Total cross sections
Even though the combined laboratory, astrophysical and cosmological evidence implies that neutrinos have masses, neutrinos provide only a small cosmic dark matter component. The study of solar neutrinos provides important information on nuclear processes inside the Sun as well as on matter densities. Moreover, supernova neutrinos provide sensitive probes for studying supernova explosions, neutrino properties and stellar collapse mechanisms. Neutrino-nucleus reactions at energies below 100 MeV play essential roles in core-collapse supernovae, explosive and r-process nucleosynthesis, as well as observation of solar and supernova neutrinos by earthbound detectors. On the other hand, recent experimental data of high-energy extragalactic neutrinos at 1 PeV open a new window to probe non-standard neutrino properties, such as resonant effects in the oscillation probability.
- neutrino physics
- neutrino oscillations
- charge current neutrino-nucleus scattering
- dark matter
- sterile neutrino
Neutrinos play a fundamental role in cosmology and astrophysics, two rapidly progressing fields. The origin of neutrino masses and the nature of dark matter (DM) are two most pressing open questions in modern astro-particle physics. We know from the observation of neutrino oscillations that neutrinos have masses [1, 2]. The smallness of neutrino masses relative to those of the standard model (SM) charged fermions remains a puzzle. The effect of small neutrino masses may be probed in precision cosmic microwave background (CMB) radiation observations [3–10] as well as large-scale galaxy surveys [11–13]. The absolute scale of neutrino mass may also affect the long-standing issue of cosmic structure formation. Furthermore, neutrinos govern big-bang nucleosynthesis so that neutrino properties can be inferred from the observed light-element abundances [14–16]. Massive neutrinos may also be responsible to account for the mystery of the matter to anti-matter asymmetry in the Universe. Finally, core-collapse supernovae are powerful ‘laboratories’ to probe neutrino properties if in the future one were to observe a high-statistics neutrino signal. For example, a stellar core collapse in the Milky Way satellite galaxies may produce an enormous burst of neutrinos ‘visible’ by terrestrial detectors. Such an effect will carry important information in astrophysics, cosmology and particle physics [17, 18]. In addition, dedicated experiments are now planned involving intense accelerator-produced neutrino beams to study neutrino properties over long baselines. These will traverse the mantle or/and core of the Earth  so that the interpretation of the results will require geophysical details [20, 21].
Neutrinos could be key particles to unravel the nature of the DM in the Universe. The dark matter problem has been a long-standing one in physics [22, 23]. Even though we know that it must exist [24–27], we do not know much about its true nature. It is clear, though, that massive neutrinos and dark matter are both part of nature and should be incorporated in models of physics beyond the standard model. It may be that they are related to each other  and that, in addition, both originate from new physics at the TeV scale.
Several studies have noted that the existence of light sterile neutrinos would have important consequences for dark matter searches . Moreover, MSW-enhanced transitions between active and sterile neutrinos would have a substantial impact on searches for neutrinos from dark matter annihilation in the Sun [30, 31]. Furthermore, if sterile neutrinos in addition to their mixing with the active neutrinos possess some new gauge interactions, they could lead to signals which appear to favour a dark matter interpretation. These can be used to investigate sterile states and may also generate strong signals in DM detectors [32–34]. Couplings between neutrino, either active or sterile, and dark matter have been studied in many different contexts [35–46].
Understanding the explosion of supernovae or the physics of the early universe, where neutrinos play an essential role, requires a solid theoretical background in astrophysics and cosmology and reliable input from nuclear physics. Neutrino-nucleus scattering at energies below 100 MeV plays an essential role in core-collapse supernova simulations in various interactions of neutrinos with the supernova environment. Based on the improved supernova simulations, it is found that inelastic neutrino-nucleus reactions will also allow for an additional mode of energy deposition to the matter ahead of the shock wave in the post-shock explosion phase, supporting the shock propagation.
A call for reliable neutrino-nucleus cross sections has also been made in the context of explosive nucleosynthesis, occurring when the shock wave passes through the exploding star and leads to fast nuclear reactions. It has also been pointed out that neutrino-induced reactions in the outer layers of the star can actually be the major source for the production of certain nuclides in nature. This is the so-called
Recently, the IceCube Collaboration has reported the detection of ultra-high energy (UHE) neutrino events coming from extraterrestrial sources, that is, neutrinos with energies in the range TeV–PeV [59–61]. The most plausible sources that these events are connected are from unique high-energy cosmic ray accelerators like semi-relativistic hypernova remnants (HNRs) [62–64], and remnants from gamma ray bursts in star-burst galaxies, which can produce primary cosmic rays with the required energies and abundance . Neutrino interactions with DM could have strong implications at cosmological scales, such as reduction of the relic neutrino density, modification of the CMB spectra  or even a connection between the smallness of neutrino mass and a MeV-mass scalar field DM . Many DM candidates have been proposed in this context: heavy neutrinos as dark matter, lightest supersymmetric particles (LSP) and MeV-mass scalar field. Furthermore, sterile neutrinos appear in models attempting to explain the dark matter problem either as the main component for the dark matter content or as an additional subleading component of a multiparticle dark matter model. Those particles interact with matter through mixing with the active neutrino states. If there is a mixing between active and sterile neutrinos, UHE neutrinos interacting with dark matter may experience an enhancement in the oscillation probability when they propagate in a DM medium. This is a mechanism that could be tested from future UHE experimental data.
The chapter has been organized as follows. In Section 2, we outline the basic formalism used in the evaluation of neutrino-nucleus cross sections. Section 3 presents original cross section calculations for charged current (CC) neutrino and antineutrino scattering off targets from 12C to 208Pb, at energies below 100 MeV. Illustrative test calculations are performed for CC (anti)neutrino reactions on 56Fe and 40Ar, and the results are compared with other previous theoretical studies. Such cross section calculations provide us with significant information regarding the range of efficiency of these isotopes in low-energy neutrino searches. The event estimates are made by convolving the calculated cross sections with two different distributions: the Fermi-Dirac (FD) flux and the Livermore one. In Section 4, results are presented concerning the interaction potential of extragalactic neutrinos, at ultra-high energies, with dark matter, which might induce resonant effects in the oscillation survival probability. Finally, in Section 5, the main conclusions extracted from the present work are summarized.
2. Charge current neutrino-nucleus cross-section formalism
Let us consider a neutrino-nucleus interaction in which a low or intermediate energy neutrino (or antineutrino) is scattered inelastically from a nucleus (
The standard model effective Hamiltonian in a charge current interaction can be written as:
Here, denotes the Fermi weak coupling constant and is the Cabibbo angle. According to V-A theory, the leptonic current takes the form:
where, are the neutrino/antineutrino spinors. The hadronic current of vector, axial-vector and pseudo-scalar components is written as:
(stands for the nucleon mass and denotes the nucleon spinors). By the conservation of the vector current (CVC), the vector form factors can be written in terms of the proton and neutron electromagnetic form factors . The axial-vector form factor is assumed to be of dipole form :
where GeV is the axial cut-off mass and is the static value (at ) of the axial form factor. Recently, it has been shown in modelling the
where MeV represents the mass of the charged pion. The strangeness contributions are not taken into account since the energy region considered here is below the quasi-elastic region where the contributions from strangeness can be neglected .
In the convention we used in the present work , the square of the four-momentum transfer is written as:
where is the excitation energy of the nucleus. denotes the energy of the incoming lepton and that of the outgoing lepton. and
The neutrino/antineutrino-nucleus differential cross section, after applying a multipole analysis of the weak hadronic current, is written as:
The contributions of and are written as:
where , and . In Eq. (9), the (−) sign corresponds to neutrino scattering and the (+) sign to antineutrino. The absolute value of the three-momentum transfer is given by:
For charge current (CC) reactions, the cross section of Eq. (7) must be corrected for the distortion of the outgoing lepton wave function by the Coulomb field of the daughter nucleus  and references therein.
3. Original cross sections
Development of large mass detectors for low energy neutrinos and dark matter may allow supernova detection via neutrino-nucleus scattering (elastic or inelastic). An analysis of the events observed by these detectors requires a detailed calculation of the interaction cross sections of neutrinos with the detector material. Especially interesting is modelling the reaction cross sections of neutrinos scattering on nuclei that can be used as targets for SN neutrino detectors. The target materials include a range of isotopes from 4He to 208Pb. In this chapter, we report results concerning the cross sections of charge current (CC) (anti)neutrino-nucleus reactions for some isotopes of astrophysical interest. The results refer to the target isotopes 12C, 16O, 18O, 40Ar, 56Fe, 114Cd, 116Cd, 132Xe and 208Pb. The nuclear matrix elements entering in Eqs. (8) and (9) have been calculated in the framework of pnQRPA [73–75]. The respective cross sections are listed in Tables 1 and 2 for various incoming (anti)neutrino energies
Charge current interactions proceed through interaction of
An important application of microscopic models of neutrino-nucleus reactions is the calculation of cross sections for supernova neutrinos. Thus, in order to estimate the response of a nucleus to a specific source of neutrinos, the calculated cross sections given in Tables 1 and 2 must be folded with a specific supernova neutrino energy distribution. The neutrino spectrum of a core-collapse supernova is believed to be similar to a Fermi-Dirac (FD) spectrum, with temperatures in the range 3–8 MeV . The FD energy distribution is given by:
Some characteristic values of are listed in Table 4 .
|T = 3.5MeV||T = 5MeV||T = 8MeV|
For a connection of the present theoretical results with the neutrino experiments and the neutrino sources, we carry out the folding (convolution) of the calculated cross sections given in Tables 1 and 2 with the distribution and estimate the response of the given isotopes to the corresponding spectrum. These responses (signals to the detector) are evaluated by:
We close this subsection by exploiting our predictions of total cross sections to estimate the number of expected electron (anti)neutrino events in a detector. For current detectors , typical event yields are a few hundred events per kt of detector material for a core-collapse event at
Two examples of supernova models are used to predict the neutrino flux: (i) the model based on the FD distribution with a single temperature (3.5 MeV for neutrinos and 5 MeV for antineutrinos) and zero chemical parameter (
If the mass of the target material is
where is the total cross section (see Tables 1 and 2 ). Figure 5 shows the event rates in 1 kt of the target material for the Livermore model. The total number of events per kiloton for each of the two neutrino fluxes are listed in Table 5 . The actual detected number of events may be significantly fewer, if the detector energy threshold, detector efficiency and other background contamination effects coming from radioactive isotopes are taken into account. The results show that there is no considerable variation in the total antineutrino events between the two supernova models used in the calculation.
4. Interaction of neutrinos with dark matter
Dark matter particles (hereafter generically denoted by
If there is a mixing between active and sterile neutrinos, high-energy neutrinos interacting with dark matter may suffer a kind of MSW effect when they propagate in a dark matter medium. In a simplified model, which includes ordinary and dark matter potentials, the evolution equation with one sterile
It is interesting to compute the survival probability for active neutrinos for various values of . Figure 6 depicts
where the parameters
The study of neutrino scattering with nuclei provides the most attractive mechanism to detect or distinguish neutrinos of different flavour and to investigate the basic structure of weak interactions. Further studies involving neutrino-induced transitions between discrete nuclear states may help us to explore the structure of the weak hadronic currents and also constitute good sources of explanation for neutrino properties.
Neutrino-induced reactions are of particular significance in view of studies on modern detectors, based on neutrino scattering on various isotopes. So far, experimental neutrino cross sections are not available for modest energies below 100 MeV, with the exception of 12C and, with large uncertainty, 56Fe. These are rather important for astrophysical and cosmological applications and must be calculated. In this chapter, we have presented neutrino(antineutrino)-nucleus reactions via charge current related to a range of targets from 12C to 208Pb. The calculated cross sections are tabulated for a set of neutrino energies which are relevant for supernova neutrinos. The rather low neutrino energies involved introduce, however, some sensitivity to nuclear structure effects and, in particular, for neutrinos with energies lower than 20 MeV, where state-of-the-art nuclear models must be employed which describe the many-body correlations in the nucleus accurately. The model of choice is the pnQRPA yielding to reasonable cross sections in a wide range of nuclear isotopes. The nuclear responses of these isotopes (used in common detector materials) to supernova neutrinos have been studied for two neutrino flux models. The two-parameter Fermi-Dirac neutrino energy model with zero chemical potential and the Livermore model assuming Fermi-Dirac spectra with average neutrino energies indicated as a function of time integrated over 14 seconds burst. The expected number of events per kt are predicted for supernova-detector distance 10 kpc. The results show that there is no considerable variation in the total antineutrino events between the two supernova models used in the calculation.
Furthermore, we also present results concerning the interaction potential of extragalactic neutrinos, at high energies 1 PeV, with DM in the presence of sterile neutrino state. High-energy neutrinos interacting with DM may suffer a kind of MSW effect when propagating in DM medium. The resonance effect happens at around 0.4–0.6 PeV for various density DM profiles. The existence of light sterile neutrinos can impact existing and future dark matter searches. The mechanism of MSW effect in the UHE neutrino survival probability may be tested in future experimental searches using experimental data, for instance, as those taken from IceCube operation.