Dynamics and Energy Balance in Stellar Transition Regions Cycle 2

Details Dynamics and Energy Balance in Stellar Transition Regions Cycle 2 Dynamics and Energy Balance in Stellar Transition Regions Cycle 2

Jul 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992hst..prop.3964l&link_type=abstract

HST Proposal ID #3964

Computer Science

Hst Proposal Id #3964

Scientific paper

Late-type stars with convective zones and magnetic fields have plasma above the photosphere heated to temperatures above 10,000 K. We will use the GHRS to study the dynamics, energy balance, and nonradiative heating rates in these hot regions for a sample of late-type stars spanning a range of spectral type and luminosity. We will study the dynamics of stellar transition regions by measuring the redshifts, indicative of downflows, with high precision in lines of C III, C IV, Si IV, and O IV. The energy balance and local heating rates in stellar transition regions will be derived from an emission measure analysis of emission line fluxes and electron densities inferred from density-sensitive line ratios. Cycle 0 observations of the RS CVn system Capella show that the GHRS can measure ALL of the UV intersystem lines of Si III, C III, O III, N III, O IV, and S IV, which are useful density diagnostics. These data may require atmospheric models with two components (quiet and active regions).

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