Physics – Plasma Physics
Scientific paper
Oct 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003aps..dppqi2005h&link_type=abstract
American Physical Society, 45th Annual Meeting of the Division of Plasma Physics, October 27-31, 2003, Albuquerque, New Mexico,
Physics
Plasma Physics
Scientific paper
The Chandra X-Ray Observatory grating spectrometers allow us to study stellar spectra at resolutions on the order of 1000. Prior X-ray observatories' low resolution data have shown that nearly all classes of stars emit X-rays. With Chandra, we can study in detail the line and continuum contributions to the spectra and apply atomic databases in plasma models. For cool stars with hot coronae interpreted in the Solar paradigm, we can assume collisional ionization equilibrium and derive temperature distributions, elemental abundances, and densities. Abundance trends are unlike the Sun, as are the very hot temperature distributions. For young stars, we have evidence of accretion driven X-ray emission, rather than magnetically confined plasma emission. For hot stars, we expected a shocked wind signature, but instead also have evidence for magnetically confined thermal plasmas. Hot stars also show photoexcitation in helium-like lines, which can be used to model emission structures.
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