Epsilon Eri: Structure and Non-Thermal Heating

Details Epsilon Eri: Structure and Non-Thermal Heating Epsilon Eri: Structure and Non-Thermal Heating

Dec 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997hst..prop.7479j&link_type=abstract

HST Proposal ID #7479

Physics

Hst Proposal Id #7479 Cool Stars

Scientific paper

Epsilon Eri {K2 V} is the most active single K dwarf within 10 pc of the Sun, and its proximity {3.3 pc} allows studies of emission line profiles as well as fluxes. We have observed Epsilon Eri with IUE, at Lo and Hi resolution, and with ROSAT {PSPC and WFC}, and have used these spectra to make models of the structure of the transition region and corona, and to establish the non-thermal energy requirements. The accuracy of the current models is limited by the available line widths and the electron density {Ne} derived from the Si III line at 1892 Angstrom. The aim of the observations with STIS is to measure the profiles and fluxes of lines formed in the chromosphere and transition region, including several lines which can yield Ne. Significantly improved models from the photosphere to the corona could then be obtained, to investigate the non-thermal heating. With Ne determined from line ratios there are sufficient lines of C and Si ions to find the C/Si abundance ratio, for co mparison with photospheric values. Epsilon Eri has a measured magnetic field and area filling factor, and together with xi Boo A {G8 V} {our Cycle 5 observations} and the Sun {G2 V}, the observations will aid our understanding of the observed correlations between line fluxes, magnetic fluxes and activity indicators such as the rotation period and the Rossby number.

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