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Title:
Solar-like Oscillations in α Centauri B
Authors:
Kjeldsen, Hans; Bedding, Timothy R.; Butler, R. Paul; Christensen-Dalsgaard, Jørgen; Kiss, Laszlo L.; McCarthy, Chris; Marcy, Geoffrey W.; Tinney, Christopher G.; Wright, Jason T.
Affiliation:
AA(Department of Physics and Astronomy, University of Aarhus, DK-8000 Aarhus C, Denmark; ), AB(School of Physics A28, University of Sydney, NSW 2006, Australia; ), AC(Carnegie Institution of Washington, Department of Terrestrial Magnetism, 5241 Broad Branch Road NW, Washington, DC 20015-1305 ), AD(Department of Physics and Astronomy, University of Aarhus, DK-8000 Aarhus C, Denmark; .), AE(School of Physics A28, University of Sydney, NSW 2006, Australia; .), AF(Carnegie Institution of Washington, Department of Terrestrial Magnetism, 5241 Broad Branch Road NW, Washington, DC 20015-1305 .), AG(Department of Astronomy, University of California, Berkeley, CA 94720; and Department of Physics and Astronomy, San Francisco, CA 94132; .), AH(Anglo-Australian Observatory, P.O. Box 296, Epping, NSW 1710, Australia; .), AI(Department of Astronomy, University of California, Berkeley, CA 94720; and Department of Physics and Astronomy, San Francisco, CA 94132; .)
Publication:
The Astrophysical Journal, Volume 635, Issue 2, pp. 1281-1290. (ApJ Homepage)
Publication Date:
12/2005
Origin:
UCP
ApJ Keywords:
Stars: Individual: Constellation Name: α Centauri A, Stars: Individual: Constellation Name: α Centauri B, Stars: Individual: Constellation Name: β Hydri, stars: individual (δ Pavonis), Stars: Oscillations, Sun: Helioseismology
DOI:
10.1086/497530
Bibliographic Code:
2005ApJ...635.1281K

Abstract

We have made velocity observations of the star α Centauri B from two sites, allowing us to identify 37 oscillation modes with l=0-3. Fitting to these modes gives the large and small frequency separations as a function of frequency. The mode lifetime, as measured from the scatter of the oscillation frequencies about a smooth trend, is similar to that in the Sun. Limited observations of the star δ Pav show oscillations centered at 2.3 mHz, with peak amplitudes close to solar. We introduce a new method of measuring oscillation amplitudes from heavily smoothed power density spectra, from which we estimated amplitudes for α Cen α and B, β Hyi, δ Pav, and the Sun. We point out that the oscillation amplitudes may depend on which spectral lines are used for the velocity measurements.

Based on observations collected at the European Southern Observatory, Paranal, Chile (ESO Programme 71.D-0618).

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