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Title:
Photometry and Spectroscopy of 11 γ Doradus Stars
Authors:
Henry, Gregory W.; Fekel, Francis C.; Henry, Stephen M.
Affiliation:
AA(Center of Excellence in Information Systems, Tennessee State University, Nashville, TN, USA ), AB(Center of Excellence in Information Systems, Tennessee State University, Nashville, TN, USA ; Visiting Astronomer, Kitt Peak National Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under cooperative agreement with the National Science Foundation ), AC(Center of Excellence in Information Systems, Tennessee State University, Nashville, TN, USA ; Current address: Department of Mathematical Sciences, Clemson University, Clemson, SC, USA)
Publication:
The Astronomical Journal, Volume 133, Issue 4, pp. 1421-1440 (2007). (AJ Homepage)
Publication Date:
04/2007
Origin:
IOP
DOI:
10.1086/511820
Bibliographic Code:
2007AJ....133.1421H

Abstract

We have used precise photometric and high-dispersion spectroscopic observations to study 11 γ Doradus stars, 10 of them newly confirmed. Only five of these 11 γ Doradus stars appear to be single; two are primaries of double-lined spectroscopic binaries, one is the secondary of a double-lined binary, two are primaries of visual binaries and, in the case of the double-lined binary (HD 86371), either or both components could be a pulsating γ Doradus star. We have determined a preliminary orbital period of 5.32 days for the double-lined binary HD 41547. Several of the stars show spectroscopic line-profile and low-amplitude radial velocity variability indicative of pulsation. All 11 stars are photometrically variable with amplitudes between 4 and 94 mmag in Johnson B and periods between 0.38 and 1.86 days. The 11 stars have between two and five independent periods. The variability at all periods approximates a sinusoid. We provide a new tabulation of all 66 γ Doradus stars confirmed to date and list some of their properties. All are dwarfs or subgiants and lie within a well-defined region of the H-R diagram that overlaps the cool edge of the δ Scuti instability strip. Four of the new γ Doradus variables from this paper also lie within the δ Scuti instability strip but do not exhibit the additional higher frequency variability typical of δ Scuti stars. Among the 66 confirmed γ Doradus variables, we find no correlation between the period of the strongest pulsation mode and the (B - V) color index, absolute magnitude, or luminosity.
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