SNEWPY: A Data Pipeline from Supernova Simulations to Neutrino Signals

Baxter, A.; BenZvi, S.; Jaimes, Joahan Castaneda; Coleiro, A.; Molla, Marta Colomer; Dornic, D.; Goldhagen, Tomer; Graf, Anne M.; Griswold, Spencer; Habig, A.; Hill, R.; Lang, Shunsaku Horiuchi James P. Kneller Rafael F.; Lincetto, Massimiliano; Migenda, J.; Nakamura, Kazuhiko; O’Connor, Evan; Renshaw, Andrew A.; Scholberg, K.; Uberoi, Navya; Worlikar, Arkin

doi:10.48550/arxiv.2109.08188

Cited by 2 publications

(2 citation statements)

References 48 publications

(62 reference statements)

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“…For this, we extract from the Monte Carlo data, in 0.1 ms time bins, the luminosity, average energy, and root mean squared energy for each neutrino species in a 30 ms time window around black hole formation, starting ∼7 ms before and continuing ∼23 ms after black hole formation. With these quantities, we use SNEWPY (Baxter et al 2021) and SNOwGLoBES (Scholberg et al 2021) to estimate the interaction rate of our model for two currently operating detectors, a Super-K-like, 32 kT water Cherenkov detector (Fukuda et al 2003) and an IceCube-like, longstring water Cherenkov detector (Abbasi et al 2011). We also include three future detectors: a JUNO-like, 20 kT liquid scintillator detector (An et al 2016); a Hyper-K-like, 220 kT water Cherenkov detector (Abe et al 2018); and a DUNE-like, 40 kT liquid argon detector (Abi et al 2020(Abi et al , 2021.…”

Section: Detection Estimates For Neutrino Echos From Failed Ccsnementioning

confidence: 99%

Neutrino Echos following Black Hole Formation in Core-Collapse Supernovae

Gullin,

O'Connor,

Wang

et al. 2021

Preprint

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During a failed core-collapse supernova, the protoneutron star eventually collapses under its own gravitational field and forms a black hole. This collapse happens quickly, on the dynamical time of the protoneutron star, 0.5 ms. During this collapse, barring any excessive rotation, the entire protoneutron star is accreted into the newly formed black hole. The main source of neutrinos is now removed and the signal abruptly shuts off over this formation timescale. However, while the source of neutrinos is turned off, the arrival times at an Earth-based detector will depend on the neutrino path. We show here that a modest amount of neutrinos, emitted just prior to the black hole forming, scatter on the infalling material into our line of sight and arrive after the formation of the black hole, up to 15 ms in our model. This neutrino echo, which we characterize with Monte Carlo simulations and analytic models, has a significantly higher average energy (upwards of ∼ 50 MeV) compared to the main neutrino signal, and for the canonical failed supernova explored here, is likely detectable in O(10 kT) supernova neutrino detectors for Galactic failed supernovae. The presence of this signal is important to consider if using black hole formation as a time post for triangulation or the post black hole timing profile for neutrino mass measurements. On its own, it can also be used to characterize or constrain the structure and nature of the accretion flow.

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Section: Detection Estimates For Neutrino Echos From Failed Ccsnementioning

confidence: 99%

Neutrino Echos following Black Hole Formation in Core-Collapse Supernovae

Gullin,

O'Connor,

Wang

et al. 2021

Preprint

Self Cite

View full text Add to dashboard Cite

show abstract

“…It should also be mentioned that neutrino detections through neutral current reactions have sensitivity to all flavor of neutrinos, although they are subdominant channels in detectors considered in this paper. On the other hand, there are many currently operating or future planed neutrino detectors that utilize nuclear neutral-current interactions (such as coherent elastic neutrino nucleus scattering) (Chakraborty et al 2014;Aalbers et al 2016;Lang et al 2016;Bandyopadhyay et al 2017;Abe et al 2017;Bhattacharjee et al 2020;Pattavina et al 2020;DarkSide-20k Collaboration et al 2021;Pattavina et al 2021;Akimov et al 2021;Baxter et al 2021). If TONE can be estimated from these detectors, our fitting formula (Eqs.…”

Section: Limitationsmentioning

confidence: 99%

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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SNEWPY: A Data Pipeline from Supernova Simulations to Neutrino Signals

Cited by 2 publications

References 48 publications

Neutrino Echos following Black Hole Formation in Core-Collapse Supernovae

Neutrino Echos following Black Hole Formation in Core-Collapse Supernovae

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

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