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Massive star winds and HMXB donors

Published online by Cambridge University Press:  30 December 2019

Andreas A. C. Sander Open the ORCID record for Andreas A. C. Sander [Opens in a new window]
Andreas A. C. Sander*
Affiliation:
Armagh Observatory and Planetarium, College Hill, Armagh BT61 9DG, Northern Ireland, UK email: Andreas.Sander@armagh.ac.uk Institut für Physik und Astronomie, Universität Potsdam, Karl-Liebknecht-Str. 24/25, D-14476 Potsdam, Germany
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Abstract

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Understanding the complex behavior of High Mass X-ray binaries (HMXBs) is not possible without detailed information about their donor stars. While crucial, this turns out to be a challenge on multiple fronts. First, multi-wavelength spectroscopy is vital. As such systems can be highly absorbed, this is often already hard to accomplish. Secondly, even if the spectroscopic data is available, the determination of reliable stellar parameters requires sophisticated model atmospheres that accurately describe the outermost layers and the wind of the donor star.

For early-type donors, the stellar wind is radiatively driven and there is a smooth transition between the outermost layers of the star and the wind. The intricate non-LTE conditions in the winds of hot stars complicate the situation even further, as proper model atmospheres need to account for a multitude of physics to accurately provide stellar and wind parameters. The latter are especially crucial for the so-called “wind-fed” HXMBs, where the captured wind of the supergiant donor is the only source for the material accreted by the compact object.

In this review I will briefly address the different approaches for treating stellar winds in the analysis of HMXBs. The fundamentals of stellar atmosphere modeling will be discussed, also addressing the limitations of modern models. Examples from recent analysis results for particular HMXBs will be outlined. Furthermore, the path for the next generation of stellar atmosphere models will be outlined, where models can be used not only for measurement purposes, but also to make predictions and provide a laboratory for theoretical conclusions. Stellar atmospheres are a key tool in understanding HMXBs, e.g. by providing insights about the accretion of stellar winds onto the compact object, or by placing the studied systems in the correct evolutionary context in order to identify potential gravitational wave (GW) progenitors.

Keywords

accretionhydrodynamicsmethods: numericalradiative transferstars: atmospheresstars: early-typestars: individual (4U 1700-37, 4U1907+09, 4U 1909+07, GX304-01, IGR J16465-4507, IGR J17544-2619, Vela X-1)stars: mass lossstars: neutronstars: windsoutflowsX-rays: binaries
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. 17 - 27
Copyright
© International Astronomical Union 2019 

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