[Previous] | [Session 9] | [Next]
A. Brown, R.A. Osten (CASA, U. of Colorado), C.W. Ambruster (Villanova U.), G.E. Bromage (U. of Central Lancashire, UK), R. Jeffries (Keele U., UK)
We present coronal EUV, X-ray and radio data for a sample of nearby (\leq 45 pc), young Pleaides-age K and M dwarfs. Nine of the stars form an essentially equal mass (spectral types K0-3 V) sample whose coronal activity is determined by a single parameter - the stellar rotation rate. Within this sample rotation period ranges from 0.4 to 6.6 days with a good sampling of all periods. We show how the activity level seen from the thermal (EUV, X-ray) and non-thermal (radio) coronae changes as a function of rotation. Similarly the coronal temperature also correlates with the rotation rate. Finally, we discuss large and small scale coronal flaring on these stars.
This work is supported by NASA grants NAG5-3226, NAG5-2259, NAG5-1792, and HST grant GO-06068.01-94A.
If the author provided an email address or URL for general inquiries,
it is as follows: