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Mapping the ZZ Ceti Instability Strip Discovery of 6 New Pulsators
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Accepted for Publication in the Astronomical Journal
Preprint typeset using LATEX style emulateapj v. 12/14/05
MAPPING THE ZZ CETI INSTABILITY STRIP: DISCOVERY OF 6 NEW PULSATORS
A. Gianninas, P. Bergeron, and G. Fontaine
De?partement de Physique, Universite? de Montre?al, C.P. 6128, Succ. Centre-Ville, Montre?al, Que?bec, Canada, H3C 3J7.
Accepted for Publication in the Astronomical Journal
ABSTRACT
As part of an ongoing program to map better the empirical instability strip of pulsating ZZ Ceti
white dwarfs, we present a brief progress report based on our last observing season. We discuss here
high-speed photometric measurements for 6 new pulsators. These stars were selected on the basis of
preliminary measurements of their effective temperature and surface gravity that placed them inside
or near the known ZZ Ceti instability strip. We also report detection limits for a number of DA white
dwarfs that showed no sign of variability. Finally, we revisit the ZZ Ceti star G232-38 for which we
obtained improved high-speed photometry.
Subject headings: stars : oscillations – white dwarfs
1. MOTIVATION
The ZZ Ceti stars are pulsating white dwarfs whose
optical spectra are dominated by hydrogen lines (DA
stars). They are found in a very well defined region in the
Teff-log g plane, known as the ZZ Ceti instability strip.
They exhibit pulsation periods in the range 100-1400 s,
corresponding to low degree gravity-mode oscillations.
The detected pulsation modes have amplitudes that are
found in the range from a few millimagnitudes in the
low-amplitude pulsators to a fraction of a magnitude in
the largest amplitude ones. The ZZ Ceti stars show some
remarkable trends, although there are a few exceptions.
For instance, the cooler pulsators tend to show longer
periods and larger amplitudes. Also, for a given effective
temperature, the observed periods tend to be longer for
lower gravity objects.
Since the early 90
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