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V. Strelnitski (Maria Mitchell Obs.), T. Mazeh (The U. of Tel-Aviv), C. Peterson (Georgetown U. & Maria Mitchell Obs.)
Detection of spectral lines from an extrasolar planet would allow for determining the true value of the planet's mass and would give valuable information about its chemical composition. We investigate the principle possibility of detectable maser/laser amplification of certain spectral lines in the atmospheres of giant extrasolar planets close to their parent stars. Rates of possible radiative, collisional, and chemical pumping mechanisms are estimated. Upper limits for the flux density in the amplified line are obtained for optimal positions of the planet with respect to the observer. We show that lines in the microwave domain are most prospective for the current state of observational technology. A list of the most prospective molecules and transitions is presented. This project was partially supported by the NSF/REU grant AST-9820555.
The author(s) of this abstract have provided an email address for comments about the abstract: vladimir@mmo.org