The Luminous and Carbon-rich Supernova 2006gz: A Double Degenerate Merger?
M. HickenHarvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138P. GarnavichDepartment of Physics, University of Notre Dame, Notre Dame, IN 46556J. L. PrietoDepartment of Astronomy, The Ohio State University, Columbus, OH 43210S. BlondinHarvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138D. L. DePoyDepartment of Astronomy, The Ohio State University, Columbus, OH 43210R. KirshnerHarvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138J. ParrentDepartment of Physics and Astronomy, University of Oklahoma, Norman, OK 73019
2007en
ABI
Аннотация
Spectra and light curves of SN 2006gz show the strongest signature of unburned carbon and one of the slowest fading light curves ever seen in a type Ia event (Delta m_15 = 0.69 +/- 0.04). The early-time Si II velocity is low, implying it was slowed by an envelope of unburned material. Our best estimate of the luminosity implies M_V = -19.74 and the production of ~ 1.2 M_sun of 56Ni. This suggests a super-Chandrasekhar mass progenitor. A double degenerate merger is consistent with these observations.
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