Brightness variations of an extrasolar giant planet rotating around its central star

Details Brightness variations of an extrasolar giant planet rotating around its central star Brightness variations of an extrasolar giant planet rotating around its central star

Oct 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002kfnt...18..419v&link_type=abstract

Kinematika i Fizika Nebesnykh Tel, vol. 18, no. 5, p. 419-432.

Physics

1

Scientific paper

Extrasolar giant planets (EGPs) were discovered around 65 stars (visual magnitude 4m-8m) in the last seven years. Almost all information on them was derived from precise measurements of radial velocities. The mass-radius ratio for EGP orbiting the star HD 209458 is known to be R/M = 1.55/0.69(RJ/MJ) = 2.25(RJ/MJ). This ratio enabled us to estimate magnitudes of EGPs around 65 stars. These magnitudes lie between 25.1m and 12.8m. The planet's contribution is 0.003-0.047% of the star radiation for 21 stars. Therefore, the systems of this kind can be accessible for photometric observations. The planets orbiting the stars τ Boo, HD 121504, HD 217107, HD 187123, HD 209458, HD 83443, HD 75289, 51 Peg, and HD 46375 are most suitable for these observations.

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