Radii and Mass-loss Rates of Type IIb Supernova Progenitors
| Autor: | Ryoma Ouchi, Keiichi Maeda |
|---|---|
| Rok vydání: | 2017 |
| Předmět: |
High Energy Astrophysical Phenomena (astro-ph.HE)
Physics education.field_of_study 010308 nuclear & particles physics Population FOS: Physical sciences Binary number Astronomy and Astrophysics Radius Astrophysics 01 natural sciences Spectral line Supernova Type iib Space and Planetary Science 0103 physical sciences Astrophysics - High Energy Astrophysical Phenomena education 010303 astronomy & astrophysics Order of magnitude |
| Zdroj: | The Astrophysical Journal. 840:90 |
| ISSN: | 1538-4357 |
| DOI: | 10.3847/1538-4357/aa6ea9 |
| Popis: | Several Type IIb supernovae (SNe IIb) have been extensively studied, both in terms of the progenitor radius and the mass-loss rate in the final centuries before the explosion. While the sample is still limited, evidence has been accumulating that the final mass-loss rate tends to be larger for a more extended progenitor, with the difference exceeding an order of magnitude between the more and less extended progenitors. The high mass-loss rates inferred for the more extended progenitors are not readily explained by a prescription commonly used for a single stellar wind. In this paper, we calculate a grid of binary evolution models. We show that the observational relation in the progenitor radii and mass-loss rates may be a consequence of non-conservative mass transfer in the final phase of progenitor evolution without fine tuning. Further, we find a possible link between SNe IIb and SNe IIn. The binary scenario for SNe IIb inevitably leads to a population of SN progenitors surrounded by dense circumstellar matter (CSM) due to extensive mass loss ($\dot{M} \gtrsim 10^{-4} M_{\odot} \mathrm{yr}^{-1}$) in the binary origin. About 4% of all observed SNe IIn are predicted to have dense CSM, produced by binary non-conservative mass transfer, whose observed characteristics are distinguishable from SNe IIn from other scenarios. Indeed, such SNe may be observationally dominated by systems experiencing huge mass loss in the final $10^3$ yr, leading to luminous SNe IIn or initially bright SNe IIP or IIL with characteristics of SNe IIn in their early spectra. Comment: 18 pages, 12 figures, Accepted for publication in The Astrophysical Journal |
| Databáze: | OpenAIRE |
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