A Semi-Empirical Model of the Structured Wind of 32 Cygni

Details A Semi-Empirical Model of the Structured Wind of 32 Cygni A Semi-Empirical Model of the Structured Wind of 32 Cygni

Jul 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999hst..prop.8376b&link_type=abstract

HST Proposal ID #8376

Physics

Hst Proposal Id #8376 Cool Stars

Scientific paper

I propose to construct a semi-empirical wind model of the supergiant primary of the eclipsing binary 32 Cygni {K5 Iab + B6 V}, using archival HST/GHRS observations obtained at 6 epochs around the December 1996 eclipse. From these observations, I will empirically determine the hydrogen column density structure along each line of sight to the early-type secondary star using the Tau-v method. I will use codes developed for the analysis of HST/GHRS observations of the similar binary Zeta Aur. Successful Tau-v inversion of the UV absorption line profiles requires high spectral resolution and high S/N, limiting the useful data to those from HST/GHRS. Recent HST/GHRS observations of Zeta Aur in Cycles 2 & 5, and of 32 Cyg in Cycle 6, have shown the primary's wind has discrete structure along some lines of sight. However, global flux diagnostics such as UV emission line profiles and radio continuum fluxes, show that the globally-averaged wind is only slightly variable in time, implying most of the observed variability in the absorption lines is on small scales. Semi- empirical mean models of these winds are useful. Therefore, I will construct a semi-empirical model of the mean density, temperature, and velocity structure of the wind of 32 Cygni. I will also do a radial velocity analysis of the GHRS spectra of 32 Cyg, in conjunction with eclipse and flux constraints, to obtain accurate masses and radii of the 32 Cyg stars.

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