Luminosity and Detectability of Young Giant Planets

Details Luminosity and Detectability of Young Giant Planets Luminosity and Detectability of Young Giant Planets

May 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...21010202f&link_type=abstract

American Astronomical Society Meeting 210, #102.02; Bulletin of the American Astronomical Society, Vol. 39, p.229

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I will present new thermal evolution models for giant planets that couple one implementation of the core accretion formation mechanism to their subsequent evolution. Traditional thermal evolution models, which aim to predict the luminosity of giant planets, employ arbitrary initial conditions selected more for computational expediency than physical accuracy. We find these previous models may overestimate the luminosity of "young Jupiters" by a factor of a few to 100. The post-formation luminosity is quite sensitive to initial conditions and young giant planets may be smaller, cooler, and fainter than previously appreciated. I will also present model infrared spectra and colors for these planets, which are computed using an atmospheric metallicity enhancement similar to Jupiter and Saturn. These results have important consequences both for detection strategies and for assigning masses to young Jovian planets based on their luminosity and spectra.

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