English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

Massive stars drive powerful, supersonic winds via the radiative momentumassociated with the thermal UV emission from their photospheres. Shockphenomena are ubiquitous in these winds, heating them to millions, andsometimes tens of millions, of degrees. The emission line spectra from theshock-heated plasma provide powerful diagnostics of the winds' physicalconditions, which in turn provide constraints on models of wind shock heating.Here I show how x-ray line transfer is affected by photoelectric absorption inthe partially ionized component of the wind and how it can be modeled todetermine the astrophysically important mass-loss rates of these stellar winds.I also discuss how photoexcitation out of metastable excited levels ofhelium-like ions can provide critical information about the location of the hotplasma in magnetically channeled massive star winds.

X-ray Spectroscopy of the Radiation-Driven Winds of Massive Stars: Line Profile and Line Ratio Diagnostics