Computer Science
Scientific paper
Jul 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995hst..prop.6069b&link_type=abstract
HST Proposal ID #6069
Computer Science
Hst Proposal Id #6069 Cool Stars
Scientific paper
Zeta Aur is a long period (972 day) binary containing a K supergiant and a B dwarf. In Cycle 2 we observed with the GHRS the last eclipse of the B dwarf by the K star's wind and chromosphere. An analysis of these spectra have lead us to a significantly improved understanding of how the K star wind flows from the binary system. A low density stagnation region forms in front of the binary system which periodically becomes an H II region as the B star moves in front of the K star, and the wind shows much lower turbulence velocities than previously inferred from IUE data. Unfortunately the HST data have also emphasised just how complex this process really is and the high degree of asymmetry involved. The wind outflow and orbital velocity are comparable and this leads to accelerated and stagnant zones in the flow, which is itself modulated by the varying separation of the two stars. We propose to observe during and near the next eclipse centered on December 1 1995, so that new observations can be obtained to help answer some of the questions raised as a result of our analysis and modeling. The main objectives of this proposal are to (1) measure the turbulence and N_e of the K star chromosphere during eclipse, (2) determine the stability of the system from orbit-to-orbit, (3) measure the symmetry of the K star atmosphere, (4) determine the ISM column density and reddening, and (5) measure the turbulence in the K star wind.
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