Modeling X-ray Emission Line Profiles from Massive Star Winds - A Review

TL;DR

This review discusses modeling techniques for X-ray emission line profiles from massive star winds, emphasizing recent high-resolution spectroscopic observations and various wind conditions.

Contribution

It provides a comprehensive overview of modeling approaches for X-ray line profiles considering wind clumping, optical depth, and absorption effects.

Findings

Spectroscopic resolution has improved understanding of wind-broadened lines.

Models account for wind clumping and optical depth variations.

Photoabsorption effects influence line profile shapes.

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.