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Pulsating Red Giants: New Results

Published online by Cambridge University Press:  12 April 2016

J.R. Percy ,
A.G. Bakos ,
H. Dunlop ,
A. Hussain ,
L. Kassim ,
R. Kastrukoff ,
Z. Nyssa ,
J.B. Wilson  and
G.W. Henry
J.R. Percy
Affiliation:
Department of Astronomy and Astrophysics, University of Toronto, Toronto ONCanadaM5S 3H8; e-mail:jpercy@erin.utoronto.ca
A.G. Bakos
Affiliation:
Department of Astronomy and Astrophysics, University of Toronto, Toronto ONCanadaM5S 3H8; e-mail:jpercy@erin.utoronto.ca
H. Dunlop
Affiliation:
Department of Astronomy and Astrophysics, University of Toronto, Toronto ONCanadaM5S 3H8; e-mail:jpercy@erin.utoronto.ca
A. Hussain
Affiliation:
Department of Astronomy and Astrophysics, University of Toronto, Toronto ONCanadaM5S 3H8; e-mail:jpercy@erin.utoronto.ca
L. Kassim
Affiliation:
Department of Astronomy and Astrophysics, University of Toronto, Toronto ONCanadaM5S 3H8; e-mail:jpercy@erin.utoronto.ca
R. Kastrukoff
Affiliation:
Department of Astronomy and Astrophysics, University of Toronto, Toronto ONCanadaM5S 3H8; e-mail:jpercy@erin.utoronto.ca
Z. Nyssa
Affiliation:
Department of Astronomy and Astrophysics, University of Toronto, Toronto ONCanadaM5S 3H8; e-mail:jpercy@erin.utoronto.ca
J.B. Wilson
Affiliation:
Department of Astronomy and Astrophysics, University of Toronto, Toronto ONCanadaM5S 3H8; e-mail:jpercy@erin.utoronto.ca
G.W. Henry
Affiliation:
Tennessee State University, Nashville TN 37203-3401; e-mail:henry@schwab.tsuniv.edu

Abstract

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We have (1) accumulated long-term (up to 15 years) photoelectric photometry of 76 bright pulsating red giants (PRGs) and related stars, with V amplitudes of 0.04 to ≥ 1 magnitude; (2) used a variety of techniques, including autocorrelation, to determine both “short” radial pulsation periods, and long secondary periods; (3) determined pulsation modes using the Q-value method; the modes range from fundamental to second overtone, independent of temperature; (4) tested wavelet analysis on small-amplitude PRGs; (5) made a special study of PRGs with amplitudes less than 0.1 magnitude; and (6) called further attention to the problem of the long secondary periods of these stars. Our studies provide a “model” for the analysis and interpretation of larger, fainter surveys such as MACHO and OGLE.

Type
Part 5. Mass Loss in Pulsating Stars
Information
International Astronomical Union Colloquium , Volume 185: Radial and Nonradial Pulsations as Probes of Stellar Physics , 2002 , pp. 562 - 565
Copyright
Copyright © Astronomical Society of the Pacific 2002

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