Evan O'Connor and Christian D. Ott, The Astrophysical Journal 762 126 (2013) ApJ link ads
Abstract
We perform spherically-symmetric general-relativistic simulations of core collapse and the postbounce preexplosion phase in 32 presupernova stellar models of solar metallicity with zero-age-main-sequence masses of 12 M_{sun} to 120 M_{sun}. Using energy-dependent three-species neutrino transport in the two-moment approximation with an analytic closure, we show that the emitted neutrino luminosities and spectra follow very systematic trends that are correlated with the compactness (~M/R) of the progenitor star's inner regions via the accretion rate in the preexplosion phase. We find that these qualitative trends depend only weakly on the nuclear equation of state, but quantitative observational statements will require independent constraints on the equation of state and the rotation rate of the core as well as a more complete understanding of neutrino oscillations. We investigate the simulated response of water Cherenkov detectors to the electron antineutrino fluxes from our models and find that the large statistics of a galactic core collapse event may allow robust conclusions on the inner structure of the progenitor star. |
Here we provide the numerical results of this paper. Should you have comments, questions, or requests for additional data, or if you find something peculiar, please contact Evan O'Connor (evanoc #at# tapir.caltech.edu).
SNOwGLObES fluency data for 5ms bins
We provide SNOwGLObES fluency data in 5ms bins for each progenitor model (32 in total) and equation of state (LS220 and HShen). The unoscillated fluxes are for a supernova located at 10kpc. There are specific files for each models, EOS, and time snapshot starting at 20ms prebounce and going to 450ms post bounce, in intervals of 5ms, totaling 2*32*104=6656 files. These are tarred and gzipped into two files, one for each EOS. The format for each file is:
<energy (in GeV)> <nu_e fluence (#/cm^2)> <nu_x fluence (#/cm^2)> <nu_x fluence (#/cm^2)> <anu_e fluence (#/cm^2)> <nu_x fluence (#/cm^2)> <nu_x fluence (#/cm^2)>
The nu_x luminosity is L_nux = L_nu_mu = L_anu_mu = L_nu_tau = L_anu_tau. We note that these luminosities are for the preexplosion phase only. The simulations did not explode.
LS220_datafiles.tar.gz
HShen_datafiles.tar.gz
Luminosities and average energies in 1ms bins
Here we provide the luminosity, average energy, and rms energy of all species, for all models and EOS in 1ms intervals up to 500ms, totaling 2*32=64 files. These are tarred and gzipped into two files, one for each EOS. The format is:
<postbounce time (s)> <nu_e luminosity (ergs/s)> <anu_e luminosity (ergs/s)> <nu_x luminosity (ergs/s)> <nu_e average energy (MeV)> <anu_e average energy (MeV)> <nu_x average energy (MeV)> <nu_e rms energy (MeV)> <anu_e rms energy (MeV)> <nu_x rms energy (MeV)>
The nu_x luminosity is L_nux = L_nu_mu = L_anu_mu = L_nu_tau = L_anu_tau. We note that these neutrino signals are for the preexplosion phase only. The simulations did not explode.
LS220_timeseries.tar.gz
HShen_timeseries.tar.gz
Spectra in 1ms bins
Here we provide the full spectra of all species, for all models and EOS in 1ms intervals up to 500ms, totaling 2*32=64 files. These are tarred and gzipped into two files, one for each EOS. The format is:
<postbounce time 1 (s)>
<Energy (MeV)> <nu_e flux (#/cm^2/s/MeV)> <anu_e flux(#/cm^2/s/MeV)> <nu_x flux(#/cm^2/s/MeV)>
(remaining energies)...
<postbounce time 2 (s)>
<Energy (MeV)> <nu_e flux (#/cm^2/s/MeV)> <anu_e flux(#/cm^2/s/MeV)> <nu_x flux(#/cm^2/s/MeV)>
(remaining energies)...
(remaining times)...
The nu_x luminosity is L_nux = L_nu_mu + L_anu_mu + L_nu_tau + L_anu_tau. We note that these neutrino signals are for the preexplosion phase only. The simulations did not explode.
LS220_timeseries_spectra.tar.gz
HShen_timeseries_spectra.tar.gz