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The Newly-Discovered γ Doradus Variables

Published online by Cambridge University Press:  12 April 2016

Anthony B. Kaye ,
Gerald Handler ,
Kevin Krisciunas ,
Ennio Poretti  and
Filippo M. Zerbi
Anthony B. Kaye
Affiliation:
Applied Theoretical and Computational Physics Division, Los Alamos National Laboratory X-TA, MS B-220, Los Alamos, New Mexico 87545, U.S.A.
Gerald Handler
Affiliation:
South African Astronomical Observatory, P.O. Box 9, Observatory 7935, West Cape, South Africa
Kevin Krisciunas
Affiliation:
Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195-1580, USA
Ennio Poretti
Affiliation:
Osservatorio Astronomico di Brera/Merate Via Bianchi 46, I-23807 Merate (Lc), Italy
Filippo M. Zerbi
Affiliation:
Osservatorio Astronomico di Brera/Merate Via Bianchi 46, I-23807 Merate (Lc), Italy

Abstract

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In this contribution we describe a new class of pulsating stars, the prototype of which is the bright, early F-type dwarf, γ Doradus. These stars typically have between 1 and 5 periods ranging from 0.4 to 3 d with photometric amplitudes up to 0ṃ1 in Johnson V. The mechanism for these observed variations is high-order, low-degree, nonradial, gravity-mode pulsation. A recent theoretical development describing a proposed driving mechanism for these new variables is discussed.

Type
Part 6. Variables Close to the Main Sequence
Information
International Astronomical Union Colloquium , Volume 176: The Impact of Large-Scale Surveys on Pulsating Star Research , 2000 , pp. 426 - 429
Copyright
Copyright © Astronomical Society of the Pacific 2000

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