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• W2079078636 abstract "Despite intense scrutiny, the progenitor system(s) that gives 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 runaway 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, but has only rarely been sought. Here we present results from a campaign to obtain deep, nebular-phase spectroscopy of nearby Type Ia supernovae, and include multiepoch 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 M☉ of solar abundance material in the ejecta is established from the models of Mattila et al., which, when coupled with the mass-stripping simulations of Marietta et al. and Meng et al., 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. Alternative explanations for the absence of Hα emission, along with suggestions for future investigations necessary to confidently exclude them as possibilities, are critically evaluated." @default.
• W2079078636 created "2016-06-24" @default.
• W2079078636 creator A5003690438 @default.
• W2079078636 date "2007-12-01" @default.
• W2079078636 modified "2023-10-18" @default.
• W2079078636 title "Constraining the Type Ia Supernova Progenitor: The Search for Hydrogen in Nebular Spectra" @default.
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• W2079078636 doi "https://doi.org/10.1086/522367" @default.
• W2079078636 hasPublicationYear "2007" @default.
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