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Rossby Number or Rotation Period?

Published online by Cambridge University Press:  19 July 2016

K. Stȩpień
K. Stȩpień*
Affiliation:
Astrophysical Institute Potsdam, An der Sternwarte 16 D-O-1561 Potsdam Warsaw University Observatory, Al. Ujazdowskie 4 00-478 Warszawa

Abstract

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It is shown that the scaling of rotation periods by a color-dependent parameter (turnover time) improves substantially the observed activity-period relations only for single, main sequence, solar type stars with 0.5 ≲ B – V ≲ 0.8. For other single main sequence stars and for single giants activity indices correlate equally well with rotation period and the Rossby number, or show no correlation with either parameter.

Keywords

stellar activitystellar rotation
Type
4. Late-Type and Other Stars
Information
Symposium - International Astronomical Union , Volume 157: The Cosmic Dynamo , 1993 , pp. 141 - 145
Copyright
Copyright © Kluwer 1993 

References

Basri, G.: 1986, in Cool Stars, Stellar Systems and the Sun , ed(s). Zeilik, M. and Gibson, D. M., Springer:Berlin, p. 184 Google Scholar
Durney, B.R. and Latour, J.: 1978, Geophys., Astrophys. Fluid Dyn. 9, 241 Google Scholar
Lopéz, J. García, Rebolo, R., Beckman, J.E. and Keith, C.D. Mc: 1991, in The Sun and Cool Stars: activity, magnetism, dynamos , ed(s). Tuominen, I. et al., Springer:Berlin, p. 477 CrossRefGoogle Scholar
Gilliland, R.L.: 1985, Ap. J. 299, 286 CrossRefGoogle Scholar
Hartmann, L.W. and Noyes, R.W.: 1987, Ann. Rev. Astr. Ap. 25, 271 CrossRefGoogle Scholar
Kichatinov, L.L. and Ruediger, G.: 1992, Astr. Ap. , in print Google Scholar
Kraft, R.P.: 1967, Ap. J. 150, 551 Google Scholar
Maggio, A., Vaiana, G.S., Haisch, B.B., Stern, R.A., Bookbinder, J., Harnden, F.R. Jr. and Rosner, R.: 1990, Ap. J. 348, 253 Google Scholar
Noyes, R.W., Hartmann, L.W., Baliunas, S.L., Duncan, D.K. and Vaughan, A.H.: 1984, Ap. J. 279, 763 Google Scholar
Pinsonneault, M.H., Kawaler, S.D., Sofia, S. and Demarque, P.: 1989, Ap. J. 338, 424 Google Scholar
Rucinski, S.M. and VandenBerg, D.A.: 1986, Pub.A.S.P. 98, 669 Google Scholar
Ruediger, G, and Elstner, D.: 1992, Astr. Ap. , in print Google Scholar
Rutten, R.G.M.: 1986, Astr. Ap. 159, 291 Google Scholar
Rutten, R.G.M.: 1987, Astr. Ap. 177, 131 Google Scholar
Schmitt, J.H.M.M., Golub, L., Harnden, F.H. Jr., Maxon, G.W. and Vaiana, S.G.: 1985, Ap. J. 290, 307 Google Scholar
Schrijver, C.J.: 1992, Proc. of IAU Coll. 137 , in print Google Scholar
Simon, T. and Drake, S.A.: 1989, Ap. J. 346, 303 Google Scholar
Simon, T. and Landsman, W.: 1987, in Cool Stars, Stellar Systems and the Sun , ed(s). Linsky, J. L. and Stencel, R. E., Springer:Berlin, p. 265 Google Scholar
Stȩpień, K.: 1988, Ap. J. 335, 907 Google Scholar
Stȩpień, K.: 1989, Astr. Ap. 210, 273 Google Scholar
Wolff, S.C., Boesgaard, A.M. and Simon, T.: 1986, Ap. J. 310, 360 Google Scholar
Young, A., Ajir, F. and Thurman, G.: 1989, Pub.A.S.P. 101, 1017 Google Scholar