Chromospheric Emission of Close Binaries
Abstract
It is generally believed that rapid rotation of stars enhances chromospheric emission. Studies of G stars have led to this conclusion. Our studies of Mg II k emission in early F stars only shows that close binaries show increased emission while single rapidly rotating stars with v(r) sin i > 40 km/sec do not. For G stars close binaries are usually the only ones that rotate at a measurable rate. Rapid rotation and binary nature are correlated. For early F stars this is not the case. We therefore propose to study early F star binaries of known periods and different rotational velocities in order to decide on the cause of enhanced emission: either tidal effects in close binaries or rapid rotation.
- Publication:
-
IUE Proposal
- Pub Date:
- 1983
- Bibcode:
- 1983iue..prop.1400B