The long term period stability of the hot DBV white dwarf EC20058-5234

Details The long term period stability of the hot DBV white dwarf EC20058-5234 The long term period stability of the hot DBV white dwarf EC20058-5234

Jun 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009jphcs.172a2070s&link_type=abstract

Journal of Physics: Conference Series, Volume 172, Issue 1, pp. 012070 (2009).

Physics

1

Scientific paper

Since its discovery over a decade ago, the helium atmosphere pulsator EC 20058-5234 (QU Tel) has been studied both spectroscopically, and also extensively using the techniques of time-series photometry. Model atmosphere fits to quality spectra obtained with one of the Magellan telescopes have confirmed its status as the hottest know DBV, so it currently defines the blue edge of the DBV instability strip. Extensive time-series photometry (primarily from Mt John in NZ but also including a Whole Earth Telescope run) clearly demonstrates that this white dwarf is a very stable low amplitude pulsator. This is consistent with its position at or near the blue edge of the DBV instability strip. However, of perhaps greater significance is the possibility of employing this period stability to look for a period change that can be sourced to the predicted neutrino-dominated cooling of the hot white dwarfs. This paper provides an update on this work.

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