Three-dimensional simulation of a rotating supernova

Journal Article · Fri May 02 04:00:00 EDT 2014 · AIP Conference Proceedings

DOI:https://doi.org/10.1063/1.4874084· OSTI ID:22280474

Nakamura, K. ^[1]; Kuroda, T. ^[2]; Takiwaki, T. ^[3]; Kotake, K. ^[4]

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1. Faculty of Science and Engineering, Waseda University, Ohkubo 3-4-1, Shinjuku, Tokyo 169-8555 (Japan)
2. Department of Physics, University of Basel, Klingelbergstrasse 82, 4056 Basel (Switzerland)
3. Center for Computational Astrophysics, National Astronomical Observatory of Japan, Osawa 2-21-1, Mitaka, Tokyo 181-8588 (Japan)
4. Department of Applied Physics, Fukuoka University, Jonan, Fukuoka 814-0180 (Japan)

We investigate the effects of rotation on the evolution of core-collapse supernova explosion using a 15 solar mass progenitor model with a variety of neutrino luminosity and rotational velocity. Stars should have some amount of angular momentum, which would affect stellar evolution and its final explosion. In this paper we focus on the effect of rotation on gravitational collapse of a core, on a core bounce of accreting matter, and on subsequent generation and evolution of a shock wave. We find that the rotation plays a positive role for supernova explosions. More rapidly rotating models present more rapid expansion of the shock front and more energetic explosions. When the rotational speed is moderate, the shock once stalls at about 200 km away from the center similarly to a non-rotating model. Then the rotating progenitor experiences effective neutrino heating especially around an equatorial plane and explodes even with somewhat low neutrino luminosity for which the non-rotating model cannot overcome accreting matter and finally collapses. When the rotational speed is fast, the shock expands to about 300 km immediately after the core bounce and then evolves to move outward without shock stalling. We conclude that this positive effect of rotation to explosions is dominant against some possible negative aspects, for example, lower neutrino luminosity caused by less contraction of the rotating core.

• OSTI ID: 22280474
• Journal Information: AIP Conference Proceedings, Journal Name: AIP Conference Proceedings Journal Issue: 1 Vol. 1594; ISSN APCPCS; ISSN 0094-243X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTRONOMY AND ASTROPHYSICS
ANGULAR MOMENTUM
ASTROPHYSICS
COMPUTERIZED SIMULATION
COSMIC NEUTRINOS
COSMOLOGY
GRAVITATIONAL COLLAPSE
LUMINOSITY
ROTATION
SHOCK WAVES
STAR EVOLUTION
STARS
THREE-DIMENSIONAL CALCULATIONS
VELOCITY