Modeling X-ray Emission Line Profiles from Massive Star Winds - A Review
arXiv:1601.00552 · doi:10.1016/j.asr.2015.12.044
Abstract
The Chandra and XMM-Newton X-ray telescopes have led to numerous advances in the study and understanding of astrophysical X-ray sources. Particularly important has been the much increased spectral resolution of modern X-ray instrumentation. Wind-broadened emission lines have been spectroscopically resolved for many massive stars. This contribution reviews approaches to the modeling of X-ray emission line profile shapes from single stars, including smooth winds, winds with clumping, optically thin versus thick lines, and the effect of a radius-dependent photoabsorption coefficient.
to appear in Advances in Space Research
References in corpus (14)
- Pre-Supernova Evolution of Massive Single and Binary Stars
- X-Ray Spectroscopy of Stars
- The Effect of Porosity on X-ray Emission Line Profiles from Hot-Star Winds
- High resolution X-ray spectroscopy of bright O type stars
- An Extensive Collection of Stellar Wind X-ray Source Region Emission Line Parameters,Temperatures, Velocities, and Their Radial Distributions as Obtained from Chandra Observations of 17 OB Stars
- A consistent solution for the velocity field and mass-loss rate of massive stars
- Direct spectroscopic observations of clumping in O-star winds
- On the Importance of the Interclump Medium for Superionization: O VI Formation in the Wind of Zeta Pup
- Evidence for the importance of resonance scattering in X-ray emission line profiles of the O star Puppis
- The Effects of Clumps in Explaining X-ray Emission Lines from Hot Stars
- Measuring the shock-heating rate in the winds of O stars using X-ray line spectra
- Does The Addition of a Duration Improve the L_iso - E_peak Relation For Gamma-Ray Bursts?
- Probing Wolf-Rayet Winds: Chandra/HETG X-Ray Spectra of WR 6
- Polarimetric modeling of corotating interaction regions (CIRs) threading massive-star winds