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].
Minit Z Supernova models BH
trevive= 100ms trevive= 200ms trevive= 300ms 13Msolar 0.02 258kB 257kB 256kB --- 20Msolar 258kB 257kB 257kB 30Msolar 257kB 257kB 255kB 50Msolar 257kB 256kB 256kB 13Msolar 0.004 258kB 257kB 257kB 20Msolar 258kB 257kB 256kB 30Msolar --- 4.97MB (Shen) 2.69MB (LS220) 50Msolar 259kB 258kB 257kB ---
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.
Minit Z Supernova models BH
trevive= 100ms trevive= 200ms trevive= 300ms 13Msolar 0.02 2.13kB 2.13kB 2.13kB --- 20Msolar 2.13kB 2.13kB 2.13kB 30Msolar 2.13kB 2.13kB 2.13kB 50Msolar 2.13kB 2.13kB 2.13kB 13Msolar 0.004 2.13kB 2.13kB 2.13kB 20Msolar 2.13kB 2.13kB 2.13kB 30Msolar --- 2.13kB (Shen) 2.13kB (LS220) 50Msolar 2.13kB 2.13kB 2.13kB ---
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.
Minit Z νRHD PNSC trevive= 100ms trevive= 200ms trevive= 300ms 13Msolar 0.02 1.83MB 2.63MB 1.68MB 1.24MB 20Msolar 1.67MB 2.87MB 2.10MB 1.78MB 30Msolar 2.88MB 1.52MB 1.16MB 1.03MB 50Msolar 2.48MB 1.36MB 1.18MB 1.05MB 13Msolar 0.004 1.79MB 2.65MB 1.70MB 1.36MB 20Msolar 2.19MB 1.43MB 1.22MB 1.04MB 30Msolar 4.97MB (Shen) Black hole formation 2.69MB (LS220) 50Msolar 2.06MB 1.37MB 1.18MB 1.03MB
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.
- Supernova Neutrino Light Curves and Spectra for Various Progenitor Stars: From Core Collapse to Proto-neutron Star Cooling,
K. Nakazato, K. Sumiyoshi, H. Suzuki, T. Totani, H. Umeda, and S. Yamada,
Astrophys. J. Supp. 205 (2013) 2, arXiv:1210.6841 [astro-ph.HE]