No hot and luminous progenitor for Tycho's supernova
| Autor: | Woods, T. E., Ghavamian, P., Badenes, C., Gilfanov, M. |
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| Rok vydání: | 2017 |
| Předmět: | |
| Zdroj: | Nature Astronomy (2017) |
| Druh dokumentu: | Working Paper |
| DOI: | 10.1038/s41550-017-0263-5 |
| Popis: | Type Ia supernovae have proven vital to our understanding of cosmology, both as standard candles and for their role in galactic chemical evolution; however, their origin remains uncertain. The canonical accretion model implies a hot and luminous progenitor which would ionize the surrounding gas out to a radius of $\sim$10--100 parsecs for $\sim$100,000 years after the explosion. Here we report stringent upper limits on the temperature and luminosity of the progenitor of Tycho's supernova (SN 1572), determined using the remnant itself as a probe of its environment. Hot, luminous progenitors that would have produced a greater hydrogen ionization fraction than that measured at the radius of the present remnant ($\sim$3 parsecs) can thus be excluded. This conclusively rules out steadily nuclear-burning white dwarfs (supersoft X-ray sources), as well as disk emission from a Chandrasekhar-mass white dwarf accreting $\gtrsim 10^{-8}M_{\odot}$yr$^{-1}$ (recurrent novae). The lack of a surrounding Str\"omgren sphere is consistent with the merger of a double white dwarf binary, although other more exotic scenarios may be possible. Comment: 17 pages, 2 figures, including supplementary information. Original accepted manuscript (before copyediting/formatting by Nature Astronomy) |
| Databáze: | arXiv |
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