Статья

A COMPACT DEGENERATE PRIMARY-STAR PROGENITOR OF SN 2011fe

J. S. BloomDepartment of Astronomy, University of California, Berkeley, Berkeley CA, 94720-3411, USA; [email protected]Daniel KasenDepartment of Astronomy, University of California, Berkeley, Berkeley CA, 94720-3411, USA; [email protected]Ken J. ShenNuclear Science Division, Lawrence Berkeley National Laboratory, Berkeley, CA 94720, USAP. NugentDepartment of Astronomy, University of California, Berkeley, Berkeley CA, 94720-3411, USA; [email protected]N. ButlerSchool of Earth and Space Exploration, Arizona State University, P.O. Box 871404, Tempe, AZ 85287-1404, USAM. L. GrahamDepartment of Physics, University of California Santa Barbara, Santa Barbara, CA 93106, USAD. A. HowellDepartment of Physics, University of California Santa Barbara, Santa Barbara, CA 93106, USAU. KolbDepartment of Physical Sciences, The Open University, Walton Hall, Milton Keynes MK7 6AA, UKStefan HolmesDepartment of Physical Sciences, The Open University, Walton Hall, Milton Keynes MK7 6AA, UKC. A. HaswellDepartment of Physical Sciences, The Open University, Walton Hall, Milton Keynes MK7 6AA, UKV. BurwitzMax-Planck-Institut für extraterrestrische Physik, Giessenbachstrasse, 85748 Garching, GermanyJuan RodriguezObservatori Astronòmic de Mallorca, Camí de l’Observatori, 07144 Costitx, Mallorca, SpainM. SullivanDepartment of Physics (Astrophysics), University of Oxford, Keble Road, Oxford OX1 3RH, UK

2011en

ABI

Аннотация

While a white dwarf is, from a theoretical perspective, the most plausible primary star in Type Ia supernova (SN Ia), many other candidates have not been formally ruled out. Shock energy deposited in the envelope of any exploding primary contributes to the early SN brightness and, since this radiation energy is degraded by expansion after the explosion, the diffusive luminosity depends on the initial primary radius. We present a new non-detection limit of the nearby SN Ia 2011fe, obtained what appears to be just 4 hours after explosion, allowing us to directly constrain the initial primary radius, R_p. Coupled with the non-detection of a quiescent X-ray counterpart and the inferred synthesized Ni mass, we show that R_p <~ 0.02 R_sun (a factor of 5 smaller than previously inferred), that the average density of the primary must be rho_p > 10,000 gm cm^{-3}, and that the effective temperature must be less than a few x 10^5 K. This rules out hydrogen burning main sequence stars and giants. Constructing the helium-burning main sequence and carbon-burning main sequence, we find such objects are also excluded. By process of elimination, we find that only degeneracy-supported compact objects---WDs and neutron stars---are viable as the primary star of SN 2011fe. With few caveats, we also restrict the companion (secondary) star radius to R_ c <~ 0.1 R_sun, excluding Roche-Lobe overflowing red giant and main-sequence companions to high significance.

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Идентификаторы

DOI: 10.1088/2041-8205/744/2/l17

Цитирования и источники

Цитирований: 5Использованных источников: 0

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