# Heavy Sterile Neutrino in Dark Matter Searches.

1. IntroductionThere 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> [approximately equal to] 50 keV ([m.sub.WIMP]/ 100 GeV), they are not likely to excite the nucleus, even if they are quite massive, [m.sub.WIMP] > 100 GeV. 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 [LAMBDA]CDM 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 Ly[alpha] forest constraints [37] and the number of Milky Way satellites [38], as in standard [LAMBDA]WDM 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 about [10.sup.-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 Section 2 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 about [10.sup.-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

[mathematical expression not reproducible], (1)

where [C.sup.2.sub.[nu]] is the square of the mixing of the sterile neutrino with the standard electron neutrino [[nu].sub.e] and [G.sub.F] = G cos [[theta].sub.c], where G = 1.1664 x [10.sup.-5] [GeV.sup.-2] denotes the Fermi weak coupling constant and [[theta].sub.c] [equivalent] 13[degrees] is the Cabibbo angle [58]. The integration over the outgoing neutrino momentum is trivial due to the momentum [delta] function yielding

[mathematical expression not reproducible], (2)

where [xi] = [[??].sub.e] x [[??].sub.[nu]], 0 [less than or equal to] [xi] [less than or equal to] 1, [upsilon] is the WIMP velocity, and [[mu].sub.r] is the WIMP-electron reduced mass, [[mu].sub.r] [approximately equal to] [m.sub.[nu]]. The electron energy T is given by

T = [p.sup.2.sub.e]/2[m.sub.e] = 2 [[m.sup.2.sub.[nu]]/[m.sub.e]] [([upsilon][xi]).sup.2] [??] 0 [less than or equal to] T [less than or equal to] 2 [[m.sup.2.sub.[nu]]/[m.sub.e]] [[upsilon].sup.2.sub.esc], (3)

where [[upsilon].sub.esc] is the maximum WIMP velocity (escape velocity). Integrating (2) over the angles, using the [delta] function for the [xi] integration we obtain

[mathematical expression not reproducible]. (4)

We are now in a position to fold the velocity distribution assuming it to be MB with respect to the galactic center:

[mathematical expression not reproducible]. (5)

In the local frame, assuming that the sun moves around the center of the galaxy with velocity [[upsilon].sub.0] = 220km/s, [upsilon]' = [upsilon] + [[upsilon].sub.0][??], we obtain

[mathematical expression not reproducible], (6)

where [xi] is now the cosine of the angle between the WIMP velocity [upsilon] and the direction of the sun's motion. Eventually we will need the flux so we multiply with the velocity [upsilon] before we integrate over the velocity. The limits of integration are between [[upsilon].sub.min] and [[upsilon].sub.esc]. The velocity is given via (3); namely,

[upsilon] = [square root of (2[m.sub.e]T)]/2[m.sub.[nu]][xi] [??] [[upsilon].sub.min] = [square root of (2[m.sub.e]T)]/2[m.sub.[nu]] (7)

We find it convenient to express the kinetic energy T in units of [T.sub.0] = 2([m.sup.2.sub.[nu]]/[m.sub.e])[[upsilon].sup.2.sub.0]. Then

[y.sub.min] = [square root of (x)], x = T/[T.sub.0]. (8)

Thus

[mathematical expression not reproducible]. (9)

These integrals can be done analytically to yield

[mathematical expression not reproducible], (10)

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

[mathematical expression not reproducible]. (11)

Now dT = [T.sub.0]dx. Thus

[mathematical expression not reproducible], (12)

where

[mathematical expression not reproducible]. (13)

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 1.5k[T.sub.c], which is in the meV region; that is, the electrons are essentially free. In what follows, we assume the values

[g.sub.A] = 1, [g.sub.V] = 1 + 4 [sin.sup.2] [[theta].sub.W] = 1.92, [G.sup.2.sub.F = 5.02 x [10.sup.-44] [cm.sup.2]/[MeV.sup.2] (14)

while [C.sup.2.sub.[nu]] is taken as a parameter and will be discussed in Section 7. Thus we obtain

<[upsilon][sigma]>/[[upsilon].sub.0] = 3.47 x [10.sup.-47][C.sup.2.sub.[nu]] [cm.sup.2]. (15)

The neutrino particle density is

[N.sub.[nu]] = [rho]/[m.sub.[nu]] = [0.3 GeV/[cm.sub.3]]/[50 x [10.sup.-6] GeV] = 6 x [10.sup.3] [cm.sup.-3] (16)

while the neutrino flux

[[PHI].sub.[nu]] = [[rho]/[m.sub.[nu]]] [[upsilon].sub.0] = 1.32 x [10.sup.11] [cm.sup.-2][s.sup.-1], (17)

where [rho] = 0.3 GeV/[cm.sup.3], being the dark matter density. Assuming that the number of electron pairs in the target is 2 x [N.sub.A] = 2 x [10.sup.24] we find that the number of events per year is

[[PHI].sub.[nu]] [<[upsilon][sigma]>/[[upsilon].sub.0]] 2 x [N.sub.A] = 2.89 x [10.sup.-4][C.sup.2.sub.[nu]] [y.sup.-1]. (18)

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 [N.sub.A] [approximately equal to] [10.sup.24]. 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 Crystalline [sup.130]Te[O.sub.2] 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

ME = [G.sub.F]/2[square root of (2)] N[g.sub.V], N = number of neutrons in the nucleus. (19)

A detailed analysis of the frequencies of [sup.130]Te[O.sub.2] can be found [60]. The analysis involved crystalline phases of tellurium dioxide: paratellurite [alpha]-Te[O.sub.2], tellurite [beta]-Te[O.sub.2], 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 [alpha] and [beta]-Te[O.sub.2] can be interpreted in terms of vibrations of Te[O.sub.2] molecular units. The [alpha]-Te[O.sub.2] modes are associated with the symmetry [D.sub.4] or 422, which has 5 irreducible representations, two 1-dimensional representations of the antisymmetric type indicated by A1 and [A.sub.2], two 1-dimensional representations of the symmetric types B1 and [B.sub.2], 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:

[T.sub.D] = (232 [+ or -] 7) [degrees]K [??] [[omega].sub.D] = 0.024 eV. (20)

This frequency is smaller than the maximum sterile neutrino energy estimated to be [T.sub.max] = 0.11 eV. Those frequency modes of interest to us are given in Table 1. The differential cross section is, therefore, given by

[mathematical expression not reproducible], (21)

where [N.sub.i] will be specified below and q is the momentum transferred to the nucleus. The momentum transfer is small and the form factor [F.sup.2]([q.sup.2]) can be neglected.

In 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 Table 1 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

[mathematical expression not reproducible]; (22)

performing the integration using the [delta] function we get

[mathematical expression not reproducible], (23)

where [T.sub.1] = (1/2)[m.sub.[nu]][[upsilon].sup.2.sub.0], y = [upsilon]/[[upsilon].sub.0]

Folding with the velocity distribution we obtain

[mathematical expression not reproducible]. (24)

We see that we have the constraint imposed by the available energy; namely,

[N.sub.k] = IP [[y.sup.2.sub.esc][T.sub.1]/[[omega].sub.k] - 1/2], (25)

where IP[x] = integer part of x. We thus find [N.sub.k] listed in Table 1. The functions [mathematical expression not reproducible] are exhibited in Figure 2. The relevant integrals are [I.sub.n]([[omega].sub.1]) = (1.170, 0.972, 0.785, 0.621) for n = 0, 1, 2, 3, [I.sub.n]([[omega].sub.2]) = (1.032, 0.609), for n = 0, 1, [I.sub.n]([[omega].sub.3]) = (1.025, 0.592), for n = 0, 1, and [I.sub.0]([[omega].sub.k]) = (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 [m.sub.t] which takes the form

R = [[PHI].sub.[nu]][C.sup.2.sub.[nu]][N.sup.2] ([g.sup.2.sub.V]) [G.sup.2.sub.F] [1/8[pi]] [[m.sub.t]/A[m.sub.p]] [m.sup.2.sub.[nu]] 17.8. (26)

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.

For a [sup.130]Te[O.sub.2] target (N = 78) of 1 kg of mass get

R = 1.7 x [10.sup.-6][C.sup.2.sub.[nu]] per kg-s = 51[C.sup.2.sub.[nu]] per kg-y (27)

This 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 x [10.sup.24]). 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 |[j.sub.1], [m.sub.1]> to a nearby level |[j.sub.2], [m.sub.2]> at energy [DELTA] = [E.sub.2] - [E.sub.1], which has the same orbital structure. The excitation energy has to be quite low; that is,

[DELTA] [less than or equal to] [1/2] [m.sub.[nu]] [[upsilon].sup.2.sub.esc] = [1/2] 50 x [10.sup.3][2.84.sup.2] [(2.2/3).sup.2] [10.sup.-6] = 0.11 eV. (28)

The target is selected so that the two levels |[j.sub.1], [m.sub.1]> and |[j.sub.2], [m.sub.2]> 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 |[j.sub.1], [m.sub.1]> is occupied by electrons but the higher one |[j.sub.2], [m.sub.2]> 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 |[j.sub.2], [m.sub.2]> to a higher state |[j.sub.3], [m.sub.3]>, 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

[mathematical expression not reproducible] (29)

(in the case of the axial current we have [g.sub.A] = 1 and we need evaluate the matrix element of [[sigma].sub.[nu]] x [[sigma].sub.e] and then square it and sum and average over the neutrino polarization).

[mathematical expression not reproducible] (30)

expressed 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

[mathematical expression not reproducible]. (31)

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 [delta] function we obtain

[mathematical expression not reproducible], (32)

where we have set E - [DELTA] = [m.sub.[nu]] + [T.sub.1] - [DELTA] [approximately equal to] [m.sub.[nu]].

Folding the cross section with the velocity distribution from a minimum [square root of ([DELTA]/[T.sub.1])] to [y.sub.esc] we obtain

[mathematical expression not reproducible]. (33)

Clearly the maximum excitation energy that can be reached is [[DELTA].sub.max] = [2.84.sup.2][T.sub.0] = 0.108 eV. The function g ([DELTA]/[T.sub.1]) is exhibited in Figure 3.

Proceeding as in Section 2 and noting that for small excitation energy g([DELTA]/[T.sub.1]) [approximately equal to] 1.4 we find

[mathematical expression not reproducible]. (34)

The expected rate will be smaller after the angular momentum factor [mathematical expression not reproducible] 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

[mathematical expression not reproducible]. (35)

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 |[j.sub.3], [m.sub.3]> mentioned above. The photon energy can be changed if the target is put in a magnetic field by a judicious choice of |[j.sub.3], [m.sub.3]>.

(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 Appendix B) 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:

[bar.[nu]] + [e.sub.b] + A(N, Z) [right arrow] A [(N + 1,Z - 1).sup.*] (36)

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 [sup.157]Tb 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 that [DELTA] is the mass difference of the two neutral atoms. Let us consider a transition to the final state with energy [E.sub.x]. 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 [upsilon] and kinetic energy [E.sub.[nu]] is given by

[mathematical expression not reproducible], (37)

where [p.sub.A] is the recoiling nucleus momentum. Integrating over the recoil momentum using the [delta] function we obtain

[mathematical expression not reproducible]. (38)

We note that since the oncoming neutrino has a mass, the excited state must be higher than the highest excited state at [E'.sub.x] = [DELTA] - b. With indicating by [epsilon] = [E.sub.x] - [E'.sub.x] the above equation can be written as

[mathematical expression not reproducible]. (39)

Folding it with the velocity distribution as above we obtain

[mathematical expression not reproducible] (40)

or using the delta function

[mathematical expression not reproducible]. (41)

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 [epsilon]. 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 [epsilon] = [m.sub.[nu]] (1 + 2.8 x [10.sup.-7]) = 50 keV + 0.014 eV and has a width [GAMMA] = [m.sub.[nu]](1 + 9.1 x [10.sup.-7]) - [m.sub.[nu]](1 + 0.32 x [10.sup.-7]) [approximately equal to] 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.

If there is a resonance in the final nucleus at the energy [E.sub.x] = [epsilon] + ([DELTA] - b) with a width [GAMMA] then perhaps it can be reached even if [epsilon] is a bit larger than [m.sub.[nu]]; for example, [epsilon] = [m.sub.[nu]] + [GAMMA]/2. The population of this resonance can be determined by measuring the energy of the deexcitation [gamma]-ray, which should exceed by [epsilon] the maximum observed in ordinary electron capture.

For antineutrinos having zero kinetic energy the atom in the final state has to have an excess energy [DELTA] - (b - [m.sub.[nu]]) 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 [DELTA]-value could be suitable for this detection. In the second case, there should exist a nuclear level that matches the energy difference [E.sub.x] = [DELTA] - (b - [m.sub.[nu]]) and therefore the incoming antineutrino has no energy threshold. Moreover, spontaneous electron capture decay is energetically forbidden, since this is allowed for [E.sub.x] < [DELTA] - (b + [m.sub.[nu]]).

As an example we consider the capture of a very low energy [bar.[nu]] by the [sup.157.sub.65]Tb nucleus:

[bar.[nu]] + [e.sup.-] + [sup.157.sub.65]Tb [right arrow] [sup.165.sub.64][Gd.sup.*] (42)

taking the allowed transitions from the ground state ([3/2.sup.+]) of parent nucleus, [sup.157.sub.65]Tb, to the first excited [5/2.sup.+] state of the daughter nucleus [sup.157.sub.64]Gd. The spin and parity of the nuclei involved obey the relations [DELTA]J = 1, [[PI].sub.f][[PI].sub.i] = +1, and the transition is dubbed as allowed. The nuclear matrix element ME can be written as

[[absolute value of (ME)].sup.2] = [([g.sub.A]/[g.sub.V]).sup.2] [<GT>.sup.2], (43)

where [g.sub.A] = 1.2695 and [g.sub.V] = 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 [[absolute value of (ME)].sup.2] = 0.96. The experimental value of first excited [5/2.sup.+] is at 64 keV [65] while that predicted by the model is at 65 keV. The [DELTA]-value is ranging from 60 to 63 keV [65].

For K-shell electron capture where [<[[phi].sup.e]>.sup.2] = [(([alpha]Z/[pi])[m.sub.e]).sup.3] (1s capture) with binding energy b = 50.24 keV, the velocity averaged cross section takes the value

<[sigma][upsilon]> = 8.98 x [10.sup.-46][C.sup.2.sub.[nu]] [cm.sup.2] (44)

and the event rate we expect for mass [m.sub.t] = 1kg is

R = 8.98 x [10.sup.-46] [C.sup.2.sub.[nu]] x 6 [10.sup.3] x 6.023 [10.sup.23] x [m.sub.t]/A x 9.28 x [10.sup.17] [y.sup.-1] = 19[C.sup.2.sub.[nu]] [y.sup.-1]. (45)

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.

6. Modification of the End Point Spectra of [beta] Decaying Nuclei

The end point spectra of [beta] decaying nuclei can be modified by the reaction involving sterile (anti)neutrinos:

[nu] + A(N,Z) [right arrow] A (N - 1,Z + 1) + [e.sup.-] (46)

or

[bar.[nu]] + A(N,Z) [right arrow] A (N + 1,Z - 1) + [e.sup.+]. (47)

This can be exploited in on ongoing experiments, for example, in the tritium decay:

[nu] + [sup.3.sub.1]H [right arrow] [sup.3.sub.2]He + [e.sup.-]. (48)

The relevant cross section is

[mathematical expression not reproducible], (49)

where [DELTA] is the atomic mass difference. Integrating over the nuclear recoil momentum and the direction of the electron momentum we get

[mathematical expression not reproducible], (50)

where

[E.sub.e] = [m.sub.[nu]] + [1/2] [m.sub.[nu]][[upsilon].sup.2] + [DELTA] + [m.sub.e], [P.sub.e] = [square root of ([E.sup.2.sub.e] - [m.sup.2.sub.e])]. (51)

Folding the cross section with the velocity distribution we find

[mathematical expression not reproducible], (52)

where

[mathematical expression not reproducible] (53)

with

y = [upsilon]/[[upsilon].sup.0]. (54)

The Fermi function, F([Z.sub.f], [E.sub.e]), encapsulates the effects of the Coulomb interaction for a given lepton energy [E.sub.e] and final state proton number [Z.sub.f]. The function f(y) is exhibited in Figure 6.

In transitions happening inside the same isospin multiplet ([J.sup.[pi]] [right arrow] [J.sup.[pi]], J [not equal to] 0) both the vector and axial form factors contribute and in this case the nuclear matrix element ME([E.sub.x]) can be written as

[[absolute value of (ME)].sup.2] = [<F>.sup.2] + [([g.sub.A]/[g.sub.V]).sup.2] [<GT>.sup.2], (55)

where [g.sub.A] = 1.2695 and [g.sub.V] = 1 are the axial and vector coupling constants, respectively. In case of [sup.3]H target we adopt [<F>.sup.2] = 0.9987 and [<GT>.sup.2] = 2.788 from [68]. Thus [[absolute value of (ME)].sup.2] = 5.49.

Thus the velocity averaged cross section takes the value

<[sigma][upsilon]> = 3.44 x [10.sup.-46] [C.sup.2.sub.[nu]] [cm.sup.2] (56)

and the expected event rate becomes

R = 3.44 x [10.sup.-46] [C.sup.2.sub.[nu]] x 6 [10.sup.3] x 6.023 [10.sup.23] x [m.sup.t]/A x 9.28 x [10.sup.17] [y.sup.-1]. (57)

For a mass of the current KATRIN target, that is, about 1 gr, we get

R = 0.380[C.sup.2.sub.[nu]] [y.sup.-1]. (58)

It is interesting to compare the neutrino capture rate

[R.sub.[nu]] = <[sigma][upsilon]> [rho]/[m.sub.[nu]] = 3.44 x [10.sup.-46] [C.sup.2.sub.[nu]] x 6 [10.sup.3] x 9.28 x [10.sup.17] = 1.91 x [10.sup.-24] [C.sup.2.sub.[nu]] [y.sup.-1] (59)

with that of beta decay process [sup.3]H [right arrow] [sup.3]He + [e.sup.-] + [[bar.[nu]].sub.j], whose rate [R.sub.[beta]] is given by

[mathematical expression not reproducible], (60)

where [W.sub.o] is the maximal electron energy or else beta decay endpoint

[W.sub.o] = [K.sub.end] + [m.sub.e] (61)

with

[mathematical expression not reproducible], (62)

the electron kinetic energy at the endpoint, and

[mathematical expression not reproducible]. (63)

Masses [mathematical expression not reproducible] and [mathematical expression not reproducible] are nuclear masses [58, 69, 70]. The calculation of (60) gives [R.sub.[beta]] = 0.055 [y.sup.-1]. The ratio of [R.sub.[nu]] to corresponding beta decay [R.sub.[beta]] is very small.

[R.sub.[nu]] = 0.034 x [10.sup.-21] [C.sup.2.sub.[nu]][R.sub.[beta]]. (64)

The situation is more optimistic in a narrow interval [W.sub.o] - [delta] < [E.sub.e] < [W.sub.o] near the endpoint. As an example, we consider an energy resolution [delta] = 0.2 eV close to the expected sensitivity of the KATRIN experiment [57]. Then the ratio of the event rate [R.sub.[beta]]([delta] = 0.2 eV) to that of neutrino capture [R.sub.[nu]] gives

[R.sub.[nu]] = 5.75 x [10.sup.-9] [C.sup.2.sub.[nu]] [R.sub.[beta]] ([delta] = 0.2 eV) . (65)

In Figure 7 we present the ratio of the event rate decay rate of [R.sub.[beta]]([delta]) for the beta decay compared with the neutrino capture rate [R.sub.[nu]] as a function of the energy resolution [delta] in the energy region [W.sub.o] - [delta] < [E.sub.e] < [W.sub.o].

Moreover, the electron kinetic energy [K.sub.e] due to neutrino capture process (48) is

[K.sub.e] = [E.sub.[nu]] + [K.sub.end] > [m.sub.[nu]] + 18.591 keV; (66)

this means that the electron in the final state has a kinetic energy of at least [m.sub.[nu]] 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 amass 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.sup.-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 [gamma] ray. Finally the sterile neutrino will lead to [nu] + A(N, Z) [right arrow] [e.sup.-] + A(N - 1, Z + 1) reaction. The produced electrons will have a maximum energy which goes beyond the end point energy of the corresponding [beta] 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 as [C.sup.2.sub.[nu]]. This parameter is not known. In neutrino oscillation experiments a value of [C.sup.2.sub.[nu]] [approximately equal to] [10.sup.-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 [C.sup.2.sub.[nu]] is not consistent, however, with a sterile 50 kev neutrino. In fact such a neutrino would have a life time [71] of 2 x [10.sup.5] 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 [C.sup.2.sub.[nu]] < 1.3 x [10.sup.-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.

https://doi.org/10.1155/2018/1479313

Appendix

A. Angular Momentum Coefficients Entering Atomic Excitations

The angular momentum coefficients entering single particle transitions are shown in (A.1) and (B.4).

Equation (A.1). The coefficients [mathematical expression not reproducible] connect via the spin operator a given initial state |i> = |nl, [j.sub.1], [m.sub.1]> with all possible states |f> = |nl, [j.sub.2], [m.sub.2]>, for l = 0, 1. Note s-states are favored.

[mathematical expression not reproducible]. (A.1)

B. Exotic Atomic Experiments

As we have mentioned the atomic experiment has to be done at low temperatures. It may be difficult to find materials exhibiting atomic structure at low temperatures. It amusing to note that one may be able to employ at low temperatures some exotic materials used in quantum technologies (for a recent review see [72]) like nitrogen-vacancy (NV), that is, materials characterized by spin S = 1, which in a magnetic field allow transitions between m = 0, m = 1 and m = -1. These states are spin symmetric. Antisymmetry requires the space part to be antisymmetric, that is, a wave function of the form

[psi] = [[phi].sup.2.sub.nl (r) [L = odd, S = 1] J = L - 1, L, L + 1. (B.1)

Of special interest are

[psi] = [[phi].sup.2.sub.nl] [(r).sup.3] [P.sub.J], [[phi].sup.2.sub.nl] [(r).sup.3] [F.sub.J]. (B.2)

Then the spin matrix element takes the form

[mathematical expression not reproducible]. (B.3)

The reduced matrix elements are given in (B.5), as well as the full matrix element [mathematical expression not reproducible] of the most important component.

Equation (B.4). The same as in equation (A.1), the coefficients [mathematical expression not reproducible] for l = 2 are

[mathematical expression not reproducible]. (B.4)

Equation (B.5). The coefficients are [mathematical expression not reproducible]. For the notation see text.

[mathematical expression not reproducible] (B.5)

Disclosure

Permanent address of John D. Vergados is as follows: University of Ioannina, 451 10 Ioannina, Greece.

Conflicts of Interest

The authors declare that they have no conflicts of interest.

Acknowledgments

The authors are indebted to Professor Marco Bernasconi for useful suggestions in connection with the phonon excitations of low temperature bolometers.

References

[1] P. Ullio and M. Kamioknowski, "Velocity distributions and annual-modulation signatures of weakly-interacting massive particles," Journal of High Energy Physics, vol. 2001, no. 03, 2001.

[2] D. Spergel, R. Bean, O. Dore et al., "Three-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Implications for Cosmology," The Astrophysical Journal Supplement Series, vol. 170, no. 2, 2007.

[3] P. A. R. Ade, M. Arnaud, and M. Ashdown, "Planck 2013 results. XXXI. Consistency of the Planck data," Astronomy & Astrophysics, vol. 571, 2014.

[4] A. Bottino, V. de Alfaro, N. Fornengo, A. Morales, J. Puimedon, and S. Scopel, "Exploring the supersymmetric parameter space by direct search for WIMPs," Physics Letters B, vol. 402, no. 1-2, pp. 113-121, 1997.

[5] R. Arnowitt and P. Nath, "Event rates in dark matter detectors for neutralinos including constraints from b->s gamma decay," Physical Review Letters, vol. 74, no. 23, pp. 4592-4595, 1995.

[6] R. Arnowitt and P. Nath, "Predictions of neutralino dark matter event rates in minimal supergravity unification," Physical Review D: Particles, Fields, Gravitation and Cosmology, vol. 54, no. 3, pp. 2374-2384, 1996.

[7] V. Bednyakov, H. Klapdor-Kleingrothaus, and S. Kovalenko, "Possible constraints on SUSY-model parameters from direct dark matter search," Physics Letters B, vol. 329, no. 1, pp. 5-9, 1994.

[8] J. Ellis and L. Roszkowski, "Supergravity dark matter," Physics Letters B, vol. 283, pp. 252-260, 1992.

[9] J. Ellis and R. A. Flores, "Elastic supersymmetric relic-nucleus scattering revisited," Physics Letters B, vol. 263, pp. 259-266, 1991.

[10] J. Ellis and R. A. Flores, "Prospects for neutralino detection with a 73Ge + 76Ge detector," Physics Letters B, vol. 300, no. 1-2, pp. 175-182, 1993.

[11] J. Ellis and R. A. Flores, "Implications of LEP on laboratory searches for dark matter neutralinos," Nuclear Physics B, vol. 400, pp. 25-36, 1993.

[12] S. Nussinov, "Some estimates of interaction in matter of neutral technibaryons made of colored constituents," Physics Letters B, vol. 279, no. 1-2, pp. 111-116, 1992.

[13] S. B. Gudnason, C. Kouvaris, and F. Sannino, "Dark matter from new technicolor theories," Physical Review D: Particles, Fields, Gravitation and Cosmology, vol. 74, Article ID 095008, 2006.

[14] R. Foot, H. Lew, and R. R. Volkas, "A model with fundamental improper spacetime symmetries," Physics Letters B, vol. 272, no. 1-2, pp. 67-70, 1991.

[15] R. Foot, "Mirror & hidden sector dark matter in the light of new CoGeNT data," Physics Letters B, vol. 703, no. 1, pp. 7-13, 2011.

[16] G. Servant and T. M. P. Tait, "Is the lightest Kaluza-Klein particle a viable dark matter candidate?" Nuclear Physics B, vol. 650, no. 1-2, pp. 391-419, 2003.

[17] V. Oikonomou, J. Vergados, and C. C. Moustakidis, "Direct detection of dark matter rates for various wimps," Nuclear Physics B, vol. 773, no. 1-2, pp. 19-42, 2007.

[18] M. W. Goodman and E. Witten, "Detectability of certain dark-matter candidates," Physical Review D: Particles, Fields, Gravitation and Cosmology, vol. 31, no. 12, pp. 3059-3063, 1985.

[19] J. Angle, E. Aprile, F. Arneodo et al., "Search for light dark matter in XENON10 data," Physical Review Letters, vol. 107, p. 051301, 2013.

[20] E. Aprile, K. Arisaka, F. Arneodo et al., "Dark matter results from 100 live days of XENON100 data," Physical Review Letters, vol. 107, p. 131302, 2011.

[21] K. Abea, J. Hosakaa, and T. Iida, "Distillation of liquid xenon to remove krypton," Astroparticle Physics, vol. 31, no. 4, pp. 290-296, 2009.

[22] C. Ghag, D. Y. Akimov, H. M. Araujo et al., "Performance of the veto detector incorporated into the ZEPLIN-III experiment," Astroparticle Physics, vol. 35, no. 2, pp. 76-86, 2011.

[23] K. Ni, Proceedings of the Dark Side of the Universe, DSU2011, Beijing, China, 2011.

[24] D. C. Malling, "After LUX: The LZ Program," https://arxiv.org/ abs/1110.0103 .

[25] D. S. Akerib and et al., "Limits on spin-dependent WIMP-nucleon interactions from the Cryogenic Dark Matter Search," Physical Review D, vol. 73, 011102, 2006.

[26] C. E. Aalseth, P. S. Barbeau, N. S. Bowden et al., "Results from a search for light-mass dark matter with a p-type point contact germanium detector," Physical Review Letters, vol. 106, p. 131301, 2011.

[27] E. Armengaud, C. Augier, A. Benoit et al., "Final results of the EDELWEISS-II WIMP search using a 4-kg array of cryogenic germanium detectors with interleaved electrodes," Physics Letters B, vol. 702, no. 5, pp. 329-335, 2011.

[28] R. Bernabei, P. Belli, F. Cappella et al., "First results from DAMA/LIBRA and the combined results with DAMA/NaI," The European Physical Journal C, vol. 56, no. 3, pp. 333-355, 2008.

[29] P. Belli, R. Bernabei, and A. Bottino, "Observations of annual modulation in direct detection of relic particles and light neutralinos," Physical Review D, vol. 84, 055014, 2011.

[30] H. S. Lee et al., "Limits on Interactions between Weakly Interacting Massive Particles and Nucleons Obtained with CsI(Tl) Crystal Detectors," Physical Review Letters, vol. 99, 091301, 2007.

[31] S. Archambault, F. Aubin, M. Auger et al., "Dark matter spin-dependent limits for WIMP interactions on 19F by PICASSO," Physics Letters B, vol. 682, no. 2, pp. 185-192, 2009.

[32] S. Archambault, F. Aubin, M. Auger et al., "New Insights into Particle Detection with Superheated Liquids," New J. Phys. volume, vol. 13, Article ID 043006, 2011.

[33] C. Arguelles, N. Mavromatos, J. Rueda, and R. Ruffini, "The role of self-interacting right-handed neutrinos in galactic structure," Journal of Cosmology and Astroparticle Physics, vol. 2016, no. 04, pp. 038-038, 2016.

[34] R. Ruffini, C. R. Arguelles, and J. A. Rueda, "On the core-halo distribution of dark matter in galaxies," Monthly Notices of the Royal Astronomical Society, vol. 451, no. 1, p. 622, 2015.

[35] R. Arguelles, R. Ruffini, and J. A. Rueda, "Novel constraints on fermionic dark matter from galactic observables," https://arxiv .org/abs/1606.07040.

[36] A. Boyarsky, O. Ruchayskiy, and M. Shaposhnikov, "The role of sterile neutrinos in cosmology and astrophysics," Annual Review of Nuclear and Particle Science, vol. 59, no. 1, pp. 359-379, 2009.

[37] A. Boyarsky, J. Lesgourgues, O. Ruchayskiy, and M. Viel, "Realistic sterile neutrino dark matter with keV mass does not contradict cosmological bounds," Physical review letters, vol. 102, 201304, 2009.

[38] E. J. Tollerud, J. S. Bullock, L. E. Strigari, and B. Willman, "Hundreds of milky way satellites? Luminosity bias in the satellite luminosity function," The Astrophysical Journal, vol. 688, no. 1, pp. 277-289, 2008.

[39] M. D. Campos and W. Rodejohann, "Testing keV sterile neutrino dark matter in future direct detection experiments," Physical Review D: Particles, Fields, Gravitation and Cosmology, vol. 94, no. 9, 2016.

[40] Y. Li, X. Z. zhong, and L. Shu, "Direct detection of the cosmic neutrino background including light sterile neutrinos," Physics Letters B, vol. 692, no. 4, 1010.

[41] Y. F. Li and Z. zhong Xing, "Captures of hot and warm sterile antineutrino dark matter on EC-decaying Ho-163 nuclei," Journal of Cosmology and Astroparticle Physics, vol. 08, p. 006, 2011.

[42] A. Giorgio, "The Waning of the WIMP? A Review of Models, Searches, and Constraints," https://arxiv.org/abs/1703.07364.

[43] W. Liao, Physical Review D, vol. 82, 073001 pages, 2010.

[44] R. Adhikari, M. Agostini, and N. Anh Ky, "A White Paper on keV sterile neutrino Dark Matter," Journal of Cosmology and Astroparticle Physics, vol. 2017, 2017.

[45] A. Aguilar-Arevalo et al., "Evidence for neutrino oscillations from the observation of [bar.[nu]]e appearance in a [bar.[nu]][mu] beam," Physical Review D, vol. 64, 112007, 2001.

[46] A. A. Aguilar-Arevalo, B. C. Brown, and L. Bugel, "Improved Search for [bar.[nu]][mu] [right arrow] [bar.[nu]]e Oscillations in the MiniBooNE Experiment," Physical Review Letters, vol. 110, 6 pages, 2013.

[47] T. Katori and J. M. Conrad, "Beyond Standard Model Searches in the MiniBooNE Experiment," Advances in High Energy Physics, vol. 2015, Article ID 362971, 19 pages, 2015.

[48] T. A. Mueller, D. Lhuillier, and M. Fallot, "Improved predictions of reactor antineutrino spectra," Physical Review C: Nuclear Physics, vol. 83, no. 5, Article ID 054615, 2011.

[49] J. N. Abdurashitov et al., "Measurement of the response of a Ga solar neutrino experiment to neutrinos from a [sup.37]Ar source," Physical Review C, vol. 73, 045805, 2006.

[50] J. Kopp, P. A. N. Machado, M. Maltoni, and T. Schwetz, "Sterile neutrino oscillations: the global picture," Journal of High Energy Physics, vol. 1305, 2013.

[51] C. Giunti, M. Laveder, Y. F. Li, and H. W. Long, "Pragmatic view of short-baseline neutrino oscillations," Physical Review D: Particles, Fields, Gravitation and Cosmology, vol. 88, no. 7, 2013.

[52] G. Mention, M. Fechner, and T. H. Lasserre, "Reactor antineutrino anomaly," Physical Review D, vol. 83, 073006, 2011.

[53] T. Asaka, S. Blanchet, and M. Shaposhnikov, "The [nu]MSM, dark matter and neutrino masses," Physics Letters B, vol. 631, no. 4, pp. 151-156, 1985.

[54] A. Kusenko, "Sterile neutrinos: The dark side of the light fermions," Physics Reports, vol. 481, no. 1-2, pp. 1-28, 2009.

[55] L. Heurtier and D. Teresi, "Dark matter and observable lepton flavor violation," Physical Review D: Particles, Fields, Gravitation and Cosmology, vol. 94, no. 12, 2016.

[56] N. E. Mavromatos and A. Pilaftsis, "Anomalous Majorana Neutrino Masses from Torsionful Quantum Gravity," Physical Review D, vol. 86, p. 124038, 2012.

[57] KATRIN collaboration, "KATRIN: A next generation tritium beta decay experiment with sub-eV sensitivity for the electron neutrino mass," https://arxiv.org/abs/hep-ex/0109033.

[58] J. Beringer et al., "Review of Particle Physics," Physical Review D, vol. 86, article 010001, Article ID 010001, 2012.

[59] Y. Hochberg, M. Pyle, Y. Zhao, and K. M. Zurek, "Detecting superlight dark matter with Fermi-degenerate materials," Journal of High Energy Physics, vol. 2016, no. 8, article no. 57, 2016.

[60] M. Ceriotti, F. Pietrucci, and M. Bernasconi, Physical Review B: Condensed Matter and Materials Physics, vol. 73, no. 10, 2006.

[61] M. Barucci, C. Brofferio, A. Giuliani, E. Gottardi, I. Peroni, and G. Ventura, "Measurement of Low Temperature Specific Heat of Crystalline TeO2 for the Optimization of Bolometric Detectors," Journal of Low Temperature Physics, vol. 123, no. 5-6, pp. 303-314, 2001.

[62] J. Vergados and Y. N. Novikov, "Prospects of detection of relic antineutrinos by resonant absorption in electron capturing nuclei," Journal of Physics G: Nuclear and Particle Physics, vol. 41, article 125001, Article ID125001, 2014.

[63] J. Toivanen and J. Suhonen, "Microscopic quasiparticle-phonon description of odd-A Xe isotopes," Journal of Physics, vol. 21, no. 11, 1995.

[64] J. Toivanen and J. Suhonen, "Microscopic quasiparticle-phonon description of odd-mass [sup.127-133]Xe isotopes and their [beta] decay," Physical Review C: Nuclear Physics, vol. 57, no. 3, pp. 1237-1245, 1998.

[65] R. G. Helmer, "Nuclear data sheets for A = 157," Nuclear Data Sheets, vol. 103, no. 4, pp. 565-782, 2004.

[66] P. E. Filianin, K. Blaum, S. A. Eliseev et al., "On the keV sterile neutrino search in electron capture," Journal of Physics G: Nuclear and Particle Physics, vol. 41, no. 9, Article ID095004, 2014.

[67] J. D. Vergados and Y. N. Novikov, "Exploring new features of neutrino oscillations with very low energy monoenergetic neutrinos," Nuclear Physics B, vol. 839, no. 1-2, pp. 1-20, 2010.

[68] R. Schiavilla, V. G. J. Stoks, and W. Glockle, "Weak capture of protons by protons," Physical Review C, vol. 58, no. 1263, 1998.

[69] G. Audi, A. Wapstra, and C. Thibault, "The Nubase evaluation of nuclear and decay properties," Nuclear Physics A, vol. 729, no. 1, pp. 3-128, 2002.

[70] J. A. Bearden and A. F. Burr, "Reevaluation of X-ray atomic energy levels," Reviews of Modern Physics, vol. 39, no. 1, pp. 125-142, 1967.

[71] A. D. Dolgov and S. H. Hansen, "Massive sterile neutrinos as warm Dark Matter," Astroparticle Physics, vol. 16, no. 3, pp. 339-344, 2002.

[72] M. W. Doherty, N. B. Manson, P. Delaney, F. Jelezko, J. Wrachtrup, and L. C. L. Hollenberg, "The nitrogen-vacancy colour centre in diamond," Physics Reports, vol. 528, no. 1, pp. 1-45, 2013.

Paraskevi C. Divari (iD) (1) and John D. Vergados (iD) (2)

(1) Department of Physical Sciences and Applications, Hellenic Army Academy, Vari, 16673 Attica, Greece

(2) TEI of Western Macedonia, 501 00 Kozani, Greece

Correspondence should be addressed to John D. Vergados; vergados@uoi.gr

Received 23 November 2017; Accepted 28 January 2018; Published 15 March 2018

Academic Editor: Athanasios Hatzikoutelis

Caption: Figure 1: The shape of the spectrum of the emitted electrons in sterile neutrino-electron scattering.

Caption: Figure 2: (a) The function [mathematical expression not reproducible], exhibited as a function of y, associated with the mode [[nu].sub.1] = 52 [cm.sup.-1] for n = 0, 1, 2, 3 increasing downwards. (b) The functions [mathematical expression not reproducible] associated with [[nu].sub.2] = 124 [cm.sup.-1] for n = 0, 1 and [mathematical expression not reproducible] for [[nu].sub.4] = 157 [cm.sup.-1], n = 0, and [mathematical expression not reproducible] for [[nu].sub.6] = 176 [cm.sup.-1], n = 0, exhibited as a function of y, for thick solid, solid, dashed, and dotted lines, respectively. For definitions see text.

Caption: Figure 3: The function g([DELTA]/[T.sub.1]) for sterile neutrino scattering by an atom as a function of the excitation energy in eV.

Caption: Figure 4: The cross section exhibits resonance behavior. Shown is the resonance properly normalized as a function of X = (1/[[upsilon].sub.0])[square root of (2([epsilon]/[m.sub.[nu]] - 1))]. The width is [GAMMA] = 1.49 and the location of the maximum is at 1.03.

Caption: Figure 5: The cross section exhibits resonance behavior. Shown is F(X) as a function of ([epsilon]/[m.sub.[nu]] - 1).

Caption: Figure 6: The shape of f(y) for the decay of [sup.3]H, where the atomic mass difference between [sup.3]H and [sup.3]He is taking [DELTA] = 18.591 keV [69].

Caption: Figure 7: Ratio of decay rates [R.sub.[nu]]/[R.sub.[beta]] (in units of [C.sup.2.sub.[nu]]) as a function of energy resolution [delta] near the endpoint.

Table 1: The frequency modes below the Debye temperature for [alpha]-Te[O.sub.2] obtained from Table VIII of [60] (for notation see text). [[nu].sub.i] = 52 124 128 152 [[omega].sub.i]/ 2[pi] ([cm.sup.-1]) Symmetry [B.sub.1] E [B.sub.1] [A.sub.1] [[omega].sub.i] (eV) 0.006 0.015 0.016 0.019 [N.sub.i] 16 6 6 5 [E.sub.max](i) (meV) 106 100 102 103 [[nu].sub.i] = 157 176 177 179 [[omega].sub.i]/ 2[pi] ([cm.sup.-1]) Symmetry [B.sub.2] [A.sub.2] E [B.sub.1] [[omega].sub.i] (eV) 0.019 0.022 0.022 0.022 [N.sub.i] 5 4 4 4 [E.sub.max](i) (meV) 107 98 99 100 Table 2: Nuclides relevant for the search of the keV sterile neutrinos in the electron capture process. We give the life time [T.sub.1/2], the Q-value, the electron binding energy [B.sub.i] for various captures, and the value of [DELTA] = Q - [B.sub.i]. For details see [66]. Nuclide [T.sub.1/2] EC transition [sup.157]Tb 71 y [3/2.sup.+] [right arrow] [3/2.sup.-] [sup.163]Ho 4570 y [7/2.sup.-] [right arrow] [5/2.sup.-] [sup.179]Ta 1.82 y [7/2.sup.+] [right arrow] [9/2.sup.+] [sup.193]Pt 50 y [1/2.sup.-] [right arrow] [3/2.sup.+] [sup.202]Pb 52 ky [0.sup.+] [right arrow] [2.sup.-] [sup.205]Pb 13 My [5/2.sup.-] [right arrow] [1/2.sup.+] [sup.235]Np 396 d [5/2.sup.+] [right arrow] [7/2.sup.-] Nuclide Q (keV) [B.sub.i] (keV) [B.sub.j] (keV) [sup.157]Tb 60.04(30) K: 50.2391(5) LI: 8.3756(5) [sup.163]Ho 2.555(16) MI: 2.0468(5) NI: 0.4163(5) [sup.179]Ta 105.6(4) K: 65.3508(6) LI: 11.2707(4) [sup.193]Pt 56.63(30) LI: 13.4185(3) MI: 3.1737(17) [sup.202]Pb 46(14) LI: 15.3467(4) MI: 3.7041(4) [sup.205]Pb 50.6(5) LI: 15.3467(4) MI: 3.7041(4) [sup.235]Np 124.2(9) K: 115.6061(16) LI: 21.7574(3) Nuclide Q - [B.sub.i] (keV) [sup.157]Tb 9.76 [sup.163]Ho 0.51 [sup.179]Ta 40.2 [sup.193]Pt 43.2 [sup.202]Pb 30.7 [sup.205]Pb 35.3 [sup.235]Np 8.6

Printer friendly Cite/link Email Feedback | |

Title Annotation: | Research Article |
---|---|

Author: | Divari, Paraskevi C.; Vergados, John D. |

Publication: | Advances in High Energy Physics |

Article Type: | Report |

Geographic Code: | 1USA |

Date: | Jan 1, 2018 |

Words: | 9172 |

Previous Article: | Search for Vector Charmonium(-Like) States in the [e.sup.+][e.sup.-] [right arrow] [eta]J/[psi] Line Shape. |

Next Article: | Composite Higgs Models after Run 2. |

Topics: |