A compact degenerate primary-star progenitor of SN 2011fe

Joshua S. Bloom, Daniel Kasen, Ken J. Shen, Peter E. Nugent, Nathaniel Butler, Melissa L. Graham, D. Andrew Howell, Ulrich Kolb, Stefan Holmes, Carole A. Haswell, Vadim Burwitz, Juan Rodriguez, Mark Sullivan

Research output: Contribution to journalArticle

195 Citations (Scopus)

Abstract

While a white dwarf (WD) is, from a theoretical perspective, the most plausible primary star of a 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 at a time that appears to be just 4hr after explosion, allowing us to directly constrain the initial primary radius (Rp ). Coupled with the non-detection of a quiescent X-ray counterpart and the inferred synthesized 56Ni mass, we show that Rp ≲ 0.02 R (a factor of five smaller than previously inferred), that the average density of the primary must be ρp > 104 g cm-3, and that the effective temperature must be less than a few × 105K. This rules out hydrogen-burning main-sequence stars and giants. Constructing the helium-burning and carbon-burning main sequences, we find that 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 SN2011fe. With few caveats, we also restrict the companion (secondary) star radius to R c ≲ 0.1 R , excluding Roche-lobe overflowing red giant and main-sequence companions to high significance.

Original languageEnglish (US)
Article numberL17
JournalAstrophysical Journal Letters
Volume744
Issue number2
DOIs
StatePublished - Jan 10 2012

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stars
explosion
radii
explosions
helium
energy
main sequence stars
lobes
hydrogen
neutron stars
supernovae
elimination
brightness
envelopes
shock
luminosity
carbon
expansion
radiation
temperature

Keywords

  • supernovae: general
  • supernovae: individual (2011fe, white dwarfs)

ASJC Scopus subject areas

  • Space and Planetary Science
  • Astronomy and Astrophysics

Cite this

Bloom, J. S., Kasen, D., Shen, K. J., Nugent, P. E., Butler, N., Graham, M. L., ... Sullivan, M. (2012). A compact degenerate primary-star progenitor of SN 2011fe. Astrophysical Journal Letters, 744(2), [L17]. https://doi.org/10.1088/2041-8205/744/2/L17

A compact degenerate primary-star progenitor of SN 2011fe. / Bloom, Joshua S.; Kasen, Daniel; Shen, Ken J.; Nugent, Peter E.; Butler, Nathaniel; Graham, Melissa L.; Andrew Howell, D.; Kolb, Ulrich; Holmes, Stefan; Haswell, Carole A.; Burwitz, Vadim; Rodriguez, Juan; Sullivan, Mark.

In: Astrophysical Journal Letters, Vol. 744, No. 2, L17, 10.01.2012.

Research output: Contribution to journalArticle

Bloom, JS, Kasen, D, Shen, KJ, Nugent, PE, Butler, N, Graham, ML, Andrew Howell, D, Kolb, U, Holmes, S, Haswell, CA, Burwitz, V, Rodriguez, J & Sullivan, M 2012, 'A compact degenerate primary-star progenitor of SN 2011fe', Astrophysical Journal Letters, vol. 744, no. 2, L17. https://doi.org/10.1088/2041-8205/744/2/L17
Bloom, Joshua S. ; Kasen, Daniel ; Shen, Ken J. ; Nugent, Peter E. ; Butler, Nathaniel ; Graham, Melissa L. ; Andrew Howell, D. ; Kolb, Ulrich ; Holmes, Stefan ; Haswell, Carole A. ; Burwitz, Vadim ; Rodriguez, Juan ; Sullivan, Mark. / A compact degenerate primary-star progenitor of SN 2011fe. In: Astrophysical Journal Letters. 2012 ; Vol. 744, No. 2.
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