AAS 201st Meeting, January, 2003
Session 21. Planetary Systems: Instrumentation and Surveys
Poster, Monday, January 6, 2003, 9:20am-6:30pm, Exhibit Hall AB

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[21.05] Extrasolar Planet Transit Light Curves and a Method to Select the Best Planet Candidates for Mass Follow-up

S. Seager (Carnegie Institution of Washington), G. Mallen-Ornelas (Harvard-Smithsonian Center for Astrophysics)

A unique analytical solution of planet and star parameters can be derived from an extrasolar planet transit light curve under a number of assumptions. This analytical solution can be used in several different applications to choose the best planet transit candidates for radial velocity follow-up measurements, with or without a known spectral type. First, there is an analytic solution that allows a quick parameter estimate, in particular of planet radius. Second, the stellar density can be uniquely derived from the transit light curve alone. The stellar density can be used to immediately rule out a giant star (and hence a much larger than planetary companion) and can also be used to put an upper limit on the stellar and planet radius even considering slightly evolved stars. Third, the presence of an additional fully blended star that contaminates an eclipsing system to mimic a planet transit can be largely ruled out from the transit light curve given a spectral type for the central star. Fourth, the period can be estimated from a single-transit light curve and a measured spectral type. To use these applications in practice, the photometric precision and time sampling of the light curve must be high (better than 0.005 mag precision and 5 minute time sampling).

This work was supported by the W. M. Keck Foundation and the Carnegie Institution of Washington.

If you would like more information about this abstract, please follow the link to http://www.ciw.edu/seager/. This link was provided by the author. When you follow it, you will leave the Web site for this meeting; to return, you should use the Back comand on your browser.

The author(s) of this abstract have provided an email address for comments about the abstract: seager@dtm.ciw.edu

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