Activity-rotation relations for lower main-sequence stars
It has been known for some time that stellar rotation and activity are related, both for chromospheric activity (e.g., Noyes et al. 1984) and coronal activity (e.g., Pallavicini et al. 1981; Maggio et al. 1987). Younger, more rapidly rotating stars of a given spectral type generally show higher levels of activity than do older, more slowly rotating stars. On the Sun, activity is distinctly related to magnetic fields. This leads to the suggestion that activity, at least in solar-type stars, is traceable to a magnetic dynamo which results from the interaction of rotation and differential rotation with convection. The more efficient the coriolis forces are at introducing helicity into convective motions, the more the magnetic field will be amplified and the more activity we may expect to see. The precise nature of the relationship between magnetic fields, rotation, and activity remains to be well-defined. This thesis examines the relationship between activity (both chromospheric and coronal) and rotation in order to better define and express such a relation (or relations).
- Research Organization:
- New Mexico State Univ., Las Cruces (USA)
- OSTI ID:
- 6684719
- Resource Relation:
- Other Information: Thesis (Ph. D.)
- Country of Publication:
- United States
- Language:
- English
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GENERAL PHYSICS
MAIN SEQUENCE STARS
ROTATION
STELLAR ACTIVITY
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MAGNETIC FIELDS
ENERGY TRANSFER
HEAT TRANSFER
MASS TRANSFER
MOTION
STARS
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