EXPLOSIVE NUCLEOSYNTHESIS IN THE NEUTRINO-DRIVEN ASPHERICAL SUPERNOVA EXPLOSION OF A NON-ROTATING 15 M{sub sun} STAR WITH SOLAR METALLICITY

Journal Article · Thu Sep 01 00:00:00 EDT 2011 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/738/1/61· OSTI ID:21582945

Fujimoto, Shin-ichiro ^[1]; Kotake, Kei ^[2]; Hashimoto, Masa-aki; Ono, Masaomi ^[3]; Ohnishi, Naofumi ^[4]

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1. Kumamoto National College of Technology, 2659-2 Suya, Goshi, Kumamoto 861-1102 (Japan)
2. Division of Theoretical Astronomy, National Astronomical Observatory Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588 (Japan)
3. Department of Physics, School of Sciences, Kyushu University, Fukuoka 810-8560 (Japan)
4. Department of Aerospace Engineering, Tohoku University, 6-6-01 Aramaki-Aza-Aoba, Aoba-ku, Sendai 980-8579 (Japan)

We investigate explosive nucleosynthesis in a non-rotating 15 M{sub sun} 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{sub sun} of the ejecta from the inner region ({<=}10, 000 km) of the precollapse core. For the models, the explosion energies and the {sup 56}Ni masses are {approx_equal} 10{sup 51}erg and (0.05-0.06) M{sub sun}, 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{sub sun} progenitor.

• OSTI ID: 21582945
• Journal Information: Astrophysical Journal, Vol. 738, Issue 1; Other Information: DOI: 10.1088/0004-637X/738/1/61; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
ELEMENT ABUNDANCE
HYDRODYNAMICS
INSTABILITY
NEUTRINOS
NEUTRON STARS
NUCLEOSYNTHESIS
SHOCK WAVES
SIMULATION
SUPERNOVAE
ABUNDANCE
BINARY STARS
ELEMENTARY PARTICLES
ERUPTIVE VARIABLE STARS
FERMIONS
FLUID MECHANICS
LEPTONS
MASSLESS PARTICLES
MECHANICS
STARS
SYNTHESIS
VARIABLE STARS