Structure of the inner region of the accretion disk of the Herbig Ae star CQ Tau based on long-term monitoring data

Details Structure of the inner region of the accretion disk of the Herbig Ae star CQ Tau based on long-term monitoring data Structure of the inner region of the accretion disk of the Herbig Ae star CQ Tau based on long-term monitoring data

Jan 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007ap.....50...26k&link_type=abstract

Astrophysics, Volume 50, Issue 1, pp.26-39

Astronomy and Astrophysics

Astrophysics

Stars, Accretion Disk-Individual, Cq Tau

Scientific paper

Results from simultaneous spectral and photometric monitoring of the Herbig Ae star CQ Tau in the neighborhood of the Hα and resonance sodium doublet Na I D lines are presented. It is shown that the inner structure of the accretion disk of CQ Tau is nonuniform and consists of two regions with quite different kinematic characteristics. Region I is characterized by relative stability and a smooth long-term variation in the velocity of the gas along the line of sight. Region II is distinguished by the highest velocities and a variability in their maximum values over time scales from a few days to 700 days. The dust clouds which produse the star’s brightness minima may also be the source of cold gas and contribute to the observed spectral variability. We assume that region I of the disk coincides with the accretion disk of the star. The kinematic differences in region II may be caused by dissipation of circumstellar dust clouds which, moving in elongated orbits, are able to approach the star quite closely.

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