Wind characteristics in the Chandra HMXB sample
Abstract
High-Mass X-ray binaries (HMXBs) are powered by accretion from the dense stellar wind of their optical companion. Understanding the stellar wind is therefore paramount to understand the luminosity and spectral variability of the X-ray source. We know that the accreted medium is highly structured, due to a combination of a clumpy stellar wind and the influence of the compact object. Detailed modeling of high-resolution X-ray spectra with clumpy wind models, however, is missing. Here, we propose to re-analyze five purely wind-accreting neutron star HMXBs with the latest state-of-the-art wind models, obtaining a uniform sample to study the structure and physical conditions of the accreted medium.
- Publication:
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Chandra Proposal
- Pub Date:
- September 2015
- Bibcode:
- 2015cxo..prop.4739F