# Signature of Plausible Accreting Supermassive Black Holes in Mrk 261/262 and Mrk 266

Authors: Gagik Ter-Kazarian; Lusine Sargsyan
Journal: Advances in Astronomy
 (2013)

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## Abstract

We address the neutrino radiation of plausible accreting supermassive black holes closely linking to the 5 nuclear components of galaxy samples of Mrk 261/262 and Mrk 266. We predict a time delay before neutrino emission of the same scale as the age of the Universe. The ultrahigh energy neutrinos are produced in superdense protomatter medium via simple (quark or pionic reactions) or modified URCA processes (G. Gamow was inspired to name the process URCA after the name of a casino in Rio de Janeiro). The resulting neutrino fluxes for quark reactions are ranging from Jνεq/(εdergcm-2s-1sr-1)≃1.1×10-9 to 8.2×10-9, where εd~10-12 is the opening parameter. For pionic and modified URCA reactions, the fluxes are Jνεπ≃0.1Jνεq and JνεURCA≃7.4×10-11Jνεq, respectively. These fluxes are highly beamed along the plane of accretion disk, peaked at ultrahigh energies, and collimated in smaller opening angle θ~εd.


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## Body

## 1. Introduction

The interactions between galaxies may promote key processes in galaxy evolution including mass assembly, star formation, morphological transformation, and activity of AGNs. Among various proposals is the hierarchical galaxy formation hypothesis, wherein the galaxies and galactic structures are formed through merging of smaller galaxies/structures. The galaxy-galaxy interactions/mergers, as well known, can significantly enhance the star formation rate in the respective galaxies; see, for example, [1] for a review. Each proposal towards galaxy-galaxy interactions/mergers has its own advantage and limitations in proving the whole view of the issue. If tidal plume and tails indicative of classical merger remnants can be seen, it seems reasonable to accept the merging hypothesis, as in the case of many Markarian galaxies with a binary nucleus. However, some Markarian galaxies with multiple nuclei do not show any sign of tidal effects. If obvious tidal features are not easily detectable, it is wise to place constraints on the likelihood of the merger hypothesis as it was done in the pioneering discussions of Ambartsumian in the 1950’s and 1960’s for analyzing the observational data of eruptive activity of galactic nuclei and energetic nonstationary phenomena in the Universe [2–4]. Recently, we present a spectroscopic investigation [5] of the galaxy samples of Mrk 261/262 and Mrk 266. The nuclear components in both of these samples show quite similar emission lines in their spectra. Besides, they do not show any sign of tidal effects. Therefore, one cannot exclude the alternative possibility that galactic nuclei in these samples, for example, may separate by fission rather than merging. A useful framework for such viewpoint is the microscopic theory of black hole (MTBH), originally proposed by [6] (see references therein), and further discussed by [7]. Therefore, our interest is to apply the predictions of MTBH to observational data of unique galaxy samples of Mrk 261/262 and Mrk 266 as a backdrop to validate the microscopic approach with some observational tests. The MTBH supports the idea of accreting supermassive black holes linked to AGNs and their neutrino radiation. With this perspective in sight, we address the essential features of 5 nuclear components in Mrk 261/262 and Mrk 266. Certainly, it would be proper also to compare the prediction on neutrino emission from the large number of AGN black holes, well known from the literature. This will be done elsewhere.


### 1.1. Motivation

We have put forward the microscopic theory of black hole as a possible way to innovate the solution to the key problem of the AGN powerhouse. Recall that ever since the discovery of the rapid release of large amounts of energy from galactic nuclei and the origin of compact objects, the main problem has been to identify the physical mechanisms behind these phenomena. A major unsolved problem is how efficiently such huge energies observed can be generated. This energy scale severely challenges the conventional source models. The longstanding standard phenomenological black hole model (PBHM) cannot successfully support such investigations, because the theory breaks down inside the event horizon, whereas the meaningless singularity develops at the center inside of the stationary black hole, which is causally disconnected from the exterior world. The ultimate fate of the collapsing matter once it has crossed the black hole surface is unknown. So, the central singularity does not allow a further mass assembly. In the framework of PBHM, neither a growth of black hole mass promoted by accretion process nor an increase of energy density occur. Therefore, the required huge energy scale to account for the resulting activity of galactic nuclei cannot be reached. On the other hand, a complex study of AGN evolution requires a comprehensive understanding of the important phenomenon of the black hole growth. This idea gathers support from a breakthrough made in recent observational, theoretical, and computational efforts on understanding of coevolution of black holes and their host galaxies, particularly through self-regulated growth and feedback from accretion-powered outflows; see, for example, [8–14]. Thus, the PBHM cannot be currently accepted as the convincing model for addressing the aforementioned problems. To fill the void which the standard PBHM presents, one possible way to improve this situation is the microscopic theory of black hole. The MTBH is the extension of the PBHM, which rather completes PBHM by exploring the most important processes of rearrangement of vacuum state and a spontaneous breaking of gauge symmetry in gravity at huge energies (see [6, 15, 16]). Thereby, a discussed gravitational theory is consistent with the general relativity up to the limit of neutron stars. Namely, the observational values are in a variety of ways well within the range of theoretically allowed masses of neutron star models discussed here. But MTBH also manifests its virtues applied to the physics of internal structure of galactic nuclei. A significant change of properties of space-time continuum, so-called inner distortion (ID), arises simultaneously with the strong gravity. This causes the matter to undergo a phase transition of second kind, which supply a powerful pathway to form a stable superdense protomatter core (SPC) [6, 7] (see Appendix A.1 of present paper). The crucial difference from PMBH is that the central singularity cannot occur now. Instead, this is replaced by finite though unbelievably extreme conditions. The SPC accommodates the highest energy scale up to hundreds ZeV in protomatter core to account for the spectral distribution of the resulting radiation of galactic nuclei. External physics of accretion onto black hole in the earlier part of its lifetime has tight links to the processes in Schwarzschild’s model. However, an essential difference in the model context between a true black hole and the SPC arises in the later part of its lifetime [7]. The SPC surrounded by the accretion disk presents the microscopic model of AGN (Appendix A.1). The seed black hole might grow up driven by the accretion when it was getting most of its mass. That is, with time an infalling matter forms protomatter disk around protomatter core tapering off faster at reaching out the thin edge of event horizon. At this, metric singularity inevitably disappears and the neutrinos may escape through opened vista to the outside world. We will not be concerned here with the actual details of MTBH. The interested reader is invited to consult the original papers for further details.


### 1.2. Expected Results

Our computations in the present paper are partially based on [7], which has dealt with the preradiation time (PRT) of neutrinos from AGN black holes with well-determined masses and bolometric luminosities, collected from the literature [17]. The PRT is referred to as the earlier part of the lifetime TBH of black hole from its birth till neutrino radiation. For the latter part of the lifetime, T>TBH, the black hole no longer holds as a region of space time that cannot communicate with the external Universe (see Appendix A.1). The ultrahigh energy (UHE) neutrinos are produced in superdense protomatter medium of SPC via simple (quark or pionic reactions) or modified URCA processes. Consequently, the neutrinos may escape through opened vista to outside world even after the neutrino trapping. We estimate the MBH masses and bolometric luminosities Lbol in order to compute the PRTs and neutrino fluxes for the Mrk 261/262 and Mrk 266. These galaxy samples can be served as pure UHE neutrino sources. Note that the point-like sources of neutrinos are the most essential ingredients of Z-burst scenario [18–27] of the origin of ultrahigh energy cosmic ray (UHECR) particles. This scenario is the most economical among the various hypotheses, because the neutrinos can penetrate cosmological distances and their trajectories are not deflected by magnetic fields as they are neutral. The Z-burst scenario suggests that if ZeV astrophysical neutrino beam is sufficiently strong it can produce the observed UHECR particles within 100 Mpc by hitting local light relic neutrinos clustered in dark halos. They form such particles through the hadronic Z (s-channel production) and W-bosons (t-channel production) decays by weak interactions. The discovery of UHE neutrino sources would also clarify the production mechanism of the GeV-TeV gamma rays observed on Earth. The AGNs as significant point sources of neutrinos were analyzed, for example, in [26, 28, 29]. While being hard to detect, neutrinos have the advantage of representing unique fingerprints of hadron interactions and, therefore, of the sources of cosmic rays. At present, a numerous reports are available in the literature on expected discovery potentials and sensitivity of experiments to neutrino point-like sources. Currently, operating high energy neutrino telescopes, see, for example, Antares [30, 31], IceCube [32, 33], Baikal [34], JEM-EUSO mission [35], the Telescope Array experiment [36], Pierre Auger Observatory [37, 38], and so forth, attempt to detect UHE neutrinos. For example, in [32] it is reported on the first measurement of the atmospheric electron neutrino flux in the energy range between approximately 80 GeV and 6 TeV. Using data recorded during the first year of operation of IceCube DeepCore low-energy extension, a sample of 1029 events is observed in 281 days of data, of which 496 ± 66(stat) ± 88(syst) are estimated to be cascade events, including both electron neutrino and neutral current events. The rest of the sample includes residual backgrounds due to atmospheric muons and charged current interactions of atmospheric muon neutrinos. The flux of the atmospheric electron neutrinos is consistent with models of atmospheric neutrinos in this energy range. This constitutes the first observation of electron neutrinos and neutral current interactions in a very large volume neutrino telescope optimized for the TeV energy range.This paper is organized as follows. In Section2 we present the mass and luminosity estimates of 5 nuclear components of Mrk 261/262 and Mrk 266. Section 3 deals with the PRT-simulations for supermassive black holes in the nuclear components. In Section 4 we compute the fluxes of primary UHE neutrinos produced in the superdense protomatter medium. The concluding remarks are presented in Section 5. We will refrain from providing lengthy details of the MTBH and neutrino flux computations. For these, the reader is referred to Appendices A and B.


## 1.1. Motivation

We have put forward the microscopic theory of black hole as a possible way to innovate the solution to the key problem of the AGN powerhouse. Recall that ever since the discovery of the rapid release of large amounts of energy from galactic nuclei and the origin of compact objects, the main problem has been to identify the physical mechanisms behind these phenomena. A major unsolved problem is how efficiently such huge energies observed can be generated. This energy scale severely challenges the conventional source models. The longstanding standard phenomenological black hole model (PBHM) cannot successfully support such investigations, because the theory breaks down inside the event horizon, whereas the meaningless singularity develops at the center inside of the stationary black hole, which is causally disconnected from the exterior world. The ultimate fate of the collapsing matter once it has crossed the black hole surface is unknown. So, the central singularity does not allow a further mass assembly. In the framework of PBHM, neither a growth of black hole mass promoted by accretion process nor an increase of energy density occur. Therefore, the required huge energy scale to account for the resulting activity of galactic nuclei cannot be reached. On the other hand, a complex study of AGN evolution requires a comprehensive understanding of the important phenomenon of the black hole growth. This idea gathers support from a breakthrough made in recent observational, theoretical, and computational efforts on understanding of coevolution of black holes and their host galaxies, particularly through self-regulated growth and feedback from accretion-powered outflows; see, for example, [8–14]. Thus, the PBHM cannot be currently accepted as the convincing model for addressing the aforementioned problems. To fill the void which the standard PBHM presents, one possible way to improve this situation is the microscopic theory of black hole. The MTBH is the extension of the PBHM, which rather completes PBHM by exploring the most important processes of rearrangement of vacuum state and a spontaneous breaking of gauge symmetry in gravity at huge energies (see [6, 15, 16]). Thereby, a discussed gravitational theory is consistent with the general relativity up to the limit of neutron stars. Namely, the observational values are in a variety of ways well within the range of theoretically allowed masses of neutron star models discussed here. But MTBH also manifests its virtues applied to the physics of internal structure of galactic nuclei. A significant change of properties of space-time continuum, so-called inner distortion (ID), arises simultaneously with the strong gravity. This causes the matter to undergo a phase transition of second kind, which supply a powerful pathway to form a stable superdense protomatter core (SPC) [6, 7] (see Appendix A.1 of present paper). The crucial difference from PMBH is that the central singularity cannot occur now. Instead, this is replaced by finite though unbelievably extreme conditions. The SPC accommodates the highest energy scale up to hundreds ZeV in protomatter core to account for the spectral distribution of the resulting radiation of galactic nuclei. External physics of accretion onto black hole in the earlier part of its lifetime has tight links to the processes in Schwarzschild’s model. However, an essential difference in the model context between a true black hole and the SPC arises in the later part of its lifetime [7]. The SPC surrounded by the accretion disk presents the microscopic model of AGN (Appendix A.1). The seed black hole might grow up driven by the accretion when it was getting most of its mass. That is, with time an infalling matter forms protomatter disk around protomatter core tapering off faster at reaching out the thin edge of event horizon. At this, metric singularity inevitably disappears and the neutrinos may escape through opened vista to the outside world. We will not be concerned here with the actual details of MTBH. The interested reader is invited to consult the original papers for further details.


## 1.2. Expected Results

Our computations in the present paper are partially based on [7], which has dealt with the preradiation time (PRT) of neutrinos from AGN black holes with well-determined masses and bolometric luminosities, collected from the literature [17]. The PRT is referred to as the earlier part of the lifetime TBH of black hole from its birth till neutrino radiation. For the latter part of the lifetime, T>TBH, the black hole no longer holds as a region of space time that cannot communicate with the external Universe (see Appendix A.1). The ultrahigh energy (UHE) neutrinos are produced in superdense protomatter medium of SPC via simple (quark or pionic reactions) or modified URCA processes. Consequently, the neutrinos may escape through opened vista to outside world even after the neutrino trapping. We estimate the MBH masses and bolometric luminosities Lbol in order to compute the PRTs and neutrino fluxes for the Mrk 261/262 and Mrk 266. These galaxy samples can be served as pure UHE neutrino sources. Note that the point-like sources of neutrinos are the most essential ingredients of Z-burst scenario [18–27] of the origin of ultrahigh energy cosmic ray (UHECR) particles. This scenario is the most economical among the various hypotheses, because the neutrinos can penetrate cosmological distances and their trajectories are not deflected by magnetic fields as they are neutral. The Z-burst scenario suggests that if ZeV astrophysical neutrino beam is sufficiently strong it can produce the observed UHECR particles within 100 Mpc by hitting local light relic neutrinos clustered in dark halos. They form such particles through the hadronic Z (s-channel production) and W-bosons (t-channel production) decays by weak interactions. The discovery of UHE neutrino sources would also clarify the production mechanism of the GeV-TeV gamma rays observed on Earth. The AGNs as significant point sources of neutrinos were analyzed, for example, in [26, 28, 29]. While being hard to detect, neutrinos have the advantage of representing unique fingerprints of hadron interactions and, therefore, of the sources of cosmic rays. At present, a numerous reports are available in the literature on expected discovery potentials and sensitivity of experiments to neutrino point-like sources. Currently, operating high energy neutrino telescopes, see, for example, Antares [30, 31], IceCube [32, 33], Baikal [34], JEM-EUSO mission [35], the Telescope Array experiment [36], Pierre Auger Observatory [37, 38], and so forth, attempt to detect UHE neutrinos. For example, in [32] it is reported on the first measurement of the atmospheric electron neutrino flux in the energy range between approximately 80 GeV and 6 TeV. Using data recorded during the first year of operation of IceCube DeepCore low-energy extension, a sample of 1029 events is observed in 281 days of data, of which 496 ± 66(stat) ± 88(syst) are estimated to be cascade events, including both electron neutrino and neutral current events. The rest of the sample includes residual backgrounds due to atmospheric muons and charged current interactions of atmospheric muon neutrinos. The flux of the atmospheric electron neutrinos is consistent with models of atmospheric neutrinos in this energy range. This constitutes the first observation of electron neutrinos and neutral current interactions in a very large volume neutrino telescope optimized for the TeV energy range.This paper is organized as follows. In Section2 we present the mass and luminosity estimates of 5 nuclear components of Mrk 261/262 and Mrk 266. Section 3 deals with the PRT-simulations for supermassive black holes in the nuclear components. In Section 4 we compute the fluxes of primary UHE neutrinos produced in the superdense protomatter medium. The concluding remarks are presented in Section 5. We will refrain from providing lengthy details of the MTBH and neutrino flux computations. For these, the reader is referred to Appendices A and B.


## 2. The Mass and Luminosity Estimates from Optical Observations of Mrk 261/262 and Mrk 266

BH Mass Estimate. The results of observations for Mrk 266 with the Spitzer, Hubble, GALEX, Chandra, and XMM-Newton space telescopes are presented in [39]. The relationship between H-band bulge luminosity and the mass of the nuclear black hole [40] (Group 1 Galaxies) provides MBH estimates of 2.3×108 and 2.6×108M⊙ for Mrk 266 SW and NE, respectively, where the scatter is 0.3 in log. The luminosity of high ionization, mid-infrared emission lines can also be used to estimate MBH using relationships derived by [41]. The [Ne V] 14.32 μm ([O IV] 25.89 μm) emission line luminosity of 1.58(10.5)×1041 erg s−1, computed from published high resolution Infrared Spectrograph on board Spitzer Space Telescope (IRS) measurements [42, 43], corresponds to MBH=1.7(3.2)×108M⊙ for the SW nucleus, where the scatter is 0.46 and 0.47 in log. These values are in good agreement with the estimates based on the SW bulge luminosity. However, it should be emphasized that the available IRS data did not have sufficient spectral and spatial resolution to extract [Ne V] and [O IV] line fluxes for the NE nucleus. The differences arise from the wide scatter in calibrating MBH versus luminosity or velocity dispersion. Also, there is no similar infrared spectral observation for Mrk261/262. Therefore, we are going to estimate the black hole masses in the same way from our optical spectra of Mrk261/262 and Mrk 266 [5], using the width of the [OIII]λ5007 line. Note that a tight correlation exists for active galaxies between the velocity dispersion σ* of the bulge in a galaxy and the mass of its nuclear black hole MBH [44, 45]. Moreover, many groups have used the width of the [OIII]λ5007 line as a substitute for the stellar velocity dispersion σ* of galaxy bulges. So, at the very beginning we may plot the MBH/M⊙-σ* relation on logarithmic scales (Figure 1) for 17 objects chosen from [46]. These objects have the most accurate MBH measurements based on a complete and consistent reanalysis of broad emission-line reverberation-mapping data and [OIII]λ5007 FWHMs. Scatter about the mass-luminosity relationship for these AGNs appears to be real and could be correlated with either Eddington ratio or object inclination. The formula of the fitted solid line to the data with a scatter of ±0.42 in log is
(1)Log(MBHM⊙)=2.01(±0.83)Logσ*+3.07(±1.83).
Next, from our optical spectra [5] (Figures 2, 3, and 4) we may calculate the values of σ* for Mrk 261/262 and Mrk 266. As a proxy for the velocity dispersion σ* we use the [OIII]λ5007 line width FWHM[OIII]/2.35(km/s); see Table 1. And then, from relation (1) we may derive the black hole masses for these values of σ*; see Table 2. Our optical spectra of the Mrk261/262 are obtained on the 6 m telescope at Special Astrophysical Observatory of Russia, with the Universal Astronomical Grating Spectrograph. The detector was a 530 × 580, 18 × 24 μm pixel CCD, and the spectral band was λ(3720Å)-λ(7150Å). The hz44 standard star was chosen for flux calibration, and the spectral dispersion was 5.9 Å/pix. The resolution, as measured on the night sky lines, was ~16.3 Å (FWHM). In [5], we also used the observational data of Mrk 266, obtained on the 5 m Hale telescope at Palomar Observatory with the Norris Spectrograph. Rotating the position angle by 45 degrees, each component was observed in red and blue parts at different position angles of 31°, 76°, 121°, and 166°. The pixel scale of detector was 1024 × 256 pixels for red part and 180 × 800 pixels for blue part. The exposure times amounted to 900 s for each spectrum in case of position angle 31°, but the 420 s exposures were taken for the rest of position angles. The spectral dispersions were 2.2 and 0.66 Å/pix, respectively, for spectral bands of blue part, λ(3750Å)-λ(5500Å), and red part, λ(6450Å)-λ(7100Å). The resolution, as measured on the night sky lines, was ~7.5 Å (FWHM) for the blue part, and ~1.8 Å (FWHM) for the red part. As it is seen, the nuclear components in both of these samples show quite similar emission lines in their spectra. Treating the instrumental profile and the intrinsic profile to sum as Gaussians is a good approximation [47]. A formal solution, in general, is a deconvolution, but this comes very close to the same result. Thus, unfolding wholly the forbidden [OIII]λ5007 line profile into its Gaussian component, the question can be resolved by subtraction of instrumental broadening (for the real Doppler broadening λD of the [OIII]λ5007 lines see Table 1).Table 1
The characteristics of the [OIII](λ 5007) km/s line from nuclear spectra in Mrk 261/262 and Mrk 266. Columns: (1) name; (2) redshift; (3) FWHM of the line [OIII]λ5007 in km/s; and (4) σ*=FWHM[OIII]/2.35(km/s) is the width of the [OIII]λ5007 line as a proxy for the stellar velocity dispersion σ* on logarithmic scale.
Name
z
[OIII]λ5007 FWHM km/s
log
σ
*
Mrk 261/262
Mrk261_(1)
0.0296
531
2.35
Mrk261_(2)
0.0301
426
2.26
Mrk 262
0.0304
671
2.46
Mrk 266
A
0.02759
414
2.25
B
0.02800
501
2.33Table 2
The physical characteristics of components in Mrk 261/262 and Mrk 266. Columns: (1) name; (2) log of black hole mass; (3) log ofλLλ(5100Å)/L⊙ luminosity; and (4) log of (bolometric luminosity/L⊙).
Name
log
(
M
BH
/
M
⊙
)
log
(
λ
L
λ
(
5100
Å
)
/
L
⊙
)
log
(
L
bol
/
L
⊙
)
Mrk 261/262
Mrk261_(1)
7.97
10.30
11.27
Mrk261_(2)
7.77
10.07
11.04
Mrk 262
8.18
10.55
11.51
Mrk 266
A
7.74
10.04
11.01
B
7.91
10.24
11.21Figure 1
TheMBH/M⊙-σ* relation on logarithmic scales for 17 objects from [46]. The solid line is the best fits to data of samples.The spectra of the nuclear components Mrk 261_1 and Mrk 261_2 in the sample Mrk 261/262.
(a)
(b)Figure 3
The spectrum of the nuclear component Mrk 262 in the sample Mrk 261/262.The blue and red spectra of the nuclear components (A) and (B) in the Mrk 266.
(a)
(b)
(c)
(d)Bolometric Luminosity Estimate. The bolometric luminosity is not straightforward to derive for most of the AGNs because of beaming and obscuration. It was sometimes also approximated from optical luminosity, since integration of the spectral energy distribution is usually hampered by lack of wavelength coverage and by variability. In our calculation, we use the total bolometric luminosity, which, according to [48], equals 9.26 times the value of the visual luminosity λLλ(5100 Å). For this, we need to derive the visual luminosities λLλ(5100 Å) for the Mrk 266 and Mrk 251/262. In the first step, we may find a correlation between the visual luminosities λLλ(5100 Å) for 34 AGNs and black hole masses, presented in [46], which is plotted in Figure 5. The fitted line formula is
(2)Log(λLλ(5100Å)L⊙)=1.16(±0.12)Log(MBHM⊙)+1.06(±0.99),
with the scatter ±0.45 in log. We then looked for the visual luminosities λLλ(5100 Å) for Mrk 266 and Mrk 251/262, which can be estimated from this relation. And then, we derive the required bolometric luminosities; see Table 2.Figure 5
TheMBH/M⊙-Lλ(5100Å)/L⊙ relation on logarithmic scales for 34 objects from [46]. The solid line is the best fits to data of samples.


## 3. PRT Simulations for Mrk 261/262 and Mrk 266

In the framework of MTBH, the PRT is referred to as the earlier part of the lifetimeTBH of SPC. During this time an infalling matter forms protomatter disk around the protomatter core tapering off faster at reaching out the thin edge of event horizon. That is, TBH=Md/M˙, where M˙ is the accretion rate. Assuming a typical mass-energy conversion efficiency of about ϵ~10%, in approximation Rd≪Rg the PRT reads (see Appendix A.2)
(3)TBH≃0.32RdrOV(MBHM⊙)21039WLbolyr,
where rOV=13.68 km.SPC-Configurations. As a working model we assume the SPC-configurations, which are discussed in [6]. They are composed of spherical-symmetric distribution of matter in many-phase stratified states. The I-class SPC-configuration above the density ρ>ρd=2.6×1016 g cm−3 is thought to have central core composed of the n-p-e protomatter, which is mixture of neutrons, protons, and electrons in complete β-equilibrium, at short nucleon-nucleon distances rNN≤0.4 fm in presence of ID. The second class SPC-configuration, above the density ρ>ρd, is thought to have protomatter core made of quarks in one bag in complete β-equilibrium under the weak interactions and gluons, including the effects of QCD-perturbative interactions (for details see Appendix A.1).Modeling. With the black hole masses and bolometric luminosities given in Tables 2 and 3, we proceed to PRT-simulations. The main idea comes to solving an inverse problem. Namely, by reiterating integrations of the state equations of SPC-configurations we determine those required central values of particle concentration n(0) and ID-field x(0), for which the total mass of configuration obtained after integration is equal to the black hole mass estimated from observations. Among all the integral characteristics, the radius Rd is also computed, which is used to calculate TBH. The results are summed up in Table 3. The obtained PRT values are ranging from Log(TBH/yr)≃9.89 to 10.43 for the masses Log(MBH/M⊙)≃7.77 to 8.18 of central black holes in 5 nuclear components of the samples of Mrk 261/262 and Mrk 266. Figure 6 plots the PRT-mass relation on logarithmic scales.Table 3
The PRTs and fluxes for the multinuclei samples Mrk 261/262 and Mrk 266. Columns: (1) name; (2) log of radius (km) of PC; (3) log of PRT (yr); (4)Jq is the log of the (Jνεq/εd erg cm−2 s−1 sr−1); (5) Jπ is the log of the (Jνεπ/εd erg cm−2 s−1 sr−1); and (6) Ju is the log of the (JνεURCA/εd erg cm−2 s−1 sr−1).
Name
log
(
R
d
) (km)
log
(
T
BH
) (yr)
J
ε
q
J
ε
π
J
ε
u
Mrk 261/262
Mrk261_(1)
−4.13
10.22
−8.55
−9.51
−18.69
Mrk261_(2)
−4.0
9.89
−8.22
−9.17
−18.35
Mrk 262
−4.38
10.43
−8.95
−9.90
−18.08
Mrk 266
A
−4.07
10.20
−8.09
−9.04
−18.22
B
−4.35
9.95
−8.40
−9.35
−18.53Figure 6
TheMBH/M⊙-PRT relation on logarithmic scales in Mrk 261/262 and Mrk 266. The resulting PRTs are of the same scale as the age of the Universe.


## 4. UHE Neutrino Fluxes

We are now in a position to compute the UHE neutrino fluxes. We have chosen the cosmological model favored today, with a flat Universe filled with matterΩM=ρM/ρc and vacuum energy densities ΩV=ρV/ρc. Thereby ΩV+ΩM=1, where the critical energy density ρc=3H02/(8πGN) is defined through the Hubble parameter H0. For our calculations we have taken the values H0=70 km/s/Mpc, ΩV=0.7, and ΩM=0.3.


### 4.1. URCA Reactions

In the framework of MTBH, the total UHE neutrino spectral flux of cooling of the SPC, of given massM~, by modified URCA reactions with no muons, reads (Appendix B.1),
(4)JνεURCA≃5.22×10-8εdI2(z)(1+z)(M⊙M~)1.75ergcm-2s-1sr-1,
where the neutrino is radiated in a cone with the beaming angle θ~εd=d/2Rg, d is the thickness of the protomatter disk at the edge of even horizon and I(z)=(1+z)∫11+z‍dx/2.3+x3. As it is seen, the nucleon modified URCA reactions can contribute efficiently only for extragalactic objects with enough small redshift z≪1.


### 4.2. Pionic Reactions

The pionic reactions, which occurred in the superdense protomatter medium of SPC, allow both the distorted energy and momentum to be conserved. The following is the analogue of the simple URCA processes:(5)π-+n⟶n+e-+ν-e,π-+n⟶n+μ-+ν-μ,
and the two inverse processes. As in the modified URCA reactions, the total rate for all four processes is essentially four times the rate of each reaction alone. The muons are already present when pions appear. The UHE neutrino mean flux is given (Appendix B.2) as
(6)Jνεπ≃7.91εdI2(z)(1+z)(M⊙M~)1.75ergcm-2s-1sr-1.
The resulting total energy-loss rate will then be dramatically larger due to the pionic reactions (5) rather than the modified URCA processes.


### 4.3. Quark Reactions

In the superdense protomatter medium, the distorted quark Fermi energies are far below the charmedc-, t-, and b-quark production thresholds. Therefore, only up, down, and strange quarks are present. The β equilibrium is maintained by reactions like
(7)d⟶u+e-+ν-e,u+e-⟶d+νe,(8)s⟶u+e-+ν-e,u+e-⟶s+νe,
which are β decay and its inverse. These reactions constitute simple URCA processes, in which there is a net loss of a νlν-l pair at nonzero temperatures. In this application, a sufficient accuracy is obtained by assuming β equilibrium and that the neutrinos not to be retained in the medium of Λ-like protomatter. The quark reactions (7) and (8) proceed at equal rates in β equilibrium, where the participating quarks must reside close to their Fermi surface. Hence, the total energy of flux due to simple URCA processes is rather twice that of (7) or (8) alone. The total flux of UHE neutrino can be written (Appendix B.3) as
(9)Jνεq≃70.68εdI2(z)(1+z)(M⊙M~)1.75ergcm-2s-1sr-1.


### 4.4. Total Flux Simulation

For total flux simulation we use the data of all the black hole mass and luminosity estimates from Table2. Solving the inverse problem, we determine the radii and surface temperatures corresponding to these sources. The results of the computation are summed up in the Table 3, and are shown in Figures 7, 8, and 9. The last three columns present the neutrino fluxes Fεi (i=q,π,u), which are the log of (εdFi/(erg cm−2 s−1 sr−1)). They are ranging from Jνεq/(εdergcm-2s-1sr-1)≃1.1×10-9 to 8.2×10-9; Jνεπ≃0.1Jνεq; JνεURCA≃7.4×10-11Jνεq.Figure 7
UHE neutrino fluxes on logarithmic scales of the plausible black holes in 5 nuclear components in Mrk 261/262 and Mrk 266.Ju is the Log of (JνεURCA/εd erg cm−2 s−1 sr−1).Figure 8
UHE neutrino fluxes on logarithmic scales of the plausible black holes in 5 nuclear components in Mrk 261/262 and Mrk 266.Jπ is the Log of (Jνεπ/εd erg  cm−2 s−1 sr−1).Figure 9
UHE neutrino fluxes on logarithmic scales of the plausible black holes in 5 nuclear components in Mrk 261/262 and Mrk 266.Jq is the Log of (Jνεq/εd erg cm−2 s−1 sr−1).


## 4.1. URCA Reactions

In the framework of MTBH, the total UHE neutrino spectral flux of cooling of the SPC, of given massM~, by modified URCA reactions with no muons, reads (Appendix B.1),
(4)JνεURCA≃5.22×10-8εdI2(z)(1+z)(M⊙M~)1.75ergcm-2s-1sr-1,
where the neutrino is radiated in a cone with the beaming angle θ~εd=d/2Rg, d is the thickness of the protomatter disk at the edge of even horizon and I(z)=(1+z)∫11+z‍dx/2.3+x3. As it is seen, the nucleon modified URCA reactions can contribute efficiently only for extragalactic objects with enough small redshift z≪1.


## 4.2. Pionic Reactions

The pionic reactions, which occurred in the superdense protomatter medium of SPC, allow both the distorted energy and momentum to be conserved. The following is the analogue of the simple URCA processes:(5)π-+n⟶n+e-+ν-e,π-+n⟶n+μ-+ν-μ,
and the two inverse processes. As in the modified URCA reactions, the total rate for all four processes is essentially four times the rate of each reaction alone. The muons are already present when pions appear. The UHE neutrino mean flux is given (Appendix B.2) as
(6)Jνεπ≃7.91εdI2(z)(1+z)(M⊙M~)1.75ergcm-2s-1sr-1.
The resulting total energy-loss rate will then be dramatically larger due to the pionic reactions (5) rather than the modified URCA processes.


## 4.3. Quark Reactions

In the superdense protomatter medium, the distorted quark Fermi energies are far below the charmedc-, t-, and b-quark production thresholds. Therefore, only up, down, and strange quarks are present. The β equilibrium is maintained by reactions like
(7)d⟶u+e-+ν-e,u+e-⟶d+νe,(8)s⟶u+e-+ν-e,u+e-⟶s+νe,
which are β decay and its inverse. These reactions constitute simple URCA processes, in which there is a net loss of a νlν-l pair at nonzero temperatures. In this application, a sufficient accuracy is obtained by assuming β equilibrium and that the neutrinos not to be retained in the medium of Λ-like protomatter. The quark reactions (7) and (8) proceed at equal rates in β equilibrium, where the participating quarks must reside close to their Fermi surface. Hence, the total energy of flux due to simple URCA processes is rather twice that of (7) or (8) alone. The total flux of UHE neutrino can be written (Appendix B.3) as
(9)Jνεq≃70.68εdI2(z)(1+z)(M⊙M~)1.75ergcm-2s-1sr-1.


## 4.4. Total Flux Simulation

For total flux simulation we use the data of all the black hole mass and luminosity estimates from Table2. Solving the inverse problem, we determine the radii and surface temperatures corresponding to these sources. The results of the computation are summed up in the Table 3, and are shown in Figures 7, 8, and 9. The last three columns present the neutrino fluxes Fεi (i=q,π,u), which are the log of (εdFi/(erg cm−2 s−1 sr−1)). They are ranging from Jνεq/(εdergcm-2s-1sr-1)≃1.1×10-9 to 8.2×10-9; Jνεπ≃0.1Jνεq; JνεURCA≃7.4×10-11Jνεq.Figure 7
UHE neutrino fluxes on logarithmic scales of the plausible black holes in 5 nuclear components in Mrk 261/262 and Mrk 266.Ju is the Log of (JνεURCA/εd erg cm−2 s−1 sr−1).Figure 8
UHE neutrino fluxes on logarithmic scales of the plausible black holes in 5 nuclear components in Mrk 261/262 and Mrk 266.Jπ is the Log of (Jνεπ/εd erg  cm−2 s−1 sr−1).Figure 9
UHE neutrino fluxes on logarithmic scales of the plausible black holes in 5 nuclear components in Mrk 261/262 and Mrk 266.Jq is the Log of (Jνεq/εd erg cm−2 s−1 sr−1).


## 5. Conclusions

In the framework of MTBH, we address the neutrino radiation of plausible accreting supermassive black holes closely linked to 5 nuclear components of unusual galaxy samples of Mrk261/262 and Mrk 266. This necessarily requires to estimate more accurately the values of black hole masses and bolometric luminosities for these nuclear components. We estimate these values from our observations and predict an ~10 Gyr time delay before neutrino emission. The UHE neutrinos with energies up to hundreds ZeV are produced in superdense protomatter medium via simple (quark and pionic reactions) or modified URCA processes, even after the neutrino trapping. The computed neutrino fluxes for quark reactions are ranging fromJνεq/(εdergcm-2s-1sr-1)≃1.1×10-9 to 8.2×10-9. For pionic and modified URCA reactions, the fluxes are Jνεπ≃0.1Jνεq and JνεURCA≃7.4×10-11Jνεq, respectively. These fluxes are highly beamed along the plane of accretion disk, peaked at ultrahigh energies and collimated in smaller opening angle εd~θ~10-12. The Mrk 261/262 and Mrk 266, therefore, may be of interest for the Z-burst scenario of origin of UHECRs. Such neutrinos may initiate the cascades of UHE cosmic rays via very complex chains of Z-burst interactions. Some part of UHE neutrinos may produce in accretion disk and in a torus of hot gas surrounding the AGN core the secondary electrons with huge energies. The latter, in turn, may give rise to a secondary flux of the GeV-TeV gamma rays.



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*Source: 710906-2013-09-29.xml*