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Does a Common Dynamo Mechanism Exist for Lower Main Sequence Stars?

Published online by Cambridge University Press:  08 February 2017

R.B. Teplitskaya  and
V.G. Skochilov
R.B. Teplitskaya
Affiliation:
SibIZMIR P.O. Box 4, Irkutsk 33 664033, USSR
V.G. Skochilov
Affiliation:
SibIZMIR P.O. Box 4, Irkutsk 33 664033, USSR

Abstract

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Based on an extended list of lower main sequence stars from Rutten (1987), the relation between chromospheric activity and Rossby number has been revised. The increased statistics changes the shape of the curve as compared with that of Noyes et al. (1984). The saturation at small Rossby numbers has disappeared. The dependence on Rossby number in the range of very large Rossby numbers has weakened. The standard deviation of the activity indices from the mean curve is about 40%. This scatter of individual stars is not due to differences in the spectral type or age of the stars.

Type
VII. Convection and Magnetic Fields in Solar-type Stars
Information
Symposium - International Astronomical Union , Volume 138: Solar Photosphere: Structure, Convection and Magnetic Fields , 1990 , pp. 455 - 459
Copyright
Copyright © Kluwer 1990 

References

Barry, D.C., Cromwell, R.H., and Hege, E.K. (1987) ‘Chromospheric activity and ages of solar-type stars’, Astrophys. J. 315, 264–272.CrossRefGoogle Scholar
Catalano, S. and Marilli, E. (1983) ‘Ca II chromospheric emission and rotation of main sequence stars’, Astron. Astrophys. 121, 190–197.Google Scholar
Duncan, D.K. (1981) ‘Lithium abundances, K line emission, and ages of nearby solar type stars’, Astrophys. J. 248, 651–669.CrossRefGoogle Scholar
Durney, B.R. and Robinson, R.D. (1982) ‘On an estimate of the dynamo-generated magnetic fields in late-type stars’, Astrophys. J. 253, 290–297.CrossRefGoogle Scholar
Gilliland, R.L. (1985) ‘The relation of chromospheric activity to convection, rotation and evolution of the main sequence’, Astrophys. J. 299, 286–294.CrossRefGoogle Scholar
Giovanelli, R.G. (1980) ‘An exploratory two-dimensional study of the coarse structure of network magnetic fields’, Solar Phys. 68, 49–69.CrossRefGoogle Scholar
Noyes, R.W., Hartmann, L.W., Baliunas, S.L., Duncan, D.K., and Vaughan, A.H. (1984) ‘Rotation, convection, and magnetic activity in lower main-sequence stars’ , Astrophys. J. 279, 763–777.CrossRefGoogle Scholar
Rutten, R.G.M. (1987) ‘Magnetic structure in cool stars. XII. Chromospheric activity and rotation of giants and dwarfs’, Astron. Astrophys. 177, 131–142.Google Scholar
Schrijver, C.J. and Rutten, R.G.M. (1987) ‘Magnetic structure in cool stars. XIV. Deficiency in chromospheric fluxes from M-type dwarfs’, Astron. Astrophys. 177, 143–149.Google Scholar
Stauffer, J.R., Hartman, L., Soderblom, D.R., and Burnham, N. (1984) ‘Rotational velocities of low-mass stars in the Pleiades’, Astrophys. J. 280, 202–212.CrossRefGoogle Scholar
Teplitskaya, R.B. (1989) ‘On the relation between activity and rotation in the main-sequence stars’ , Astron. Nachr. 310, in press.CrossRefGoogle Scholar