2010/09/23 by В. П. Утробин, V. P. Utrobin, Н. Н. Чугай +2
Physics and Astronomy · #Accretion (finance) #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Black hole (networking) #Ejecta #Gamma-ray bursts and supernovae #Hypernova #Mass ratio #Physics #Pulsars and Gravitational Waves Research #RADIUS #Supernova #astro-ph.SR
paper · pdf · doi:10.1088/2041-8205/723/1/l89
14 pages, 4 figures, 1 table, accepted for publication in ApJ Letters
arxiv created 2010/09/23 · openalex publication_date 2010/10/13 · arxiv updated 2015/05/20 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
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 ☉ , explosion energy of 2.2 × 10 52 erg, and presupernova radius of 2 × 10 3 R ☉ assuming that 56 Ni mass is equal to the upper limit of 0.4 M ☉ . We analyzed effects of the uncertainties in the extinction and 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 ☉ . We propose a scenario in which massive binary evolution might result in the SN 2009kf event.