The ultraviolet and visible light variability of BP Tauri - Possible clues for the origin of T Tauri star activity

Details The ultraviolet and visible light variability of BP Tauri - Possible clues for the origin of T Tauri star activity The ultraviolet and visible light variability of BP Tauri - Possible clues for the origin of T Tauri star activity

Dec 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990aj....100.1957s&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 100, Dec. 1990, p. 1957-1967.

Astronomy and Astrophysics

Astronomy

51

Irregular Variable Stars, Light Curve, Stellar Activity, T Tauri Stars, Ultraviolet Radiation, Iue, Stellar Spectrophotometry, Visual Photometry

Scientific paper

BP Tau is a moderate-strength T Tauri star, which has previously been studied photometrically by Vrba et al. (1986, 1989) and shown to have a 7.6-day light cycle. Here, BP Tau was reobserved in order to monitor this star with the IUE satellite. In conjunction with the UV spectroscopy, nearly simultaneous ground-based optical photometry was also obtained. At optical wavelengths, the star was initially found to be varying with a period of 7.6 days. This variability suddenly vanished and was followed by a quiescent state that lasted about 11 days. The star then resumed its variability with a period of about 6.1 days. The UV continuum and most of the UV emission lines appeared to vary in phase with the optical flux. No variations were observed on the very short timescales ranging from several hours to half a day, expected on the basis of axisymmetric, quasi-steady-state accretion disk models of T Tauri stars. However, the nearly week-long variations that were observed may be consistent with a magnetically buffered accretion model, which has been proposed by Uchida and Shibata.

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