The Red Edge of the ZZ Ceti Instability Strip

Details The Red Edge of the ZZ Ceti Instability Strip The Red Edge of the ZZ Ceti Instability Strip

Jul 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994hst..prop.5314v&link_type=abstract

HST Proposal ID #5314

Physics

Hst Proposal Id #5314 Cool Stars Pulsating 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 and the detailed structure of the outer stellar layers. 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 and should ultimately allow an accuracy of 200 K. Observations for G117-B15A (defining the hot edge of the instability strip) have been obtained in Nov. 92. In this project, we propose to observe BPM30551, one of the coolest ZZ Ceti stars.

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