Welsh, William F., Orosz, Jerome A., Aerts, Conny, Brown, Timothy M., Brugamyer, Erik, Cochran, William D., Gilliland, Ronald L., Guzik, Joyce Ann, Kurtz, Donald Wayne, Latham, David W., Marcy, Geoffrey W., Quinn, Samuel N., Zima, Wolfgang, Allen, Christopher, Batalha, Natalie M., Bryson, Steve, Buchhave, Lars A., Caldwell, Douglas A., Gautier, Thomas N., Howell, Steve B., Kinemuchi, K., Ibrahim, Khadeejah A., Isaacson, Howard, Jenkins, Jon M., Prsa, Andrej, Still, Martin, Street, Rachel, Wohler, Bill, Koch, David G. and Borucki, William J. (2011) KOI-54: THEKEPLERDISCOVERY OF TIDALLY EXCITED PULSATIONS AND BRIGHTENINGS IN A HIGHLY ECCENTRIC BINARY. The Astrophysical Journal Supplement Series, 197 (1). p. 4. ISSN 0067-0049
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Official URL: http://dx.doi.org/10.1088/0067-0049/197/1/4
Kepler observations of the star HD 187091 (KIC 8112039, hereafter KOI-54) revealed a remarkable light curve exhibiting sharp periodic brightening events every 41.8 days with a superimposed set of oscillations forming a beating pattern in phase with the brightenings. Spectroscopic observations revealed that this is a binary star with a highly eccentric orbit, e = 0.83. We are able to match the Kepler light curve and radial velocities with a nearly face-on (i = 5fdg5) binary star model in which the brightening events are caused by tidal distortion and irradiation of nearly identical A stars during their close periastron passage. The two dominant oscillations in the light curve, responsible for the beating pattern, have frequencies that are the 91st and 90th harmonic of the orbital frequency. The power spectrum of the light curve, after removing the binary star brightening component, reveals a large number of pulsations, 30 of which have a signal-to-noise ratio gsim7. Nearly all of these pulsations have frequencies that are either integer multiples of the orbital frequency or are tidally split multiples of the orbital frequency. This pattern of frequencies unambiguously establishes the pulsations as resonances between the dynamic tides at periastron and the free oscillation modes of one or both of the stars. KOI-54 is only the fourth star to show such a phenomenon and is by far the richest in terms of excited modes.
|Uncontrolled Keywords (separate with ;):||binaries: close; binaries: spectroscopic; stars: individual (KID 8112039, HD 187091, 2MASS J19461553+4356513); stars: oscillations; stars: variables: general|
|Subjects:||Q Science > QC Physics|
|Schools:||College of Science and Technology > School of Computing Engineering & Physical Sciences > Jeremiah Horrocks Institute|
|Deposited By:||Helen Cooper|
|Deposited On:||22 Mar 2012 14:13|
|Last Modified:||05 Dec 2012 11:45|
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