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Massive star mass-loss revealed by X-ray observations of young supernovae

Published online by Cambridge University Press:  30 December 2019

Vikram V. Dwarkadas Open the ORCID record for Vikram V. Dwarkadas [Opens in a new window]
Vikram V. Dwarkadas*
Affiliation:
Dept. of Astronomy and Astrophysics, Univ of Chicago5640 S Ellis Ave, Chicago, IL 60637 email: [email protected]
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Abstract

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Massive stars lose a considerable amount of mass during their lifetime. When the star explodes as a supernova (SN), the resulting shock wave expands in the medium created by the stellar mass-loss. Thermal X-ray emission from the SN depends on the square of the density of the ambient medium, which in turn depends on the mass-loss rate (and velocity) of the progenitor wind. The emission can therefore be used to probe the stellar mass-loss in the decades or centuries before the star’s death.

We have aggregated together data available in the literature, or analysed by us, to compute the X-ray lightcurves of almost all young supernovae detectable in X-rays. We use this database to explore the mass-loss rates of massive stars that collapse to form supernovae. Mass-loss rates are lowest for the common Type IIP supernovae, but increase by several orders of magnitude for the highest luminosity X-ray SNe.

Keywords

radiation mechanisms: thermalshock wavesastronomical data bases: miscellaneouscircumstellar matterstars: mass losssupernovae: generalstars: windsoutflowsstars: Wolf-RayetX-rays: general
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S346: High-mass X-ray Binaries: Illuminating the Passage from Massive Binaries to Merging Compact Objects , August 2018 , pp. 83 - 87
Copyright
© International Astronomical Union 2019 

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