期刊
ASTROPHYSICAL JOURNAL
卷 852, 期 2, 页码 -出版社
IOP PUBLISHING LTD
DOI: 10.3847/1538-4357/aa9e4c
关键词
nuclear reactions, nucleosynthesis, abundances; supernovae: individual (SN 2014J)
资金
- NASA [NAS5-26555]
- NASA Office of Space Science [NNX09AF08G]
- NSF [AST-0708873]
- Mitchell Postdoctoral Fellowship
- NASA/STScI [HST-GO-13717.001-A, HST-GO-14139.001-A, HST-GO-14663.001-A]
- Benoziyo Prize Postdoctoral Fellowship
- Royal Society University Research Fellowship
- Chinese Academy of Sciences [XDB09000000]
- Major State Basic Research Development Program [2013CB834903]
- National Natural Science Foundation of China (NSFC) [11178003, 11325313]
The very nearby Type Ia supernova 2014J in M82 offers a rare opportunity to study the physics of thermonuclear supernovae at extremely late phases (greater than or similar to 800 days). Using the Hubble Space Telescope, we obtained 6 epochs of high-precision photometry for SN 2014J from 277 days to 1181 days past the B-band maximum light. The reprocessing of electrons and X-rays emitted by the radioactive decay chain Co-57 -> Fe-57 is needed to explain the significant flattening of both the F606W-band and the pseudo-bolometric light curves. The flattening confirms previous predictions that the late-time evolution of type Ia supernova luminosities requires additional energy input from the decay of Co-57. By assuming the F606W-band luminosity scales with the bolometric luminosity at similar to 500 days after the B-band maximum light, a mass ratio Ni-57/Ni-56 similar to 0.065(-0.005)(+0.004) is required. This mass ratio is roughly similar to 3 times the solar ratio and favors a progenitor white dwarf with a mass near the Chandrasekhar limit. A similar fit using the constructed pseudo-bolometric luminosity gives a mass ratio Ni-57/Ni-56 similar to 0.066(-0.009)(+0.008) . Astrometric tests based on the multi-epoch HST ACS/WFC images reveal no significant circumstellar light echoes in between 0.3 and 100 pc from the supernova.
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