K Giant Stars Observed with WIRE: Lifetimes and Amplitudes

Details K Giant Stars Observed with WIRE: Lifetimes and Amplitudes K Giant Stars Observed with WIRE: Lifetimes and Amplitudes

May 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...210.8805p&link_type=abstract

American Astronomical Society Meeting 210, #88.05; Bulletin of the American Astronomical Society, Vol. 39, p.201

Astronomy and Astrophysics

Astronomy

Scientific paper

Following the failure of the main experiment on board the Wide-Field Infrared Explorer satellite (WIRE), the on-board star camera was used as the first space-based asteroseismology experiment. From May 1999 through November 2006, well over 200 targets were observed for periods ranging up to 40+ days. The typical noise level (measured at a frequency of 10 mHz) of these observations was <5 ppm for a 3rd magnitude star.
WIRE operated in a mode where it observed a single primary and up to 4 serendipitous secondary targets simultaneously. Among the primary targets observed were some 30 K giants, and K giants constitute the plurality of the secondary targets. While data from some of these have already been analyzed and published (e.g., Alpha Boo, by Retter et al. 2003), most have not, and we begin to address this lack here. These stars have complex oscillation spectra, due to a combination of long oscillation periods and short mode lifetimes, which leads to poorly resolved power spectra. Accordingly, the unique nature of the WIRE dataset, which combines high precision, long uninterrupted observing runs, and a large unbiased sample, allows us to begin to understand the behavior of these common objects. In particular, we determine frequency envelopes, amplitudes, and damping times.

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