Computer Science
Scientific paper
Jul 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996hst..prop.6647v&link_type=abstract
HST Proposal ID #6647
Computer Science
Hst Proposal Id #6647 Cool Stars
Scientific paper
One of the major discoveries of the GHRS has been thedetection of bimodal structures and broad wings of the CIV1550 lines in some cool stars. In AB Doradus (Vilhu et al.95), for example, the quiescent (rotationally deconvolved)profile is well fitted by two Gaussians with roughly equalemission measures: a 'narrow' component with FWHM = 70 km/secand a broad one with FWHM = 330 km/sec. Qualitatively similarprofiles were found earlier in Capella (Linsky et al. 95), AUMic (Linsky and Wood, 94) and recently HR 1099 (Wood et al.95). These two distinct velocity fields may be related to theobserved two-temperature coronal structures and might becrucial in understanding how coronal heating takes place. Toput the idea into a more quantitative basis we shallobserve two solar type dwarfs ( Chi1 Ori = HD39587 and Sigma2 CrB =TZ CrB = HD146361) with medium and high activitylevels, respectively) using HRS/G160M during the 4 orbitsallocated (2 orbits for both targets). These data will becomplemented with solar spectra from the SUMER spectrometeron board SOHO. One expects the broad component to become broaderand more dominant with increasing activity level. Further, theline widths and intensities should correlate with the coronaltemperatures and emission measures, respectively. If this istrue, the energetic reservoir of the coronal heating lies inthe kinetic energies of these two velocity fields(microflaring regions on stellar surfaces).
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