The Impact of Accretion on Young Stellar Atmospheres

Details The Impact of Accretion on Young Stellar Atmospheres The Impact of Accretion on Young Stellar Atmospheres

Feb 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010head...11.1717b&link_type=abstract

American Astronomical Society, HEAD meeting #11, #17.17; Bulletin of the American Astronomical Society, Vol. 41, p.685

Astronomy and Astrophysics

Astronomy

Scientific paper

The 489 ks Chandra HETG/ACIS-S observation of the classical T Tauri star TW Hydrae has provided a wealth of spectroscopic diagnostics not available in lower signal-to-noise ratio observations. Using line ratios for electron temperature, electron density, and column density we have found that the shock produced by the accelerating material in the accretion stream behaves as predicted by standard theory. However, the properties of the post-shock plasma differ substantially from the predictions of standard 1D shock models (Brickhouset et al. 2010). The accretion process apparently heats the stellar atmosphere up to soft X-ray emitting temperatures, providing hot ions to populate the magnetic corona, in loops, stellar wind, and/or jets. This gas is highly turbulent, as evidenced by non-thermal line broadening. The observed properties of accretion-fed corona should constrain theoretical models of an accretion-driven dynamo.

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