TY - JOUR
T1 - Explosive nucleosynthesis in the neutrino-driven aspherical supernova explosion of a non-rotating 15 M ∞ star with solar metallicity
AU - Fujimoto, Shin Ichiro
AU - Kotake, Kei
AU - Hashimoto, Masa Aki
AU - Ono, Masaomi
AU - Ohnishi, Naofumi
PY - 2011/9/1
Y1 - 2011/9/1
N2 - We investigate explosive nucleosynthesis in a non-rotating 15 M ∞ star with solar metallicity that explodes by a neutrino-heating supernova (SN) mechanism aided by both standing accretion shock instability (SASI) and convection. To trigger explosions in our two-dimensional hydrodynamic simulations, we approximate the neutrino transport with a simple light-bulb scheme and systematically change the neutrino fluxes emitted from the protoneutron star. By a post-processing calculation, we evaluate abundances and masses of the SN ejecta for nuclei with a mass number ≤70, employing a large nuclear reaction network. Aspherical abundance distributions, which are observed in nearby core-collapse SN remnants, are obtained for the non-rotating spherically symmetric progenitor, due to the growth of a low-mode SASI. The abundance pattern of the SN ejecta is similar to that of the solar system for models whose masses range between (0.4-0.5) M ∞ of the ejecta from the inner region (≤10, 000 km) of the precollapse core. For the models, the explosion energies and the 56Ni masses are ≃ 10 51erg and (0.05-0.06) M ∞, respectively; their estimated baryonic masses of the neutron star are comparable to the ones observed in neutron-star binaries. These findings may have little uncertainty because most of the ejecta is composed of matter that is heated via the shock wave and has relatively definite abundances. The abundance ratios for Ne, Mg, Si, and Fe observed in the Cygnus loop are reproduced well with the SN ejecta from an inner region of the 15 M ∞ progenitor.
AB - We investigate explosive nucleosynthesis in a non-rotating 15 M ∞ star with solar metallicity that explodes by a neutrino-heating supernova (SN) mechanism aided by both standing accretion shock instability (SASI) and convection. To trigger explosions in our two-dimensional hydrodynamic simulations, we approximate the neutrino transport with a simple light-bulb scheme and systematically change the neutrino fluxes emitted from the protoneutron star. By a post-processing calculation, we evaluate abundances and masses of the SN ejecta for nuclei with a mass number ≤70, employing a large nuclear reaction network. Aspherical abundance distributions, which are observed in nearby core-collapse SN remnants, are obtained for the non-rotating spherically symmetric progenitor, due to the growth of a low-mode SASI. The abundance pattern of the SN ejecta is similar to that of the solar system for models whose masses range between (0.4-0.5) M ∞ of the ejecta from the inner region (≤10, 000 km) of the precollapse core. For the models, the explosion energies and the 56Ni masses are ≃ 10 51erg and (0.05-0.06) M ∞, respectively; their estimated baryonic masses of the neutron star are comparable to the ones observed in neutron-star binaries. These findings may have little uncertainty because most of the ejecta is composed of matter that is heated via the shock wave and has relatively definite abundances. The abundance ratios for Ne, Mg, Si, and Fe observed in the Cygnus loop are reproduced well with the SN ejecta from an inner region of the 15 M ∞ progenitor.
KW - hydrodynamics
KW - methods: numerical
KW - nuclear reactions, nucleosynthesis, abundances
KW - supernovae: general
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U2 - 10.1088/0004-637X/738/1/61
DO - 10.1088/0004-637X/738/1/61
M3 - Article
AN - SCOPUS:80052766044
VL - 738
JO - Astrophysical Journal
JF - Astrophysical Journal
SN - 0004-637X
IS - 1
M1 - 61
ER -