Constraining the Type Ia Supernova Progenitor: The Search for Hydrogen in Nebular Spectra

Details Constraining the Type Ia Supernova Progenitor: The Search for Hydrogen in Nebular Spectra Constraining the Type Ia Supernova Progenitor: The Search for Hydrogen in Nebular Spectra

Oct 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aipc..937..311l&link_type=abstract

SUPERNOVA 1987A: 20 YEARS AFTER: Supernovae and Gamma-Ray Bursters. AIP Conference Proceedings, Volume 937, pp. 311-315 (2007).

Computer Science

4

Supernovae, Supernova Remnants, Circumstellar Shells, Clouds, And Expanding Envelopes, Circumstellar Masers, Spectroscopy And Spectrophotometry, Faint Blue Stars, White Dwarfs, Degenerate Stars, Nuclei Of Planetary Nebulae

Scientific paper

Despite intense scrutiny, the progenitor system(s) that give rise to Type Ia supernovae remains unknown. The favored theory invokes a carbon-oxygen white dwarf accreting hydrogen-rich material from a close companion until a thermonuclear ranaway ensues that incinerates the white dwarf However, simulations resulting from this single-degenerate, binary channel demand the presence of low-velocity Hα emission in spectra taken during the late nebular phase, since a portion of the companion's envelope becomes entrained in the ejecta. This hydrogen has never been detected. Here we present first results from a campaign to obtain deep, nebular-phase spectroscopy of nearby Type Ia supernovae, and include multi-epoch observations of two events: SN 2005am (slightly subluminous) and SN 2005cf (normally bright). No Hα emission is detected in the spectra of either object. An upper limit of 0.01 Msolar of solar abundance material in the ejecta is established from the models of Mattila et al. (2005) which, when coupled with the mass-stripping simulations of Marietta et al. (2000), effectively rules out progenitor systems for these supernovae with secondaries close enough to the white dwarf to be experiencing Roche lobe overflow at the time of explosion.

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