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Late-Phase Observations of a Super-Chandrasekhar SN Ia

Published online by Cambridge University Press:  17 January 2013

M. Yamanaka ,
K. S. Kawabata ,
K. Maeda ,
M. Tanaka ,
M. Yoshida ,
T. Hattori ,
K. Nomoto ,
T. Komatsu  and
T. Okushima
M. Yamanaka
Affiliation:
Hiroshima Astrophysical Science Center, Hiroshima University, Higashi-Hiroshima, Hiroshima 739-8526, Japan email: myamanaka@hiroshima-u.ac.jp
K. S. Kawabata
Affiliation:
Hiroshima Astrophysical Science Center, Hiroshima University, Higashi-Hiroshima, Hiroshima 739-8526, Japan email: myamanaka@hiroshima-u.ac.jp
K. Maeda
Affiliation:
Institute for the Physics and Mathematics of the Universe, University of Tokyo, Kashiwa, Japan
M. Tanaka
Affiliation:
Institute for the Physics and Mathematics of the Universe, University of Tokyo, Kashiwa, Japan
M. Yoshida
Affiliation:
Hiroshima Astrophysical Science Center, Hiroshima University, Higashi-Hiroshima, Hiroshima 739-8526, Japan email: myamanaka@hiroshima-u.ac.jp
T. Hattori
Affiliation:
Subaru Telescope, National Astronomical Observatory of Japan, Hilo, HI, USA
K. Nomoto
Affiliation:
Institute for the Physics and Mathematics of the Universe, University of Tokyo, Kashiwa, Japan
T. Komatsu
Affiliation:
Department of Physical Science, Hiroshima University, Kagamiyama 1-3-1, Higashi-Hiroshima 739-8526, Japan
T. Okushima
Affiliation:
Department of Physical Science, Hiroshima University, Kagamiyama 1-3-1, Higashi-Hiroshima 739-8526, Japan
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Abstract

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A super-Chandrasekhar (SC) supernova (SN) has an extremely high luminosity and a slow decline rate of the light curve in the early-phase. We present late-phase observations of the SC SN 2009dc. We find that the optical luminosity a year after maximum is much fainter than that expected from its early luminosity. We attempt to fit the analytic light curve model to the observations using Arnett's rule. The model successfully explains the light curves until 120 days. This suggests that the extremely high luminosity originates from the 56Ni decay. We suggest that the late-phase decline would be caused by dust formation. The existence of strong carbon features in early-phase spectra would support this scenario. We also find a blend of [Ca ii] and [Ni ii] in its late-phase spectrum. This indicates that the calcium is distributed in the inner layer along with nickel and iron. We conclude that the mixing may occur in the inner parts of the ejecta.

Keywords

supernovae: individual (SN 2009dc)
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Issue S281: Binary Paths to Type Ia Supernovae Explosions , July 2011 , pp. 319 - 321
Copyright
Copyright © International Astronomical Union 2013

References

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