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 (13-50M_{solar}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 (30& metallicityM_{solar}), 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].Z= 0.004

- guide.pdf (61.8kB)

- download all (5.27MB) except for BH models (
**30**&*M*_{solar})*Z*= 0.004

M_{init}ZSupernova models BH

modelst_{revive}= 100mst_{revive}= 200mst_{revive}= 300ms13 M_{solar}0.02 258kB 257kB 256kB --- 20 M_{solar}258kB 257kB 257kB 30 M_{solar}257kB 257kB 255kB 50 M_{solar}257kB 256kB 256kB 13 M_{solar}0.004 258kB 257kB 257kB 20 M_{solar}258kB 257kB 256kB 30 M_{solar}--- 4.97MB (Shen) 2.69MB (LS220) 50 M_{solar}259kB 258kB 257kB --- Note:

is the shock revival time, which is an uncertain parameter reflecting the still unknown explosion mechanism. A black hole is formed for thet_{revive}30&M_{solar}model, and henceZ= 0.004is not applicable.t_{revive}

- download all (16.5kB) except for BH model (
**30**&*M*_{solar}) with*Z*= 0.004**LS220 EOS**

M_{init}ZSupernova models BH

modelst_{revive}= 100mst_{revive}= 200mst_{revive}= 300ms13 M_{solar}0.02 2.13kB 2.13kB 2.13kB --- 20 M_{solar}2.13kB 2.13kB 2.13kB 30 M_{solar}2.13kB 2.13kB 2.13kB 50 M_{solar}2.13kB 2.13kB 2.13kB 13 M_{solar}0.004 2.13kB 2.13kB 2.13kB 20 M_{solar}2.13kB 2.13kB 2.13kB 30 M_{solar}--- 2.13kB (Shen) 2.13kB (LS220) 50 M_{solar}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.

- download all (52.6MB) except for BH model (
**30**&*M*_{solar}) with*Z*= 0.004**LS220 EOS**

M_{init}ZνRHD PNSC t_{revive}= 100mst_{revive}= 200mst_{revive}= 300ms13 M_{solar}0.02 1.83MB 2.63MB 1.68MB 1.24MB 20 M_{solar}1.67MB 2.87MB 2.10MB 1.78MB 30 M_{solar}2.88MB 1.52MB 1.16MB 1.03MB 50 M_{solar}2.48MB 1.36MB 1.18MB 1.05MB 13 M_{solar}0.004 1.79MB 2.65MB 1.70MB 1.36MB 20 M_{solar}2.19MB 1.43MB 1.22MB 1.04MB 30 M_{solar}4.97MB (Shen) Black hole formation 2.69MB (LS220) 50 M_{solar}2.06MB 1.37MB 1.18MB 1.03MB

- Ken'ichiro Nakazato
- Faculty of Arts and Science, Kyushu University
- 744 Motooka, Nishi-ku, Fukuoka 819-0395, Japan
- E-mail: nakazato@artsci.kyushu-u.ac.jp

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]

- Spectrum of the Supernova Relic Neutrino Background and Metallicity Evolution of Galaxies,

K. Nakazato, E. Mochida, Y. Niino, and H. Suzuki,

Astrophys. J. 804 (2015) 75, arXiv:1503.01236 [astro-ph.HE]

Last up date, May 14, 2016.