Rotation periods of four T Tauri stars
Citations Over TimeTop 10% of 1988 papers
Abstract
BVR photometry of nine T Tauri and related stars was obtained on 13 nights in January 1988, in an attempt to confirm reported periodicities and discover new ones. Rotation periods previously reported for T Tau by Herbst et al. (1986) and HM 4 (LHα 332-20) and HM 30 (LHα 332-21) by Bouvier et al. (1986) were confirmed. A periodicity of 1.28 days was discovered for TW Hya; it was also the only star to show significant variations during the course of a single night. SU Aur, RY Tau, BF Ori, V380 Ori, and FU Ori all exhibited variability, but without detectable periodicity. This is in agreement with a previous suggestion that periodicity is more easily found in the later-type pre-main-sequence stars (i.e., later than about K0). The results for T Tau buttress arguments that we are viewing this star more nearly pole-on than equator on. Color variations indicate that the authors are seeing a hotspot on TW Hya, possibly arising in the boundary layer between an accretion disk and the photosphere. The spots on T Tau, HM 4, and HM 30 are more likely to be cool, analogous to sunspots.
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