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

  • R. B. Teplitskaya
  • V. G. Skochilov
Conference paper
Part of the International Astronomical Union book series (IAUS, volume 138)


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.


Spectral Type Main Sequence Star Rossby Number Dynamo Action Individual Star 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.


Unable to display preview. Download preview PDF.

Unable to display preview. Download preview PDF.


  1. Barry, D.C., Cromwell, R.H., and Hege, E.K. (1987) ‘Chromospheric activity and ages of solar-type stars’, Astrophys. J. 315, 264–272.ADSCrossRefGoogle Scholar
  2. Catalano, S. and Marilli, E. (1983) ‘Ca II chromospheric emission and rotation of main sequence stars’, Astron. Astrophys. 121, 190–197.ADSGoogle Scholar
  3. Duncan, D.K. (1981) ‘Lithium abundances, K line emission, and ages of nearby solar type stars’, Astrophys. J. 248, 651–669.ADSCrossRefGoogle Scholar
  4. 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.ADSCrossRefGoogle Scholar
  5. Gilliland, R.L. (1985) ‘The relation of chromospheric activity to convection, rotation and evolution of the main sequence’, Astrophys. J. 299, 286–294.ADSCrossRefGoogle Scholar
  6. Giovanelli, R.G. (1980) ‘An exploratory two-dimensional study of the coarse structure of network magnetic fields’, Solar Phys. 68, 49–69.ADSCrossRefGoogle Scholar
  7. 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.ADSCrossRefGoogle Scholar
  8. Rutten, R.G.M. (1987) ‘Magnetic structure in cool stars. XII. Chromospheric activity and rotation of giants and dwarfs’, Astron. Astrophys. 177, 131–142.ADSGoogle Scholar
  9. 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.ADSGoogle Scholar
  10. 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.ADSCrossRefGoogle Scholar
  11. Teplitskaya, R.B. (1989)’ On the relation between activity and rotation in the main-sequince stars’, Astron. Nachr. 310, in press.Google Scholar

Copyright information

© International Astronomical Union 1990

Authors and Affiliations

  • R. B. Teplitskaya
    • 1
  • V. G. Skochilov
    • 1

Personalised recommendations