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- W3103661904 abstract "Two twin Type Ia supernovae (SNe Ia), SNe 2011by and 2011fe, have extremely similar optical light-curve shapes, colors, and spectra, yet have different ultraviolet (UV) continua as measured in Hubble Space Telescope spectra and measurably different peak luminosities. We attribute the difference in the UV continua to significantly different progenitor metallicities. This is the first robust detection of different metallicities for SN Ia progenitors. Theoretical reasoning suggests that differences in metallicity also lead to differences in luminosity. SNe Ia with higher progenitor metallicities have lower 56Ni yields, and lower luminosities, for the same light-curve shape. SNe 2011by and 2011fe have different peak luminosities (Delta M_V = 0.6 mag), which correspond to different 56Ni yields: M_11fe(56Ni)/M_11by(56Ni) = 1.7^+0.7_-0.5. From theoretical models that account for different neutron to proton ratios in progenitors, the differences in 56Ni yields for SNe 2011by and 2011fe imply that their progenitor stars were above and below solar metallicity, respectively. Although we can distinguish progenitor metallicities in a qualitative way from UV data, the quantitative interpretation in terms of abundances is limited by the present state of theoretical models." @default.
- W3103661904 created "2020-11-23" @default.
- W3103661904 creator A5000747773 @default.
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- W3103661904 date "2013-05-01" @default.
- W3103661904 modified "2023-10-14" @default.
- W3103661904 title "METALLICITY DIFFERENCES IN TYPE Ia SUPERNOVA PROGENITORS INFERRED FROM ULTRAVIOLET SPECTRA" @default.
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- W3103661904 doi "https://doi.org/10.1088/2041-8205/769/1/l1" @default.
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