Astronomy and Astrophysics – Astronomy
Scientific paper
Mar 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008head...10.2302g&link_type=abstract
American Astronomical Society, HEAD meeting #10, #23.02
Astronomy and Astrophysics
Astronomy
Scientific paper
High-resolution, high-signal-to-noise X-ray spectra of stellar coronae were needed in the early years of the Chandra and XMM-Newton missions to drive improvements in collisional ionization equilibrium plasma codes over a wide range of temperatures. X-ray spectra of stellar coronae have since been used to demonstrate curious abundance anomalies on magnetically active stars and high densities and high Ne abundances in accreting T Tauri stars. High-resolution spectra have been especially useful though for diagnosing shocked plasmas in stars. X-ray shocks occur around massive O and early B stars through line-driven instabilities, via magnetically confined winds, and in the wind collision zone of close, massive binaries. Strong accretion shocks also produce the hard thermal X-ray spectra seen on many cataclysmic variables. These stellar systems produce shocks spanning a wide range of temperature, density and ionization; some show signatures of non-equilibrium electron/ion temperatures. High-resolution spectra of stars and supernova remnants will be highlighted.
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