SUMMARY OF PROPOSAL 62022
UNIVERSITY OF HAWAII
2680 WOODLAWN DRIVE
HI USA 96822
Tel: 808-956-6317 Fax: 808-988-2790
Medium: CD ROM
FIP, FIT, OR MAD?
ABSTRACTASCA and EUVE spectra of active late-type stars imply that Fe and other medium-Z elements may be 2-10 times less abundant in the coronae of these stars than in their photospheres (the MAD effect). These deficiencies may be related to the solar FIP effect, in which Fe and other low First Ionization Potential elements appear enriched in the solar corona over their photospheric values. The FIP effect is time variable. Here we request time with ASCA to measure the coronal abundances of the active K0-2 III star, 29 Dra, as a function of stellar longitude over its 31-day rotation cycle. Our goal is to learn whether the coronal abundances, and hence coronal magnetic structure, vary across the surface of 29 Dra in phase with the motion of dark starspots across the disk.
|CO-I NAME ||INSTITUTE ||COUNTRY |
| KULINDER PAL SINGH||TIFR||INDIA|
| NICHOLAS WHITE||NASA/GSFC||USA|
|TARGET NAME||PRI||RA||DEC||TIME||TC||OFF||GIS||SIS CNT||OBS|
|1)29 DR DRA|| 1||263.1717|| 74.2272|| 60 ks||Y||Y||P||0.97000||3|
TARGET 129 DRA IS WITHIN VIEW OF ASCA THE ENTIRE YEAR
Min. Interval: 700.000ksecMax. Interval: 1000.000 ksec