of11C will be significantly lower than in Borexino.Monte Carlo simulations show that forpep, CNO, and low-energy 8B-νs detection a fiducial mass of ~30 kton is necessary, while the fiducial mass for 7Be-νs and high-energy (E>5MeV) 8B-νs could be enlarged to 35 kton or more.In Table9 the expected rates in 30 kton for the neutrinos emitted in the pp chain and the CNO-bicycle are reported, using the most recent solar model predictions. This evaluation refers to a detection threshold set at about 250 keV.Table 9
Expected solar neutrino rates in LENA (channelνe→eν). The estimates are derived from the existing Borexino analyses [154, 188] as well as expectation values for the respective energy windows (EW) of observation [189–191]. The quoted fiducial masses, mfid, in LAB are based on a Monte Carlo simulation of the external γ-ray background in LENA. Table taken and adapted from [186].
Source
EW [MeV]
m
fid [kt]
Rate [cpd]
pp
>0.25
30
40
pep
0.8−1.4
30
2.8
×
10
2
7
Be
>0.25
35
1.0
×
10
4
8
B
>2.8
35
79
CNO
0.8–1.4
30
1.9
×
10
2


## 7.2.3. New Techniques with Organic Scintillators: LENS

The main goal of the Low Energy Neutrino Spectroscopy (LENS) detector is the real-time measurement of solar neutrinos as a function of their energy, focusing, on particular, in the analysis of the lowest energy neutrinos coming from the proton-proton fusion (i.e., thepp neutrinos), which represent the main contribution and the less known component of the pp-chain of fusion reactions inside the Sun.In order to make an energy spectrum measurement on low energy neutrinos, it is necessary to reach a low threshold for the charged current (CC) process and to be able to discriminate the background from radioactive decays. The CC process employed in LENS is the neutrino induced transition of115In to an excited state of 115Sn:
(14)νe+In115→Sn115*+e-(E=Eν-114keV),Sn115*(τ=4.76μs)→Sn115+γ(498keV)+γ(116keV).Thanks to that it is possible to detect low energy neutrinos with a threshold of 114 keV and measure their energy, following an idea that has been investigated since the 1970s [192].The primary interaction and the secondary cascade enable a triple coincidence, correlated in space and time. LENS employs as detection medium a liquid scintillator chemically doped with natural indium (In115 = 95.7%). In order to exploit the spatial correlation, the volume of the detector is segmented into cubic cells (7.5 cm) by clear foils (Teflon FEP) that have a lower index of refraction than the liquid scintillator. By internal reflection, the scintillation light produced in a cell is channeled in the directions of the 6-cell faces. The collected channeled light is read out at the edge of the detector by photomultiplier tubes.LENS should be able to determine the low energy solar neutrino fluxes with an accuracy ≤4%, testing neutrino and solar physics with a global precision better than the present one and also looking for any inconsistency in the LMA conversion mechanism [193].


## 8. Remarks on the Present Status and Future Outlooks

In this paper we went through the main results obtained in the study of solar neutrinos and we focused our attention mainly on the last decade advancements. Since the discovery of neutrino oscillations and the solution to the long standing solar neutrino problem at the dawn of the century, solar neutrino physics has evolved quickly and has become a mature field. It took advantage from the great amount of data of the different working phases of experiments like Super-Kamiokande and SNO, corroborated by the analogous studies of the reactor experiment KamLAND and recently sustained also by the first “low energy” real-time measurements performed by Borexino.A coherent picture emerges from all of these experimental achievements and from the global analyses performed by the single experimental collaborations and in other parallel theoretical and phenomenological studies and we can say that the basic properties and the values of the parameters driving solar neutrino oscillations,Δm122, and θ12 are now known with quite a satisfactory accuracy (Tables 7 and 8) and the validity of the MSW-LMA solution is well established (Figure 18). Nevertheless, there are still important aspects of the oscillation mechanism on which we would like to shed more light. In particular the vacuum to matter transition regime requires further study (see also Section 9).Important parallel advancements took place in the study of neutrino oscillations during the very last years; in particular a series of reactor short baseline experiments have confidently established that the mixing angleθ13 is different from zero, opening interesting opportunities for future experiments looking for leptonic CP violation (the details have been given in Section 6).From an astrophysical point of view, current solar neutrino data have put us on the verge of fulfilling the original dream of Davies and Bahcall and use solar neutrinos as a probe of the nuclear fusion processes that power the Sun and the vast majority of stars. The four relevant neutrino fluxes produced in the differentpp-chains are, thanks to the latest efforts from Borexino, now very well constrained from experimental data (7Be has the largest uncertainty, 4.5%, if the solar luminosity constraint is used in the analysis of the data). Standard solar model predictions are in excellent agreement with solar fluxes, regardless of the solar composition assumed in the construction of the model. In fact, the agreement is so good for both high-Z and low-Z solar models (Table 4) that it is very unlikely that neutrino fluxes from pp-chains will be able to discriminate between solar compositions. Borexino has also recently established the most stringent upper limit on CNO fluxes which is now only a factor of 1.5 larger than solar model predictions. CNO fluxes carry a wealth of information about the solar core and are, for solar physics, the most coveted prize. The latest developments, both experimentally and in background subtraction techniques, place Borexino at the doors of this momentous measurement. In this regard, potentiality of SNO+ is unmatched, but at present the primary solar neutrino measurements are planned to take place after the double beta decay measurements are carried out for at least 4 years. Some of the possibilities that a measurement of CNO fluxes would offer are discussed in the next section, together with some of the main questions which are still open.


## 9. Open Questions in Solar Neutrino Physics

### 9.1. The Metallicity Problem

The solar abundance or solar metallicity problem has been around for some time now. In analogy with the solar neutrino problem, there have been attempts (although in most cases, it is fair to say, of somewhat less radical nature) to solve it by introducing modifications to the input physics of SSMs. To mention a few of them, we could remember the following:(i)
large enhancement of Ne abundance [194, 195] is important because of its contribution uncertainty and a weak bond in solar abundances because its abundance is determined rather indirectly [44];(ii)
increased element diffusion rates [67, 196];(iii)
accretion of metal-poor materials leading to a “two-zone” solar model in terms of composition [64, 196, 197].Also solar models including some sort of prescriptions to account for rotation and other dynamical effects have been put forward; however, their performance is quite poor.So far, all attempts of finding a solution to all the manifestations of the solar abundance problem have failed. In some cases,YS can be brought into agreement with helioseismology, in other cases RCZ and the sound speed profile, but a simultaneous solution to all the problems has not yet been found.The exceptions are the two obvious ones: (a) thelow-Z solar abundances actually underestimate the true metal content of the Sun; (b) an increase of radiative opacities by the right amount (15% to 20% at the base of the convective zone down to about 3% in the solar core) to compensate for the decrease induced by the low-Z abundances. The drawback to this idea is that current state-of-the-art radiative opacity calculations differ by only 2 to 3% at the base of the convective envelope, much lower from what would be required by low-Z models.It has indeed been shown that by increasing the radiative opacity in low-Z SSMs the agreement with helioseismology can be restored to match results from high-Z SSMs [198]. Additionally, the 7Be and 8B fluxes of a low-Z SSMs with increased opacity coincide with those from a high-Z model [199]. As good as this may seem, it shows the intrinsic degeneracy between composition and opacities.Recently, a novel approach, the linear solar models (LSM), that relate changes in solar observables to modifications in the input physics by the calculation of kernels based on SSMs has been developed by [200] (We remark that LSMs offer an efficient way of studying the response of the solar structure to changes in any of the physical ingredients entering solar model calculations that does not require the construction of solar models with the varied physics.) LSMs have been applied in particular to the solar abundance problem and the changes required in the radiative opacity to restore the agreement between low-Z models and helioseismology [201] quantitatively, result similar to those quoted above.By using8B and now 7Be as thermometers of the solar core [79], CNO neutrinos represent a unique way to break this degeneracy and provide an independent determination of the CNO abundances, particularly the C + N abundance in the solar core. Keeping in mind the antagonism between solar interior and solar atmosphere models that the solar abundance problem has established, results from CNO fluxes will be of the outmost relevance for solar, and by extension stellar, physics.


### 9.2. The Vacuum to Matter Transition?

Solar neutrino experiments already measured the two-extreme-flavor conversion regimes, the vacuum term domination and matter term domination. There is no direct experimental evidence of the transition from one to the other. In fact, the lower energetic8B neutrinos are sensitive to the rise of the spectrum from matter combination towards vacuum, but the data (still very uncertain) seem not to show it. More data coming from Super-Kamiokande, Borexino, and SNO+ experiments will further explore the conversion in this regime.The precise measurement of low energy neutrinos like pep, exploiting the fact that are more energetic than7Be neutrinos, will also help to see small solar matter effects in the flavor conversion. This matter effects will be more precisely determined by the comparison of pep and pp neutrino measurements. In fact, the low energy neutrinos that are better suited to test matter effects are the CNO neutrinos. While the CNO neutrinos energy is around the pep neutrinos energy, the former are produced at higher temperatures and therefore at higher densities. The larger matter density where neutrinos are produced leads to larger matter effects for CNO neutrinos than for pep neutrinos. In fact, matter effects produce a significant spectral tilt of CNO neutrinos (~10%), which might be a good handle to separate the signal for background.The determination of the vacuum to matter transition has a significant impact on the determination of the solar mass splitting derived by solar data, which adds to the implications of Earth-matter effects measured by comparing the neutrino fluxes during the day and night. The good match of the independently determined solar mass splitting by solar neutrino experiments and by reactor experiments leads to the best test on nonstandard neutrino physics to solar neutrinos. There are many possibilities but the two scenarios more studied are the addition of new neutral current interactions [168, 202] which modify the amplitude of matter effects and therefore shift the effective mass splitting and the existence of a sterile neutrino which adds a new state with the appropriate mass splitting [169] to produce deviations of the flavor conversion in the 1–3 MeV range.


### 9.3. What Else Can We Learn from CNO Fluxes?

The most fundamental information the CNO fluxes carry is the most obvious one: that the CNO-bicycle operates in stars and it is a viable process for hydrogen fusion. It must not be forgotten that neutrinos are the only direct evidence of nuclear reactions being the source of energy in solar (stellar) interiors. For the Sun, models predict a marginal contribution to the total energy budget from CNO reactions, 0.8% and 0.4% forhigh-Z and low-Z solar models. However, CNO becomes the dominant mode for hydrogen burning in stars with masses right above the solar value. Detection of CNO neutrinos will provide direct evidence that CNO reactions actually take place in nature, as originally envisioned by Bethe [203]; it has been a long wait.The second important aspect of CNO neutrinos is the information they provide about the abundance of metals in the solar core. Knowing the abundance of CNO elements in the solar core is important by itself. In particular, a “perfect” measurement of the combinedN13+O15 flux translates into a determination of the solar C + N abundance with ~10% uncertainty [79], and the dominant sources of uncertainties are experimental and can be potentially reduced. Assuming we know the solar surface abundance of the same elements, that is, let us forget for the time being about the solar abundance problem, we can then put constraints on mixing mechanisms that may have created composition gradients during the evolution of the Sun. SSMs predict that the number density of C + N is enhanced in the solar core, at present day, by ~16% with respect to the surface due to the effects of the microscopic diffusion. And, although helioseismology shows that models with diffusion work much better than models without, there is no direct evidence of how efficient diffusion is. In fact, there have been suggestions that the standard prescription [204] may be too efficient in the Sun [205] and that diffusion rates should be lowered by ~15%. Solar CNO neutrinos could provide a test for the efficiency of the diffusion.There are other possibilities that might create a contrast between the solar core and surface composition. Recently, it has been shown that the Sun has a peculiar composition when compared to “solar twins,” that is, stars almost identical to the Sun in their surface properties [206, 207]. The authors found that the Sun is enhanced in volatile elements with respect to the solar twins that show no sign of harbouring planets by about 20%. In fact, they have associated this fact to the presence of rocky planets in the solar system, where refractory elements are locked, and the occurrence of an accretion episode of volatile-enriched material [207] after rocky cores is formed in the protoplanetary disk. If this was true, then the Sun would have an envelope that is richer in CNO than its interior. If a measurement of the N13+O15 flux would yield as a result a core composition where the abundance of C + N would be comparable or less than the surface value, then we would have an extremely exciting piece of evidence about the earlier phases of planet formation in the solar system [79].


## 9.1. The Metallicity Problem

The solar abundance or solar metallicity problem has been around for some time now. In analogy with the solar neutrino problem, there have been attempts (although in most cases, it is fair to say, of somewhat less radical nature) to solve it by introducing modifications to the input physics of SSMs. To mention a few of them, we could remember the following:(i)
large enhancement of Ne abundance [194, 195] is important because of its contribution uncertainty and a weak bond in solar abundances because its abundance is determined rather indirectly [44];(ii)
increased element diffusion rates [67, 196];(iii)
accretion of metal-poor materials leading to a “two-zone” solar model in terms of composition [64, 196, 197].Also solar models including some sort of prescriptions to account for rotation and other dynamical effects have been put forward; however, their performance is quite poor.So far, all attempts of finding a solution to all the manifestations of the solar abundance problem have failed. In some cases,YS can be brought into agreement with helioseismology, in other cases RCZ and the sound speed profile, but a simultaneous solution to all the problems has not yet been found.The exceptions are the two obvious ones: (a) thelow-Z solar abundances actually underestimate the true metal content of the Sun; (b) an increase of radiative opacities by the right amount (15% to 20% at the base of the convective zone down to about 3% in the solar core) to compensate for the decrease induced by the low-Z abundances. The drawback to this idea is that current state-of-the-art radiative opacity calculations differ by only 2 to 3% at the base of the convective envelope, much lower from what would be required by low-Z models.It has indeed been shown that by increasing the radiative opacity in low-Z SSMs the agreement with helioseismology can be restored to match results from high-Z SSMs [198]. Additionally, the 7Be and 8B fluxes of a low-Z SSMs with increased opacity coincide with those from a high-Z model [199]. As good as this may seem, it shows the intrinsic degeneracy between composition and opacities.Recently, a novel approach, the linear solar models (LSM), that relate changes in solar observables to modifications in the input physics by the calculation of kernels based on SSMs has been developed by [200] (We remark that LSMs offer an efficient way of studying the response of the solar structure to changes in any of the physical ingredients entering solar model calculations that does not require the construction of solar models with the varied physics.) LSMs have been applied in particular to the solar abundance problem and the changes required in the radiative opacity to restore the agreement between low-Z models and helioseismology [201] quantitatively, result similar to those quoted above.By using8B and now 7Be as thermometers of the solar core [79], CNO neutrinos represent a unique way to break this degeneracy and provide an independent determination of the CNO abundances, particularly the C + N abundance in the solar core. Keeping in mind the antagonism between solar interior and solar atmosphere models that the solar abundance problem has established, results from CNO fluxes will be of the outmost relevance for solar, and by extension stellar, physics.


## 9.2. The Vacuum to Matter Transition?

Solar neutrino experiments already measured the two-extreme-flavor conversion regimes, the vacuum term domination and matter term domination. There is no direct experimental evidence of the transition from one to the other. In fact, the lower energetic8B neutrinos are sensitive to the rise of the spectrum from matter combination towards vacuum, but the data (still very uncertain) seem not to show it. More data coming from Super-Kamiokande, Borexino, and SNO+ experiments will further explore the conversion in this regime.The precise measurement of low energy neutrinos like pep, exploiting the fact that are more energetic than7Be neutrinos, will also help to see small solar matter effects in the flavor conversion. This matter effects will be more precisely determined by the comparison of pep and pp neutrino measurements. In fact, the low energy neutrinos that are better suited to test matter effects are the CNO neutrinos. While the CNO neutrinos energy is around the pep neutrinos energy, the former are produced at higher temperatures and therefore at higher densities. The larger matter density where neutrinos are produced leads to larger matter effects for CNO neutrinos than for pep neutrinos. In fact, matter effects produce a significant spectral tilt of CNO neutrinos (~10%), which might be a good handle to separate the signal for background.The determination of the vacuum to matter transition has a significant impact on the determination of the solar mass splitting derived by solar data, which adds to the implications of Earth-matter effects measured by comparing the neutrino fluxes during the day and night. The good match of the independently determined solar mass splitting by solar neutrino experiments and by reactor experiments leads to the best test on nonstandard neutrino physics to solar neutrinos. There are many possibilities but the two scenarios more studied are the addition of new neutral current interactions [168, 202] which modify the amplitude of matter effects and therefore shift the effective mass splitting and the existence of a sterile neutrino which adds a new state with the appropriate mass splitting [169] to produce deviations of the flavor conversion in the 1–3 MeV range.


## 9.3. What Else Can We Learn from CNO Fluxes?

The most fundamental information the CNO fluxes carry is the most obvious one: that the CNO-bicycle operates in stars and it is a viable process for hydrogen fusion. It must not be forgotten that neutrinos are the only direct evidence of nuclear reactions being the source of energy in solar (stellar) interiors. For the Sun, models predict a marginal contribution to the total energy budget from CNO reactions, 0.8% and 0.4% forhigh-Z and low-Z solar models. However, CNO becomes the dominant mode for hydrogen burning in stars with masses right above the solar value. Detection of CNO neutrinos will provide direct evidence that CNO reactions actually take place in nature, as originally envisioned by Bethe [203]; it has been a long wait.The second important aspect of CNO neutrinos is the information they provide about the abundance of metals in the solar core. Knowing the abundance of CNO elements in the solar core is important by itself. In particular, a “perfect” measurement of the combinedN13+O15 flux translates into a determination of the solar C + N abundance with ~10% uncertainty [79], and the dominant sources of uncertainties are experimental and can be potentially reduced. Assuming we know the solar surface abundance of the same elements, that is, let us forget for the time being about the solar abundance problem, we can then put constraints on mixing mechanisms that may have created composition gradients during the evolution of the Sun. SSMs predict that the number density of C + N is enhanced in the solar core, at present day, by ~16% with respect to the surface due to the effects of the microscopic diffusion. And, although helioseismology shows that models with diffusion work much better than models without, there is no direct evidence of how efficient diffusion is. In fact, there have been suggestions that the standard prescription [204] may be too efficient in the Sun [205] and that diffusion rates should be lowered by ~15%. Solar CNO neutrinos could provide a test for the efficiency of the diffusion.There are other possibilities that might create a contrast between the solar core and surface composition. Recently, it has been shown that the Sun has a peculiar composition when compared to “solar twins,” that is, stars almost identical to the Sun in their surface properties [206, 207]. The authors found that the Sun is enhanced in volatile elements with respect to the solar twins that show no sign of harbouring planets by about 20%. In fact, they have associated this fact to the presence of rocky planets in the solar system, where refractory elements are locked, and the occurrence of an accretion episode of volatile-enriched material [207] after rocky cores is formed in the protoplanetary disk. If this was true, then the Sun would have an envelope that is richer in CNO than its interior. If a measurement of the N13+O15 flux would yield as a result a core composition where the abundance of C + N would be comparable or less than the surface value, then we would have an extremely exciting piece of evidence about the earlier phases of planet formation in the solar system [79].



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*Source: 351926-2013-03-18.xml*