Astronomy and Astrophysics – Astrophysics
Scientific paper
Oct 1985
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985soph..100..385n&link_type=abstract
Solar Physics (ISSN 0038-0938), vol. 100, Oct. 1985, p. 385-396.
Astronomy and Astrophysics
Astrophysics
7
Astrophysics, Solar Magnetic Field, Stellar Activity, Convective Heat Transfer, H Lines, K Lines, Main Sequence Stars, Solar Cycles, Stellar Rotation
Scientific paper
The techniques and principal results of observational studies of stellar activity are summarized. Both chromospheric and coronal emission clearly track surface magnetic field properties, but it is not well known how the detailed relation between the emission and surface magnetic fields varies with spectral type. For lower Main-Sequence stars of the same spectral type, there is clear evidence of a close relationship between mean activity level and rotation period. For single stars, stellar rotation, and magnetic activity both decline smoothly with age. This implies a feedback between angular momentum loss rate and activity level. Temporal variations in mean stellar activity level mimic the solar cycle only for old stars like the Sun, being much more irregular for younger stars. Further data on mean activity and its variation for a large number of lower Main-Sequence stars should contribute significantly to our understanding of the causes of stellar magnetic activity.
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