The origin of the photometric and spectral variability of RW Aur

Details The origin of the photometric and spectral variability of RW Aur The origin of the photometric and spectral variability of RW Aur

Jun 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007arep...51..500p&link_type=abstract

Astronomy Reports, Volume 51, Issue 6, pp.500-511

Astronomy and Astrophysics

Astronomy

3

97.21.+A, 95.85.Kr

Scientific paper

We have studied the relationships between the brightness, color, and emission-line profiles for the classical T Tauri star RW Aur, which displays an intense emission spectrum and signs of accretion and outflow. Spectral and photometric observations carried out from 1995 to 1999 have been analyzed in the framework of magnetospheric accretion concept, where the brightness of the star depends on the level of the non-photospheric continuum (veiling), which, in turn, depends on the accretion rate. We found that (1) the equivalent widths and profiles of broad emission lines vary independently of the brightness of the star, the brightness and color variations are due primarily to absorption in dust clouds formed by the disk wind; (2) at times when the accretion in the line of sight becomes stronger, all broad emission lines are weakened substantially due to the asymmetry of the magnetosphere and screening of the radiating region; (3) the periodic variations of the U-B and B-V color indices are due to the variable contribution of broad emission lines in the photometric bands; (4) the veiling of the photospheric spectrum is not correlated with either the brightness of the star or the intensity of the accretion components.

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