# Heavy Sterile Neutrino in Dark Matter Searches

Authors: Paraskevi C. Divari; John D. Vergados
Journal: Advances in High Energy Physics
 (2018)

---

## Abstract

Sterile neutrinos are possible dark matter candidates. We examine here possible detection mechanisms, assuming that the neutrino has a mass of about 50 keV and couples to the ordinary neutrino. Even though this neutrino is quite heavy, it is nonrelativistic with a maximum kinetic energy of 0.1 eV. Thus new experimental techniques are required for its detection. We estimate the expected event rate in the following cases: (i) measuring electron recoil in the case of materials with very low electron binding; (ii) low temperature crystal bolometers; (iii) spin induced atomic excitations at very low temperatures, leading to a characteristic photon spectrum; (iv) observation of resonances in antineutrino absorption by a nucleus undergoing electron capture; (v) neutrino induced electron events beyond the end point energy of beta decaying systems, for example, in the tritium decay studied by KATRIN.


---

## Body

## 1. Introduction

There exists evidence for existence of dark matter in almost all scales, from the dwarf galaxies, galaxies, and cluster of galaxies, with the most important ones being the observed rotational curves in the galactic halos; see, for example, the review [1]. Furthermore cosmological observations have provided plenty of additional evidence, especially the recent WMAP [2] and Planck [3] data.In spite of this plethora of evidence, it is clearly essential to directly detect such matter in the laboratory in order to unravel its nature. At present there exist many such candidates, called Weakly Interacting Massive Particles (WIMPs). Some examples are the LSP (Lightest Supersymmetric Particle) [4–11], technibaryon [12, 13], mirror matter [14, 15], and Kaluza-Klein models with universal extra dimensions [16, 17]. Among other things these models predict an interaction of dark matter with ordinary matter via the exchange of a scalar particle, which leads to a spin independent interaction (SI) or vector boson interaction and therefore to a spin dependent (SD) nucleon cross section.Since the WIMPs are expected to be extremely nonrelativistic, with average kinetic energy〈T〉≈50keV(mWIMP/100GeV), they are not likely to excite the nucleus, even if they are quite massive, mWIMP>100GeV. Therefore they can be directly detected mainly via the recoiling of a nucleus, first proposed more than 30 years ago [18]. There exists a plethora of direct dark matter experiments with the task of detecting WIMP event rates for a variety of targets such as those employed in XENON10 [19], XENON100 [20], XMASS [21], ZEPLIN [22], PANDA-X [23], LUX [24], CDMS [25], CoGENT [26], EDELWEISS [27], DAMA [28, 29], KIMS [30], and PICASSO [31, 32]. These consider dark matter candidates in the multi-GeV region.Recently, however, an important dark matter particle candidate of the Fermion variety in the mass range of 10–100 keV, obtained from galactic observables, has arisen [33–35]. This scenario produces basically the same behavior in the power spectrum (down to Mpc scales) with that of standard ΛCDM cosmologies, by providing the expected large-scale structure [36]. In addition, it is not too warm; that is, the masses involved are larger than m = 1–3 keV to be in conflict with the current Lyα forest constraints [37] and the number of Milky Way satellites [38], as in standard ΛWDM cosmologies. In fact an interesting viable candidate has been suggested, namely, a sterile neutrino in the mass region of 48–300 keV [33–35, 39–43], but most likely around 50 keV. For a recent review, involving a wider range of masses, see the white paper [44].The existence of light sterile neutrinos had already been introduced to explain some experimental anomalies like those claimed in the short baseline LSND and MiniBooNE experiments [45–47], the reactor neutrino deficit [48], and the Gallium anomaly [49, 50], with possible interpretations discussed, for example, in [51, 52] as well as in [53, 54] for sterile neutrinos in the keV region. The existence of light neutrinos can be expected in an extended see-saw mechanism involving a suitable neutrino mass matrix containing a number of neutrino singlets not all of which being very heavy. In such models it is not difficult to generate more than one sterile neutrino, which can couple to the standard neutrinos [55]. As it has already been mentioned, however, the explanation of cosmological observations requires sterile neutrinos in the 50 keV region, which can be achieved in various models [33, 56].In the present paper we will examine possible direct detection possibilities for the direct detection of these sterile neutrinos. Even though these neutrinos are quite heavy, their detection is not easy. Since like all dark matters candidates move in our galaxies with no relativistic velocities, with average value about10-3 c, and with energies about 0.05 eV, not all of them can be deposited in the detectors. Therefore the standard detection techniques employed in the standard dark matter experiments like those mentioned above are not applicable in this case. Furthermore, the size of the mixing parameter of sterile neutrinos with ordinary neutrinos is crucial for detecting sterile neutrinos. Thus our results concerning the expected event rates will be given in terms of this parameter.The paper is organized as follows. In Section2 we study the option on neutrino-electron scattering. In Section 3 we consider the case of low temperature bolometers. In Section 4 the possibility of neutrino induced atomic excitations is explored. In Section 5 we will consider the antineutrino absorption on nuclei, which normally undergo electron capture, and finally in Section 6 the modification of the end point electron energy in beta decay, for example, in the KATRIN experiment [57], is discussed. In Section 7, we summarize our conclusions.


## 2. The Neutrino-Electron Scattering

The sterile neutrino as dark matter candidate can be treated in the framework of the usual dark matter searches for light WIMPs except that its mass is very small. Its velocity follows a Maxwell-Boltzmann (MB) distribution with a characteristic velocity about10-3 c. Since the sterile neutrino couples to the ordinary electron neutrino it can be detected in neutrino-electron scattering experiments with the advantage that the neutrino-electron cross section is very well known. Both the neutrino and the electron can be treated as nonrelativistic particles. Furthermore we will assume that the electrons are free, since the WIMP energy is not adequate to ionize an the atom. Thus the differential cross section is given by (1)dσ=1υCν2gV2+gA2GF222d3pν′2π3d3pe2π32π4δpν-pν′-peδpν22mν-p′ν22mν-pe22me,where Cν2 is the square of the mixing of the sterile neutrino with the standard electron neutrino νe and GF=Gcos⁡θc, where G=1.1664×10-5GeV-2 denotes the Fermi weak coupling constant and θc≃13° is the Cabibbo angle [58]. The integration over the outgoing neutrino momentum is trivial due to the momentum δ function yielding (2)dσ=1υCν2gV2+gA2GF22212π2d3peδpeυξ-pe22μr,where ξ=p^e·p^ν,0≤ξ≤1, υ is the WIMP velocity, and μr is the WIMP-electron reduced mass, μr≈mν. The electron energy T is given by (3)T=pe22me=2mν2meυξ2⟹0≤T≤2mν2meυesc2,where υesc is the maximum WIMP velocity (escape velocity). Integrating (2) over the angles, using the δ function for the ξ integration we obtain (4)dσ=Cν21υgV2+gA2GF22212πpe2dpe1peυ⟹dσ=Cν21υ2gV2+gA2GF22212πmedT.We are now in a position to fold the velocity distribution assuming it to be MB with respect to the galactic center:(5)fυ′=1πυ03e-υ′/υ02.In the local frame, assuming that the sun moves around the center of the galaxy with velocity υ0=220km/s, υ′=υ+υ0z^, we obtain (6)fly,ξ=1πυ03e-1+y2+2yξ,y=υυ0,where ξ is now the cosine of the angle between the WIMP velocity υ and the direction of the sun’s motion. Eventually we will need the flux so we multiply with the velocity υ before we integrate over the velocity. The limits of integration are between υmin and υesc. The velocity is given via (3); namely, (7)υ=2meT2mνξ⟹υmin=2meT2mνWe find it convenient to express the kinetic energy T in units of T0=2(mν2/me)υ02. Then (8)ymin=x,x=TT0.Thus (9)υdσdT=1υ01T0me16πCν2GF2gV2+gA2∫xyescdyy2πe-1+y2∫-11dξe-2yξ.These integrals can be done analytically to yield(10)υdσdT=1υ0me16πCν2GF2gV2+gA2gx,gx=12erf1-x+erfx+1+erfc1-yesc+erfcyesc+1-2,where erf is the error function and erfc(x) is its complement. The function g(x) characterizes the spectrum of the emitted electrons and is exhibited in Figure 1 and it is without any particular structure, which is the case in most WIMP searches. For a 50 keV sterile neutrino we find that(11)T0=2mνme22.23210-6mec2≈5.0×10-3eVTmax=T0yesc2=5×10-32.842≈0.04eVT=1.6T0=8.0×10-3eV.Figure 1
The shape of the spectrum of the emitted electrons in sterile neutrino-electron scattering.NowdT=T0dx. Thus (12)υσυ0=1υ02meT016πCν2GF2gV2+gA2∫0yesc2dxgx=1.43mν28πCν2GF2gV2+gA2,where (13)∫0yesc2dxgx=1.43.It is clear that with this amount of energy transferred to the electron it is not possible to eject an electron out of the atom. One therefore must use special materials such that the electrons are loosely bound. It has recently been suggested that it is possible to detect even very light WIMPS, much lighter than the electron, utilizing Fermi-degenerate materials like superconductors [59]. In this case the energy required is essentially the gap energy of about 1.5kTc, which is in the meV region; that is, the electrons are essentially free. In what follows, we assume the values(14)gA=1,gV=1+4sin2⁡θW=1.92,GF2=5.02×10-44cm2/MeV2while Cν2 is taken as a parameter and will be discussed in Section 7. Thus we obtain(15)υσυ0=3.47×10-47Cν2cm2.The neutrino particle density is (16)Nν=ρmν=0.3GeV/cm350×10-6GeV=6×103cm-3while the neutrino flux (17)Φν=ρmνυ0=1.32×1011cm-2s-1,where ρ=0.3GeV/cm3, being the dark matter density. Assuming that the number of electron pairs in the target is 2×NA=2×1024 we find that the number of events per year is(18)Φνυσυ02×NA=2.89×10-4Cν2y-1.The authors of [59] are perhaps aware of the fact that the average energy for very light WIMPS is small and as we have seen above a small portion of it is transferred to their system. With their bolometer detector these authors probably have a way to circumvent the fact that a small amount of energy will be deposited, about 0.4 eV in a year for NA≈1024. Perhaps they may manage to accumulate a larger number of loosely bound electrons in their target.


## 3. Sterile Neutrino Detection via Low Temperature Bolometers

Another possibility is to use bolometers, like the CUORE detector exploiting Low Temperature Specific Heat of CrystallineTeO1302 at low temperatures. The energy of the WIMP will now be deposited in the crystal, after its interaction with the nuclei via Z-exchange. In this case the Fermi component of interaction with neutrons is coherent, while that of the protons is negligible. Thus the matrix element becomes (19)ME=GF22NgV,N=number  of  neutrons  in  the  nucleus.A detailed analysis of the frequencies ofTeO1302 can be found [60]. The analysis involved crystalline phases of tellurium dioxide: paratellurite α-TeO2, tellurite β-TeO2, and the new phase -TeO2, recently identified experimentally. Calculated Raman and IR spectra are in good agreement with available experimental data. The vibrational spectra of α and β-TeO2 can be interpreted in terms of vibrations of TeO2 molecular units. The α-TeO2 modes are associated with the symmetry D4 or 422, which has 5 irreducible representations, two 1-dimensional representations of the antisymmetric type indicated by A1 and A2, two 1-dimensional representations of the symmetric types B1 and B2, and one 2-dimensional representation, usually indicated by E. They all have been tabulated in [60]. Those that can be excited must be below the Debye frequency which has been determined [61] and found to be quite low: (20)TD=232±7K°⟹ωD=0.024eV.This frequency is smaller than the maximum sterile neutrino energy estimated to be Tmax=0.11 eV. Those frequency modes of interest to us are given in Table 1. The differential cross section is, therefore, given by(21)dσ=1υCν2N2gV2GF222∑k=18∑ni=0Nkd3pν′2π3d3q2π32π4F2q2δpν-pν′-qδpν22mν-p′ν22mν-ni+12ωk,where Ni will be specified below and q is the momentum transferred to the nucleus. The momentum transfer is small and the form factor F2(q2) can be neglected.Table 1
The frequency modes below the Debye temperature forα-TeO2 obtained from Table VIII of [60] (for notation see text).
ν i = ω i 2 π c m - 1 52 124 128 152 157 176 177 179 Symmetry B 1 E B 1 A 1 B 2 A 2 E B 1 ω i   ( e V ) 0.006 0.015 0.016 0.019 0.019 0.022 0.022 0.022 N i 16 6 6 5 5 4 4 4 E m a x ( i )  ( m e V ) 106 100 102 103 107 98 99 100In deriving this formula we tacitly assumed a coherent interaction between the WIMP and several nuclei, thus creating a collective excitation of the crystal, that is, a phonon or few phonons. This of course is a good approximation provided that the energy transferred is small, of a few tens of meV. We see from Table1 that the maximum allowed energy is small, around 100 meV. We find that, if we restrict the maximum allowed energy by a factor of 2, the obtained results are reduced only by a factor of about 10%. We may thus assume that this approximation is good.Integrating over the nuclear momentum we get(22)dσ=1υCν2N2gV2GF22212π2∑k=18∑ni=0Nkd3pν′δpν22mν-p′ν22mν-ni+12ωkdσ=1υCν2N2gV2GF22212π2∑k=18∑ni=0Nkd3pν′δpν22mν-p′ν22mν-ni+12ωk;performing the integration using the δ function we get (23)σ=1υCν2N2gV2GF2221πmν2mν∑k=18∑ni=1NkEν-ni+12ωkσ=υ0υCν2N2gV2GF2221πmν2∑k=18∑ni=0Nky2-ni+1/2ωkT1,where T1=(1/2)mνυ02,y=υ/υ0Folding with the velocity distribution we obtain(24)υσ=υ0Cν2N2gV2GF2221πmν2∑k=18∑ni=0NkIni,ωk,Ini,ωk=∫yminyescdyfni,ωky,fni,ωky=y2-ni+1/2ωkT1ye-1-y2sinh⁡2y,ymin=ni+1/2ωkT1.We see that we have the constraint imposed by the available energy; namely,(25)Nk=IPyesc2T1ωk-12,where IP[x]= integer part of x. We thus find Nk listed in Table 1. The functions fni,ωk(y) are exhibited in Figure 2. The relevant integrals are In(ω1)=(1.170,0.972,0.785,0.621) for n=0,1,2,3, In(ω2)=(1.032,0.609), for n=0,1, In(ω3)=(1.025,0.592), for n=0,1, and I0(ωk)=(0.979,0.970,0.934,0.932,0.929) for k=4,…,8. Thus we obtain a total of 17.8. The event rate takes with a target of mass mt which takes the form (26)R=ΦνCν2N2gV2GF218πmtAmpmν217.8.If we restrict the maximum allowed energy to half of that shown in Table 1 by a factor of two, we obtain 15.7 instead of 17.8.Figure 2
(a) The functionfn,ω1(y), exhibited as a function of y, associated with the mode ν1=52 cm-1 for n=0,1,2,3 increasing downwards. (b) The functions fn,ω2(y) associated with ν2=124 cm-1 for n=0,1 and f0,ω4 for ν4=157 cm-1, n=0, and f0,ω6 for ν6=176 cm-1, n=0, exhibited as a function of y, for thick solid, solid, dashed, and dotted lines, respectively. For definitions see text.
(a) (b)For aTeO1302 target (N=78) of 1 kg of mass get (27)R=1.7×10-6Cν2per  kg-s=51Cν2per  kg-yThis is much larger than that obtained in the previous section, mainly due to the neutron coherence arising from the Z-interaction with the target (the number of scattering centers is approximately the same, 4.5×1024). In the present case, however, targets can be larger than 1 kg. Next we are going to examine other mechanisms, which promise a better signature.


## 4. Sterile Neutrino Detection via Atomic Excitations

We are going to examine the interesting possibility of excitation of an atom from a level|j1,m1〉 to a nearby level |j2,m2〉 at energy Δ=E2-E1, which has the same orbital structure. The excitation energy has to be quite low; that is, (28)Δ≤12mνυesc2=1250×1032.8422.23210-6=0.11eV.The target is selected so that the two levels |j1,m1〉 and |j2,m2〉 are closer than 0.11 eV. This can result from the splitting of an atomic level by the magnetic field so that they can be connected by the spin operator. The lower one |j1,m1〉 is occupied by electrons but the higher one |j2,m2〉 is completely empty at sufficiently low temperature. It can be populated only by exciting an electron to it from the lower one by the oncoming sterile neutrino. The presence of such an excitation is monitored by a tuned laser which excites such an electron from |j2,m2〉 to a higher state |j3,m3〉, which cannot be reached in any other way, by observing its subsequent decay by emitting photons.Since this is a one-body transition the relevant matrix element takes the form(29)MEj1,m1;j2,m22=gV2δj1,j2δm1,m2+gA2Cl,j1,m1,j2,m22(in the case of the axial current we have gA=1 and we need evaluate the matrix element of σν·σe and then square it and sum and average over the neutrino polarization). (30)Cl,j1,m1,j2,m2=nlj2m2σnlj1m1=j1m1,1m2-m1∣j2m22j1+132l+16l12j1l12j2011expressed in terms of the Clebsch-Gordan coefficient and the nine-j symbol. It is clear that in the energy transfer of interest only the axial current can contribute to excitation.The cross section takes the form(31)dσ=1υCν2GF222MEj1,m1;j2,m22d3pν′2π3d3pA2π32π4δpν-pν′-pAδEν-Δ-Eν′.Integrating over the atom recoil momentum, which has negligible effect on the energy, and over the direction of the final neutrino momentum and energy via the δ function we obtain (32)σ=1υCν2GF222MEj1,m1;j2,m221πEν-Δ2Eν-Δ-mνmν=1υCν2GF222MEj1,m1;j2,m221πmν22T1mνfy,ΔT1fy,ΔT1=y2-ΔT11/2,T1=12mνυ02,where we have set E-Δ=mν+T1-Δ≈mν.Folding the cross section with the velocity distribution from a minimumΔ/T1 to yesc we obtain (33)υσυ0=Cν2GF222mν2MEj1,m1;j2,m221πgΔT1gΔT1=2π∫Δ/T1yescdyy2y2-ΔT11/2e-1+y2sinh⁡2yy.Clearly the maximum excitation energy that can be reached is Δmax=2.842T0=0.108 eV. The function gΔ/T1 is exhibited in Figure 3.Figure 3
The functiongΔ/T1 for sterile neutrino scattering by an atom as a function of the excitation energy in eV.Proceeding as in Section2 and noting that for small excitation energy gΔ/T1≈1.4 we find(34)R=1.8×10-2Cν21ACl,j1,m1,j2,m22kg-y.The expected rate will be smaller after the angular momentum factor Cl,j1,m1,j2,m2 is included (see Appendix A). Anyway, leaving aside this factor, which can only be determined after a specific set of levels is selected, we see that the obtained rate is comparable to that expected from electron recoil (see (18)). In fact for a target with A=100 we obtain (35)R=1.8×10-4Cν2Cl,j1,m1,j2,m22kg-y.This rate, however, decreases as the excitation energy increases (see Figure 3). In the present case, however, we have two advantages. (i)
The characteristic signature of photons spectrum is following the deexcitation of the level|j3,m3〉 mentioned above. The photon energy can be changed if the target is put in a magnetic field by a judicious choice of |j3,m3〉.(ii)
The target now can be much larger, since one can employ a solid at very low temperatures. The ions of the crystal still exhibit atomic structure. The electronic states probably will not carry all the important quantum numbers as their corresponding neutral atoms. One may have to consider exotic atoms (see AppendixB) or targets which contain appropriate impurity atoms in a host crystal, for example, chromium in sapphire.In spite of this it seems very hard to detect such a process, since the expected counting rate is very low.


## 5. Sterile Neutrino Capture by a Nucleus Undergoing Electron Capture

This is essentially the process:(36)ν¯+eb+AN,Z⟶AN+1,Z-1∗involving the absorption of a neutrino with the simultaneous capture of a bound electron. It has already been studied [62] in connection with the detection of the standard relic neutrinos. It involves modern technological innovations like the Penning Trap Mass Spectrometry (PT-MS) and the Microcalorimetry (MC). The former should provide an answer to the question of accurately measuring the nuclear binding energies and how strong the resonance enhancement is expected, whereas the latter should analyze the bolometric spectrum in the tail of the peak corresponding to L-capture to the excited state in order to observe the relic antineutrino events. They also examined the suitability of 157Tb for relic antineutrino detection via the resonant enhancement to be considered by the PT-MS and MC teams. In the present case the experimental constraints are expected to be less stringent since the sterile neutrino is much heavier.Let us measure all energies from the ground state of the final nucleus and assume thatΔ is the mass difference of the two neutral atoms. Let us consider a transition to the final state with energy Ex. The cross section for a neutrino (here as well as in the following we may write neutrino, but it is understood that we mean antineutrino) of given velocity υ and kinetic energy Eν is given by (37)σEν=Cν21υMEExnuc2ϕe2GF222d3pA2π32π4δpA-pνδEν+mν+Δ-Ex-b,where pA is the recoiling nucleus momentum. Integrating over the recoil momentum using the δ function we obtain (38)σEν=Cν22π1υMEExnuc2ϕe2GF222δEν+mν+Δ-Ex-b.We note that since the oncoming neutrino has a mass, the excited state must be higher than the highest excited state at Ex′=Δ-b. With indicating by ϵ=Ex-Ex′ the above equation can be written as (39)σEν=Cν22π1υMEExnuc2ϕe2GF222δEν+mν-ϵ.Folding it with the velocity distribution as above we obtain (40)υσEν=Cν22πMEExnuc2ϕe2GF222∫0yescdyy22πe-1+y2sinh⁡2yyδmν+12mνυ02y2-ϵor using the delta function(41)υσEν=2πCν2MEExnuc2ϕe2mνυ02GF222FX,FX=2πe-1+X2sinh⁡2X,X=1υ02ϵmν-1.As expected the cross section exhibits resonance behavior though the normalized function F(X) as shown in Figure 4. It is, of course, more practical to exhibit the function F(X) as a function of the energy ϵ. This is exhibited in Figure 5. From this figure we see that the cross section resonance is quite narrow. We find that the maximum occurs at ϵ=mν(1+2.8×10-7)= 50 keV + 0.014 eV and has a width Γ=mν(1+9.1×10-7)-mν(1+0.32×10-7)≈ 0.04 eV. So for all practical purposes it is a line centered at the neutrino mass. The width may be of some relevance in the special case whereby the excited state can be determined by atomic deexcitations at the sub-eV level, but it will not show up in the nuclear deexcitations.Figure 4
The cross section exhibits resonance behavior. Shown is the resonance properly normalized as a function ofX=(1/υ0)2ϵ/mν-1. The width is Γ=1.49 and the location of the maximum is at 1.03.Figure 5
The cross section exhibits resonance behavior. Shown isF(X) as a function of (ϵ/mν-1).If there is a resonance in the final nucleus at the energyEx=ϵ+(Δ-b) with a width Γ then perhaps it can be reached even if ϵ is a bit larger than mν; for example, ϵ=mν+Γ/2. The population of this resonance can be determined by measuring the energy of the deexcitation γ-ray, which should exceed by ϵ the maximum observed in ordinary electron capture.For antineutrinos having zero kinetic energy the atom in the final state has to have an excess energyΔ-(b-mν) and this can only happen if this energy can be radiated out via photon or phonon emission. The photon emission takes place either as atomic electron or nuclear level transitions. In the first case photon energies are falling in the eV-keV energy region and this implies that only nuclei with a very small Δ-value could be suitable for this detection. In the second case, there should exist a nuclear level that matches the energy difference Ex=Δ-(b-mν) and therefore the incoming antineutrino has no energy threshold. Moreover, spontaneous electron capture decay is energetically forbidden, since this is allowed for Ex<Δ-(b+mν).As an example we consider the capture of a very low energyν¯ by the 65157Tb nucleus: (42)ν¯+e-+Tb65157⟶Gd64165∗taking the allowed transitions from the ground state (3/2+) of parent nucleus, Tb65157, to the first excited 5/2+ state of the daughter nucleus Gd64157. The spin and parity of the nuclei involved obey the relations ΔJ=1, ΠfΠi=+1, and the transition is dubbed as allowed. The nuclear matrix element ME can be written as (43)ME2=gAgV2GT2,where gA=1.2695 and gV=1 are the axial and vector coupling constants, respectively. The nuclear matrix element is calculated using the microscopic quasi-particle-phonon (MQPM) model [63, 64] and it is found to be |ME|2=0.96. The experimental value of first excited 5/2+ is at 64 keV [65] while that predicted by the model is at 65 keV. The Δ-value is ranging from 60 to 63 keV [65].For K-shell electron capture where〈ϕe〉2=(αZ/π)me3 (1s capture) with binding energy b=50.24 keV, the velocity averaged cross section takes the value (44)συ=8.98×10-46Cν2cm2and the event rate we expect for mass mt=1 kg is (45)R=8.98×10-46Cν2×6103×6.0231023×mtA×9.28×1017y-1=19Cν2y-1.The life time of the source should be suitable for the experiment to be performed. If it is too short, the time available will not be adequate for the execution of the experiment. If it is too long, the number of counts during the data taking will be too small. Then one will face formidable backgrounds and/or large experimental uncertainties.The source should be cheaply available in large quantities. Clearly a compromise has to be made in the selection of the source. One can be optimistic that such adequate quantities can be produced in Russian reactors. The nuclide parameters relevant to our work can be found in [66] (see also [67]), summarized in Table 2.Table 2
Nuclides relevant for the search of the keV sterile neutrinos in the electron capture process. We give the life timeT1/2, the Q-value, the electron binding energy Bi for various captures, and the value of Δ=Q-Bi. For details see [66].
Nuclide T1/2 EC transition Q (keV) B i (keV) B j (keV) Q - B i (keV) Tb   157 71 y 3 / 2 + → 3 / 2 - 60.04(30) K: 50.2391(5) LI: 8.3756(5) 9.76 Ho   163 4570 y 7 / 2 - → 5 / 2 - 2.555(16) MI: 2.0468(5) NI: 0.4163(5) 0.51 Ta   179 1.82 y 7 / 2 + → 9 / 2 + 105.6(4) K: 65.3508(6) LI: 11.2707(4) 40.2 Pt   1 9 3 50 y 1/2-→3/2+ 56.63(30) LI: 13.4185(3) MI: 3.1737(17) 43.2 Pb   202 52 ky 0 + → 2 - 46(14) LI: 15.3467(4) MI: 3.7041(4) 30.7 Pb   20 5 13 My 5/2-→1/2+ 50.6(5) LI: 15.3467(4) MI: 3.7041(4) 35.3 Np   235 396 d 5/2+→7/2- 124.2(9) K: 115.6061(16) LI: 21.7574(3) 8.6


## 6. Modification of the End Point Spectra ofβ Decaying Nuclei

The end point spectra ofβ decaying nuclei can be modified by the reaction involving sterile (anti)neutrinos: (46)ν+AN,Z⟶AN-1,Z+1+e-or (47)ν¯+AN,Z⟶AN+1,Z-1+e+.This can be exploited in on ongoing experiments, for example, in the tritium decay: (48)ν+H13⟶He23+e-.The relevant cross section is (49)σEν=Cν21υMEExnuc2GF222d3pA2π3d3pe2π32π4δpν-pA-peδEν+Δ-Ee,where Δ is the atomic mass difference. Integrating over the nuclear recoil momentum and the direction of the electron momentum we get (50)σEν=Cν21υMEExnuc2GF2221πEePe,where (51)Ee=mν+12mνυ2+Δ+me,Pe=Ee2-me2.Folding the cross section with the velocity distribution we find(52)συ=Cν2GF2222π3/2∫0yescdyfy,where (53)fy=ME2ysinh⁡2yEePee-1+y2FZf,Eewith (54)y=υυ0.The Fermi function, F(Zf,Ee), encapsulates the effects of the Coulomb interaction for a given lepton energy Ee and final state proton number Zf. The function f(y) is exhibited in Figure 6.Figure 6
The shape off(y) for the decay of 3H, where the atomic mass difference between3H and 3He is taking Δ=18.591keV [69].In transitions happening inside the same isospin multiplet (Jπ→Jπ,J≠0) both the vector and axial form factors contribute and in this case the nuclear matrix element ME(Ex) can be written as (55)ME2=F2+gAgV2GT2,where gA=1.2695 and gV=1 are the axial and vector coupling constants, respectively. In case of H3 target we adopt 〈F〉2=0.9987 and 〈GT〉2=2.788 from [68]. Thus |ME|2=5.49.Thus the velocity averaged cross section takes the value(56)συ=3.44×10-46Cν2cm2and the expected event rate becomes (57)R=3.44×10-46Cν2×6103×6.0231023×mtA×9.28×1017y-1.For a mass of the current KATRIN target, that is, about 1 gr, we get (58)R=0.380Cν2y-1.It is interesting to compare the neutrino capture rate(59)Rν=συρmν=3.44×10-46Cν2×6103×9.28×1017=1.91×10-24Cν2y-1with that of beta decay process 3H→3He+e-+ν¯j, whose rate Rβ is given by(60)Rβ=GF22π3∫meWopeEeFZ,EeME2EνpνdEe,where Wo is the maximal electron energy or else beta decay endpoint(61)Wo=Kend+mewith(62)Kend=m3H-me2-m3He+mν22m3H≃Δ=18.591keV,the electron kinetic energy at the endpoint, and (63)me≈510.99891013keVmH3≈2808920.820523keVmHe3≈2808391.219324keV.Masses mH3 and mHe3 are nuclear masses [58, 69, 70]. The calculation of (60) gives Rβ=0.055y-1. The ratio of Rν to corresponding beta decay Rβ is very small.(64)Rν=0.034·10-21Cν2Rβ.The situation is more optimistic in a narrow interval Wo-δ<Ee<Wo near the endpoint. As an example, we consider an energy resolution δ=0.2 eV close to the expected sensitivity of the KATRIN experiment [57]. Then the ratio of the event rate Rβ(δ=0.2eV) to that of neutrino capture Rν gives (65)Rν=5.75·10-9Cν2Rβδ=0.2eV.In Figure7 we present the ratio of the event rate decay rate of Rβ(δ) for the beta decay compared with the neutrino capture rate Rν as a function of the energy resolution δ in the energy region Wo-δ<Ee<Wo.Figure 7
Ratio of decay ratesRν/Rβ (in units of Cν2) as a function of energy resolution δ near the endpoint.Moreover, the electron kinetic energyKe due to neutrino capture process (48) is(66)Ke=Eν+Kend>mν+18.591keV;this means that the electron in the final state has a kinetic energy of at least mν above the corresponding beta decay endpoint energy. There is no reaction induced background there, but, unfortunately, the ratio obtained above is much lower than the expected KATRIN sensitivity.


## 7. Discussion

In the present paper we examined the possibility of direct detection of sterile neutrinos of a mass 50 keV, in dark matter searches. This depends on finding solutions to two problems. The first is the amount of energy expected to be deposited in the detector and the second one is the expected event rate. In connection with the energy we have seen that, even though these neutrinos are quite heavy, their detection is not easy, since like all dark matters candidates move in our galaxies with not relativistic velocities,10-3 c on the average, and with energies about 0.05 eV, not all of which can be deposited in the detectors. Thus the detection techniques employed in the standard dark matter experiments, like those looking for heavy WIMP candidates, are not applicable in this case.We started our investigation by considering neutrino-electron scattering. Since the energy of the sterile neutrino is very small one may have to consider systems with very small electron binding, for example, electron pairs in superconductors, which are limited to rather small number of electron pairs. Alternatively one may use low temperature bolometers, which can be larger in size resulting in a higher expected event rate. These experiments must be able to detect very small amount of energy.Then we examined more exotic options by exploiting atomic and nuclear physics. In atomic physics we examined the possibility of spin induced excitations. Again to avoid background problems the detector has a crystal operating at low temperatures. Then what matters is the atomic structure of the ions of the crystal or of suitably implanted impurities. The rate in this case is less than that obtained in the case of bolometers, but one may be able to exploit the characteristic feature of the spectrum of the emitted photons.From the nuclear physics point of view, we consider the antineutrino absorption on an electron capturing nuclear system leading to a fine resonance in the (N+1,Z-1) system, centered 50 keV above the highest excited state reached by the ordinary electron capture. The deexcitation of this resonance will lead to a very characteristic γ ray. Finally the sterile neutrino will lead to ν+A(N,Z)→e-+A(N-1,Z+1) reaction. The produced electrons will have a maximum energy which goes beyond the end point energy of the corresponding β decay essentially by the neutrino mass. The signature is less profound than in the case of antineutrino absorption.Regarding the event rate, as we have mentioned before, it is proportional to the coupling of the sterile neutrino to the usual electron neutrino indicated above asCν2. This parameter is not known. In neutrino oscillation experiments a value of Cν2≈10-2 has been employed. With such a value our results show that the 50 keV neutrino is detectable in the experiments discussed above. This large value of Cν2 is not consistent, however, with a sterile 50 kev neutrino. In fact such a neutrino would have a life time [71] of 2×105 y, much shorter than the age of the universe. A cosmologically viable sterile 50 keV neutrino is allowed to couple to the electron neutrino with coupling Cν2<1.3×10-7. Our calculations indicate that such a neutrino is not directly detectable with experiments considered in this work. The results, however, obtained for the various physical processes considered in this work, can be very useful in the analysis of the possible experimental searches of lighter sterile neutrinos in the mass range of 1–10 keV.



---

*Source: 1479313-2018-03-15.xml*