Astronomy and Astrophysics – Astronomy
Scientific paper
May 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003aas...202.2408k&link_type=abstract
American Astronomical Society Meeting 202, #24.08; Bulletin of the American Astronomical Society, Vol. 35, p.730
Astronomy and Astrophysics
Astronomy
Scientific paper
The origin of the X-rays from young stars is still a subject of considerable debate. While it had been thought that stellar magnetic dynamos driven by rapid rotation are ultimately responsible for the production of X-rays from T Tauri stars (TTS), recent evidence to the contrary has led to new speculation concerning alternative mechanisms. We have been exploring whether there is observational evidence that X-rays from T Tauri stars are due to interactions between stars and circumstellar disks and, hence, are diagnostic of the presence (or absence) of such disks. Archival ROSAT data demonstrates that the X-ray spectrum of a low-mass star softens as the star evolves from the T Tauri phase to the main sequence. It is unclear whether this trend can be attributed to age-dependent changes in intrinsic X-ray spectrum, to a decrease in the column density of circumstellar gas (e.g., in residual protoplanetary disks), or to the diminishing contributions of star-disk interactions to X-ray emission. New results from high-resolution spectroscopy of TW Hya --- the only classical TTS for which such data have been obtained thus far --- appear to favor the last interpretation. These results from Chandra and XMM-Newton X-ray gratings spectroscopy provide evidence that the bulk of the X-ray emission from TW Hya is generated via mass accretion from its circumstellar disk. Additional high-resolution X-ray spectra of nearby T Tauri stars will provide tests of this hypothesis.
Huenemoerder David P.
Kastner Joel H.
Schulz Norbert S.
Weintraub David A.
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