Web site of Supernova Neutrino Database

Abstract

This web site provides a series of numerical simulations of supernova neutrino emission from core collapse to neutron star cooling (~20 sec) for various progenitor stellar models (13-50Msolar with two different metallicities). These numerical data would be useful for various studies about supernova neutrinos, such as simulating future detections of supernova neutrino burst events by underground detectors, or predictions of relic supernova neutrino background flux. For the details of the calculation, caveats or limitation, etc., see Nakazato et al., Astrophys. J. Supp. 205 (2013) 2, arXiv:1210.6841 [astro-ph.HE]. This data set is open for general use in any research for astronomy, astrophysics, and physics, provided that our paper is referenced in your publication.
For the computations, we utilized the nuclear equation of state (EOS) constructed by Shen et al. [Prog. Theor. Phys. 100 (1998) 1013]. However, we provide also the result obtained with EOS constructed by Lattimer & Swesty [Nucl. Phys. A535 (1991) 331] for the black hole (BH) forming progenitor (30Msolar & metallicity Z = 0.004), because the neutrino signal from BH formation considerably depends on nuclear EOS. While the Lattimer & Swesty EOS has three choices with different values of incompressibility, we adopt the set with incompressibility of 220 MeV (hereafter, LS220). For the details of the neutrino emission from BH formation of LS220 model, see Nakazato et al., Astrophys. J. 804 (2015) 75, arXiv:1503.01236 [astro-ph.HE].


User's Guide (read me first)


Full Data from Core Collapse to Neutron Star Cooling Phase

MinitZSupernova modelsBH
models
trevive= 100mstrevive= 200mstrevive= 300ms
13Msolar0.02258kB257kB256kB---
20Msolar258kB257kB257kB
30Msolar257kB257kB255kB
50Msolar257kB256kB256kB
13Msolar0.004258kB257kB257kB
20Msolar258kB257kB256kB
30Msolar---4.97MB (Shen)
2.69MB (LS220)
50Msolar259kB258kB257kB---

Note: trevive is the shock revival time, which is an uncertain parameter reflecting the still unknown explosion mechanism. A black hole is formed for the 30Msolar & Z = 0.004 model, and hence trevive is not applicable.

Time Integrated Data

(The same as the above full data but giving only time integrated neutrino energy spectra.)

MinitZSupernova modelsBH
models
trevive= 100mstrevive= 200mstrevive= 300ms
13Msolar0.022.13kB2.13kB2.13kB---
20Msolar2.13kB2.13kB2.13kB
30Msolar2.13kB2.13kB2.13kB
50Msolar2.13kB2.13kB2.13kB
13Msolar0.0042.13kB2.13kB2.13kB
20Msolar2.13kB2.13kB2.13kB
30Msolar---2.13kB (Shen)
2.13kB (LS220)
50Msolar2.13kB2.13kB2.13kB---



Original Data for the Early and Late Phases

The full data are combination of the early and late phase calculations by different simulation methods, the neutrino radiation hydrodynamics (νRHD) and proto-neutron star cooling (PNSC). Here we provide the original simulation results separately for these phases, which are free from uncertainties about connecting scheme, and allowing users to combine by their own favorite connection scheme.
MinitZνRHDPNSC
trevive= 100mstrevive= 200mstrevive= 300ms
13Msolar0.021.83MB2.63MB1.68MB1.24MB
20Msolar1.67MB2.87MB2.10MB1.78MB
30Msolar2.88MB1.52MB1.16MB1.03MB
50Msolar2.48MB1.36MB1.18MB1.05MB
13Msolar0.0041.79MB2.65MB1.70MB1.36MB
20Msolar2.19MB1.43MB1.22MB1.04MB
30Msolar4.97MB (Shen)Black hole formation
2.69MB (LS220)
50Msolar2.06MB1.37MB1.18MB1.03MB



Contact


Reference

Please reference the following paper when you publish scientific articles using this database. If you use BH model with LS220 EOS, please reference also the following paper.


Last up date, May 14, 2016.