A hot subdwarf-white dwarf super-Chandrasekhar candidate supernova Ia progenitor
| Autor: | A. Bastian, D. Schneider, P. Neunteufel, Ingrid Pelisoli, Andreas Irrgang, Thomas Kupfer, V. Schaffenroth, Stephan Geier, Brad N. Barlow, J. van Roestel, Uli Heber |
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| Jazyk: | angličtina |
| Rok vydání: | 2021 |
| Předmět: |
Cosmology and Nongalactic Astrophysics (astro-ph.CO)
Astrophysics::High Energy Astrophysical Phenomena FOS: Physical sciences Astrophysics Astrophysics::Cosmology and Extragalactic Astrophysics 01 natural sciences Metric expansion of space 0103 physical sciences Astrophysics::Solar and Stellar Astrophysics Binary system 010303 astronomy & astrophysics Chandrasekhar limit Solar and Stellar Astrophysics (astro-ph.SR) Astrophysics::Galaxy Astrophysics Physics High Energy Astrophysical Phenomena (astro-ph.HE) 010308 nuclear & particles physics Gravitational wave White dwarf Astronomy and Astrophysics Orbital period Subdwarf Supernova Astrophysics - Solar and Stellar Astrophysics Astrophysics::Earth and Planetary Astrophysics Astrophysics - High Energy Astrophysical Phenomena Astrophysics - Cosmology and Nongalactic Astrophysics |
| Popis: | Supernova Ia are bright explosive events that can be used to estimate cosmological distances, allowing us to study the expansion of the Universe. They are understood to result from a thermonuclear detonation in a white dwarf that formed from the exhausted core of a star more massive than the Sun. However, the possible progenitor channels leading to an explosion are a long-standing debate, limiting the precision and accuracy of supernova Ia as distance indicators. Here we present HD265435, a binary system with an orbital period of less than a hundred minutes, consisting of a white dwarf and a hot subdwarf -- a stripped core-helium burning star. The total mass of the system is 1.65+/-0.25 solar-masses, exceeding the Chandrasekhar limit (the maximum mass of a stable white dwarf). The system will merge due to gravitational wave emission in 70 million years, likely triggering a supernova Ia event. We use this detection to place constraints on the contribution of hot subdwarf-white dwarf binaries to supernova Ia progenitors. Preprint of an article published in Nature Astronomy. The final authenticated version is available online at: https://doi.org/10.1038/s41550-021-01413-0 |
| Databáze: | OpenAIRE |
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