Computer Science
Scientific paper
Jul 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984iue..prop.1906w&link_type=abstract
IUE Proposal ID #CCFSW
Computer Science
Scientific paper
We propose to obtain time-resolved, coordinated observations of magnetic flux and the associated coronal emission as well as chromospheric and transition region line emission for selected active chromospheric stars. The unique data to be obtained in this program will provide a crucial input to theories that describe the heating of stellar chromospheres and coronae. In essence, the results to be acquired through the observations will establish a preliminary empirical relationship between stellar photospheric magnetic field strengths and magnetic flux, stellar coronal field strength and emission, and stellar outer atmospheric line emission. We are presently utilizing demonstrated methods to directly detect magnetic fields on stellar surfaces. We are also able to deduce coronal field strengths from X-ray or radio observations. Magnetic results indicate the existence of strong (a few kilogauss) fields that may cover up to 80% of the stellar surface. Moreover, these fields are observed to rapidly (2-3 days) vary in surface coverage, suggesting a single large magnetic spot complex on only one hemisphere of the star. We therefore propose a coordinated IUE ground-based synoptic program to obtain chromospheric-transition region data (with IUE), and photospheric and coronal magnetic field and flux measurements (ground-based observations) for several stars that exhibit rapidly varying surface field coverages over their rotational periods. Our IUE observing pattern will primarily consist of low dispersion, SWP observations and high-dispersion, LWR exposures. These data will be obtained simultaneously (or near simultaneously) with ground-based optical, IR and radio observations. The ground-based data will be used to infer magnetic field strengths and flux in the photosphere and corona. We also require that the IUE shifts be scheduled every third day to insure that we examine the entire stellar surface over 10-15 day rotational periods. We require two separate observing periods in order to access all objects in the target list from ground-based observing sites.
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