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 (13-50M_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.

User's Guide (read me first)

• guide.pdf (59.0kB)

Full Data from Core Collapse to Neutron Star Cooling Phase

• download all (5.27MB) except for BH models (30M_solar & Z = 0.004)

Minit	Z	Supernova models			BH models
		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)
					4.01MB (Togashi)
					2.69MB (LS220)
50Msolar		259kB	258kB	257kB	---

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

Time Integrated Data

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

• download all (16.5kB) except for BH models (30M_solar & Z = 0.004) with Togashi EOS and LS220 EOS

Minit	Z	Supernova models			BH models
		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 (Togashi)
					2.13kB (LS220)
50Msolar		2.13kB	2.13kB	2.13kB	---

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.

• download all (52.6MB) except for BH models (30M_solar & Z = 0.004) with Togashi EOS and LS220 EOS

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
		4.01MB (Togashi)
		2.69MB (LS220)
50Msolar		2.06MB	1.37MB	1.18MB	1.03MB

Contact

• 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

Reference

Please reference the following paper when you publish scientific articles using this database.

• 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]

If you use BH models with Togashi EOS and LS220 EOS, please reference also the following paper.

• Numerical Study of Stellar Core Collapse and Neutrino Emission Using the Nuclear Equation of State Obtained by the Variational Method,
  K. Nakazato, K. Sumiyoshi, and H. Togashi,
  Publ. Astron. Soc. Jpn. 73 (2021) 639-651, arXiv:2103.14386 [astro-ph.HE]