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Periodic Light Variability in Four Late-Type Pre-Main-Sequence Stars

Published online by Cambridge University Press:  12 April 2016

F.J. Vrba ,
A.E. Rydgren  and
J.T. Schmelz
F.J. Vrba
Affiliation:
U.S. Naval Observatory, Flagstaff Station, Flagstaff, Arizona
A.E. Rydgren
Affiliation:
Physics Dept., Rensselaer Polytechnic Institute, Troy, New York
J.T. Schmelz
Affiliation:
Physics Dept., Rensselaer Polytechnic Institute, Troy, New York

Extract

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While the T Tauri stars are the best known of the late-type pre-main-sequence (PMS) stars, there are also some late-type PMS stars with only weak line emission in their visible spectra. Several years ago we noted that the weak-emission PMS stars have B-V colors too blue for their V-I colors and suggested that their surfaces might have regions of differing temperature. During October 1981 we used the USNO 40-inch and Kitt Peak National Observatory No. 4 16-inch telescopes to monitor, over a 7 night interval with UBVRI photometry, four of these weak-emission PMS stars: HD 283447, V410 Tau, and X-ray stars 1 and 2 of Feigelson and Kriss (1981). The PMS nature of these stars is established from (1) their membership in the Taurus dark cloud T-association and (2) their location within the T Tauri band region of the H-R diagram.

Type
Session III: Observed Activity in Related Objects
Information
International Astronomical Union Colloquium , Volume 71: Activity in Red-Dwarf Stars , 1983 , pp. 503 - 504
Copyright
Copyright © Reidel 1983

References

REFERENCES

Feigelson, E.D., and Kriss, G.A., 1981, Ap.J.(Letters), 248, L35.CrossRefGoogle Scholar
Vogel, S.N., and Kuhi, L.V., 1981, Ap.J., 245, 960.CrossRefGoogle Scholar