IMPACTS OF COLLECTIVE NEUTRINO OSCILLATIONS ON CORE-COLLAPSE SUPERNOVA EXPLOSIONS

Journal Article · Sat Sep 10 04:00:00 EDT 2011 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/738/2/165; COUNTRY OF INPUT: INTERNATIONAL ATOMIC ENERGY AGENCY (IAEA)· OSTI ID:21584876

Suwa, Yudai ^[1]; Kotake, Kei ^[2]; Takiwaki, Tomoya ^[3]; Liebendoerfer, Matthias ^[4]; Sato, Katsuhiko ^[5]

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1. Yukawa Institute for Theoretical Physics, Kyoto University, Oiwake-cho, Kitashirakawa, Sakyo-ku, Kyoto 606-8502 (Japan)
2. Division of Theoretical Astronomy, National Astronomical Observatory of Japan, Mitaka, Tokyo 181-8588 (Japan)
3. Center for Computational Astrophysics, National Astronomical Observatory of Japan, Mitaka, Tokyo 181-8588 (Japan)
4. Department of Physics, University of Basel, Klingelbergstr. 82, CH-4056 Basel (Switzerland)
5. The Institute for the Physics and Mathematics of the Universe, University of Tokyo, Kashiwa, Chiba 277-8568 (Japan)

By performing a series of one- and two-dimensional (1D and 2D) hydrodynamic simulations with spectral neutrino transport, we study possible impacts of collective neutrino oscillations on the dynamics of core-collapse supernovae. To model the spectral swapping, which is one of the possible outcome of the collective neutrino oscillations, we parameterize the onset time when the spectral swap begins, the radius where the spectral swap occurs, and the threshold energy above which the spectral interchange between heavy-lepton neutrinos and electron/anti-electron neutrinos takes place. By doing so, we systematically study how the neutrino heating enhanced by the spectral swapping could affect the shock evolution as well as the matter ejection. We also investigate the progenitor dependence using a suite of progenitor models (13, 15, 20, and 25 M{sub sun}). We find that there is a critical heating rate induced by the spectral swapping that triggers explosions, and which significantly differs between the progenitors. The critical heating rate is generally smaller for 2D than for 1D due to the multidimensionality that enhances the neutrino heating efficiency. For the progenitors employed in this paper, the final remnant masses are estimated to range between 1.1-1.5 M{sub sun}. For our 2D model of the 15 M{sub sun} progenitor, we find a set of oscillation parameters that could account for strong supernova explosions ({approx}10{sup 51} erg), simultaneously leaving behind a remnant mass close to {approx}1.4 M{sub sun}.

• OSTI ID: 21584876
• Journal Information: Astrophysical Journal, Journal Name: Astrophysical Journal Journal Issue: 2 Vol. 738; ISSN ASJOAB; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTRONOMY AND ASTROPHYSICS
BINARY STARS
ERUPTIVE VARIABLE STARS
EXPLOSIONS
FLUID MECHANICS
HYDRODYNAMICS
MASS
MECHANICS
NEUTRINO OSCILLATION
ONE-DIMENSIONAL CALCULATIONS
SIMULATION
STARS
SUPERNOVAE
TWO-DIMENSIONAL CALCULATIONS
VARIABLE STARS