The ZZ Ceti Instability Strip and Stellar Convection

Details The ZZ Ceti Instability Strip and Stellar Convection The ZZ Ceti Instability Strip and Stellar Convection

Jul 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995hst..prop.6022k&link_type=abstract

HST Proposal ID #6022

Physics

Hst Proposal Id #6022 Hot Stars

Scientific paper

ZZ Ceti stars are variable white dwarfs of spectral type DA. The theoretically predicted instability strip depends on several uncertain assumptions, most importantly the efficiency of convective energy transport. Empirical determinations from optical spectra are not as accurate as desirable, because the Balmer lines reach maximum strengths within the instability strip and vary only little with temperature. The UV spectrum is much better suited since we have recently improved the quantitative description of the quasi-molecular satellite features, that vary strongly with temperature. The analysis of G117-B15A (in several studies defining the hot edge of the instability strip), which was observed by us in Cycle 2 confirms that an accuracy of 200 K or better can be achieved. It also shows that convection must be more efficient than normally assumed, and that the temperature of G117-B15A is 1000 K lower than determined previously, raising the question that perhaps GD165, the last remaining hot edge candidate with relatively uncertain temperature determination, defines the blue edge.

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