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Journal Article

A hot subdwarf–white dwarf super-Chandrasekhar candidate supernova Ia progenitor


Neunteufel,  P.
High Energy Astrophysics, MPI for Astrophysics, Max Planck Society;

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Pelisoli, I., Neunteufel, P., Geier, S., Kupfer, T., Heber, U., Irrgang, A., et al. (2021). A hot subdwarf–white dwarf super-Chandrasekhar candidate supernova Ia progenitor. Nature astronomy, 2021(6), 1052-1061. doi:10.5281/zenodo.4792304.

Cite as: https://hdl.handle.net/21.11116/0000-0009-59EC-A
Supernovae 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 supernovae Ia as distance indicators. Here we present HD 265435, a binary system with an orbital period of less than a hundred minutes that consists of a white dwarf and a hot subdwarf, which is 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 owing 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.