The Search for Extra-Solar Planets

Details The Search for Extra-Solar Planets The Search for Extra-Solar Planets

Oct 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aipc..795r.215s&link_type=abstract

WOMEN IN PHYSICS: 2nd IUPAP International Conference on Women in Physics. AIP Conference Proceedings, Volume 795, pp. 215-215 (

Physics

Extrasolar Planets, Astronomical Photometry, Brightness, Mass, Stellar Dimensions, Stars

Scientific paper

We propose a method to distinguish between planetary and stellar companions to stars that present a periodic decrease in brightness, interpreted as a transit. Lightcurves from a total of 133 stars from the Optical Gravitational Lensing Experiment (OGLE) were fitted by the model, which simulates planetary transits using an opaque disk in front of a white-light image of the sun. The simulation results yield the orbital radius (adopting circular orbit) in units of stellar radii, the orbit inclination angle, and the ratio of the planet to the star radii, taking as input the orbital period provided by the OGLE data. Using a mass-radius relation for main sequence stars, it was possible to estimate values for stellar radius and mass and, therefore, absolute values for the radii of the companion and the orbit. This method was successfully tested with the stars HD 209458, OGLE-TR-10, 56, 111, 113, and 132 data. The method consists of selecting as planetary candidates only those objects with primary masses < 2Msolar, representative of the OGLE solar type stars, and secondaries with radius less than 1.5 Jupiter radius. We propose a selection of 20 planetary companions for high-resolution spectroscopy follow up.

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