Inelastic charged current interaction of supernova neutrinos in two-phase liquid xenon dark matter detectors

Bhattacharjee, Pijushpani; Bandyopadhyay, Abhijit; Chakraborty, Sovan; Ghosh, Sayan; Kar, Kamales; Saha, S.

doi:10.48550/arxiv.2012.13986

Cited by 3 publications

(7 citation statements)

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“…The total neutron emission cross section, σ CC n,total (defined by eq. ( 22)), in units of 10 −40 cm 2 , for different neutrino energies due to νe CC interaction with 208 Pb (from [19]), 132 Xe (from [23]) and 56 Fe (from [22]). These include contributions from one-and two neutron emissions with cross sections respectively given within parentheses, (σ CC 1n , σ CC 2n ), for 208 Pb and 56 Fe.…”

Section: Resultsmentioning

confidence: 99%

“…These include contributions from one-and two neutron emissions with cross sections respectively given within parentheses, (σ CC 1n , σ CC 2n ), for 208 Pb and 56 Fe. (The 1n and 2n emission cross sections values for 132 Xe will be reported in [23].) The very small contributions from three neutron emission is neglected, so σ CC n,total ≈ σ CC 1n + 2σ CC 2n .…”

Section: Resultsmentioning

confidence: 99%

“…[22] and those for 132 Xe are from Ref. [23]. and 208 Pb, for CC interaction of the SN ν e s, for both NO and IO mass orderings.…”

Section: Resultsmentioning

confidence: 99%

“…However, such liquid xenon DM detectors, because of their low nuclear recoil thresholds, can also respond to supernova neutrinos [49,50] through the process of coherent elastic neutrino-nucleus scattering (CEνNS) [51,52]. At the same time CC and NC interactions of SN neutrinos with xenon nuclei can also result in excitation of the final state nucleus, the subsequent de-excitation of which can result in emission of neutrons which can be detected through xenon nuclear recoils caused by these neutrons [23].…”

Section: Neutron Emission From Different Detector Materialsmentioning

confidence: 99%

“…These neutrons detected in coincidence with the SN event can give valuable information about the energy spectra of the supernova neutrinos. Detectors for this purpose can in principle employ a variety of detector materials such as lead [19] (as in the HALO [20] experiment at SNOLAB), iron [21,22], liquid xenon [23], and so on. The total number of neutrons emitted due to CC interactions of ν e s with a nucleus A Z X of mass number A with Z protons and N (= A−Z) neutrons roughly scales with the "neutron excess" (= N −Z) of the nucleus.…”

Section: Introductionmentioning

confidence: 99%

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Supernova neutrino detection through neutron emission by nuclei

Bhattacharjee,

Kar

2020

Preprint

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Neutrinos from core collapse supernovae can excite nuclei of some detector materials beyond their neutron emission thresholds. Detection of these neutrons can give valuable information about the supernova explosion mechanism and possibly also throw light on neutrino properties. In this article, we give a brief review of the basic physics of neutrino induced neutron emission and describe the results of some recent calculations of supernova neutrino induced neutrons for some specific target detector materials due to charged current (CC) interactions of the electron flavored neutrinos and antineutrinos as well as due to neutral current (NC) interactions of neutrinos and antineutrinos of all flavors with the detector nuclei. We highlight the fact that a detector material such as lead with a relatively large neutron excess produces neutrons dominantly through the CC interaction of the νes, whereas a material such as iron with small neutron excess produces neutrons dominantly through the combined NC interaction of all the six neutrino and antineutrino species. This raises the interesting possibility of probing the fraction of mu-and tau flavored neutrinos (which interact only through NC interaction) in the supernova neutrino flux by means of simultaneous detection of a supernova in a lead and an iron detector, for example.

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Section: Resultsmentioning

confidence: 99%

Section: Resultsmentioning

confidence: 99%

“…[22] and those for 132 Xe are from Ref. [23]. and 208 Pb, for CC interaction of the SN ν e s, for both NO and IO mass orderings.…”

Section: Resultsmentioning

confidence: 99%

Section: Neutron Emission From Different Detector Materialsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Supernova neutrino detection through neutron emission by nuclei

Bhattacharjee,

Kar

2020

Preprint

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A next-generation liquid xenon observatory for dark matter and neutrino physics

Aalbers

AbdusSalam

Abe

et al. 2022

J. Phys. G: Nucl. Part. Phys.

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The nature of dark matter and properties of neutrinos are among the most pressing issues in contemporary particle physics. The dual-phase xenon time-projection chamber is the leading technology to cover the available parameter space for weakly interacting massive particles, while featuring extensive sensitivity to many alternative dark matter candidates. These detectors can also study neutrinos through neutrinoless double-beta decay and through a variety of astrophysical sources. A next-generation xenon-based detector will therefore be a true multi-purpose observatory to significantly advance particle physics, nuclear physics, astrophysics, solar physics, and cosmology. This review article presents the science cases for such a detector.

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Efficient estimation method for time evolution of proto-neutron star mass and radius from supernova neutrino signal

Nagakura,

Vartanyan

2021

Preprint

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In this paper we present a novel method to estimate the time evolution of proto-neutron star (PNS) structure from the neutrino signal in core-collapse supernovae (CCSN). Employing recent results of multi-dimensional CCSN simulations, we delve into a relation between total emitted neutrino energy (TONE) and PNS mass/radius, and we find that they are strongly correlated with each other. We fit the relation by simple polynomial functions connecting TONE to PNS mass and radius as a function of time. By combining another fitting function representing the correlation between TONE and cumulative number of event at each neutrino observatory, PNS mass and radius can be retrieved from purely observed neutrino data. We demonstrate retrievals of PNS mass and radius from mock data of neutrino signal, and we assess the capability of our proposed method. While underlining the limitations of the method, we also discuss the importance of the joint analysis with gravitational wave signal. This would reduce uncertainties of parameter estimations in our method, and may narrow down the possible neutrino oscillation model. The proposed method is a very easy and inexpensive computation, which will be useful in real data analysis of CCSN neutrino signal.

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Inelastic charged current interaction of supernova neutrinos in two-phase liquid xenon dark matter detectors

Cited by 3 publications

References 0 publications

Supernova neutrino detection through neutron emission by nuclei

Supernova neutrino detection through neutron emission by nuclei

A next-generation liquid xenon observatory for dark matter and neutrino physics

Efficient estimation method for time evolution of proto-neutron star mass and radius from supernova neutrino signal

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