Variability of classical T Tauri stars. Its relation to the accretion process.

Details Variability of classical T Tauri stars. Its relation to the accretion process. Variability of classical T Tauri stars. Its relation to the accretion process.

Jun 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996a%26a...310..143f&link_type=abstract

Astronomy and Astrophysics, v.310, p.143-163

Astronomy and Astrophysics

Astrophysics

36

Stars: Formation, Stars: Pre-Main Sequence, Accretion Disks, Star Spots

Scientific paper

We present the analysis of a UBV(RI)_c_ photometric monitoring program carried out from July 1988 to August 1992 on a sample of 13 classical T Tauri stars and 2 suspected classical T Tauri stars. We detected optical irregular variability with an amplitude larger than 0.1mag in the V band in 8 stars. For 5 of them most of the variability can be attributed to hot spots, for one, to cool spots and for two of them, there is no clear mechanism; nevertheless, other phenomena must explain the short term (hours-days) and long term (years) variations superimposed. For some objects an anomalous behaviour at the shorter wavelengths (U band) is detected. From the comparison between the amplitude of the optical variability due to hot spots and the equivalent width of the Halpha_ emission a correlation between them is suggested. Assuming that the Halpha_ emission is related to the accretion process, this correlation supports the idea that we are observing the hot spots where the material from the accretion disks falls onto the star.

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