TYPE IIP SUPERNOVA 2009kf: EXPLOSION DRIVEN BY BLACK HOLE ACCRETION?
- Institute of Theoretical and Experimental Physics, B. Cheremushkinskaya St. 25, 117218 Moscow (Russian Federation)
- Institute of Astronomy, RAS, Pyatnitskaya 48, 109017 Moscow (Russian Federation)
The unusually bright type IIP supernova (SN) 2009kf is studied employing hydrodynamic modeling. We derived optimal values of the ejecta mass of 28.1 M{sub sun}, explosion energy of 2.2 x 10{sup 52} erg, and presupernova radius of 2 x 10{sup 3} R{sub sun} assuming that {sup 56}Ni mass is equal to the upper limit of 0.4 M{sub sun}. We analyzed effects of the uncertainties in the extinction and {sup 56}Ni mass and concluded that both the ejecta mass and explosion energy cannot be significantly reduced compared with the optimal values. The huge explosion energy of SN 2009kf indicates that the explosion is caused by the same mechanism which operates in energetic SNe Ibc (hypernovae), i.e., via a rapid disk accretion onto black hole. The ejecta mass combined with the black hole mass and the mass lost by stellar wind yields the progenitor mass of about 36 M{sub sun}. We propose a scenario in which massive binary evolution might result in the SN 2009kf event.
- OSTI ID:
- 21452709
- Journal Information:
- Astrophysical Journal Letters, Journal Name: Astrophysical Journal Letters Journal Issue: 1 Vol. 723; ISSN 2041-8205
- Country of Publication:
- United States
- Language:
- English
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ACCRETION DISKS
BETA DECAY RADIOISOTOPES
BETA-PLUS DECAY RADIOISOTOPES
BINARY STARS
BLACK HOLES
COSMIC GAMMA BURSTS
COSMIC RADIATION
DAYS LIVING RADIOISOTOPES
ELECTRON CAPTURE RADIOISOTOPES
ERUPTIVE VARIABLE STARS
EVEN-EVEN NUCLEI
EVOLUTION
EXPLOSIONS
INTERMEDIATE MASS NUCLEI
IONIZING RADIATIONS
ISOTOPES
MASS
NICKEL 56
NICKEL ISOTOPES
NUCLEI
PRIMARY COSMIC RADIATION
RADIATIONS
RADIOISOTOPES
SIMULATION
STAR EVOLUTION
STARS
STELLAR ACTIVITY
STELLAR WINDS
SUPERNOVAE
VARIABLE STARS