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The Possible Connexion Between T Tauri Stars and UV Ceti Stars

Published online by Cambridge University Press:  14 August 2015

Guillermo Haro
Guillermo Haro*
Affiliation:
Tonantzintla and Tacubaya Observatories, México, D.F.

Extract

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As is well known, very rapid and non-periodic changes in brightness have been discovered in several late-type dwarf stars in recent years. In the vicinity of the sun, within a radius not exceeding 10 parsecs, nine or ten such objects have been found and named ‘flare’ stars because of their extraordinarily rapid variations. The prototype of these flare stars is UV Ceti. For the purpose of the present discussion, we shall call these objects ‘classical’ flare stars.

Type
I. Instability in Dwarf Stars of Later Type: T Tauri Stars and Related Objects, and The UV Ceti Variables
Information
Symposium - International Astronomical Union , Volume 3: Non-Stable Stars , 1957 , pp. 26 - 30
Copyright
Copyright © Cambridge University Press 1957 

References

1. Haro, G. and Terrazas, L. R., Bol. Obs. Tonantzintla y Tacubaya, No. 10, 3 (1954).Google Scholar
2. Haro, G., Bol. Obs. Tonantzintla y Tacubaya, No. 11, 11 (1954).Google Scholar
3. Haro, G. and Chavira, E., Bol. Obs. Tonantzintla y Tacubaya, No. 12, 3 (1955).Google Scholar
4. Joy, A. H., Ap.J. 102, 168 (1945).CrossRefGoogle Scholar
5. Thackeray, A. D., M.N. 110, 45 (1950).Google Scholar
6. Popper, D. M., Publ. A.S.P. 65, 278 (1953).CrossRefGoogle Scholar
7. Delhaye, J., Comptes rendus, 237, 294 (1953).Google Scholar