Exoplanet albedo spectra and colors as a function of orbital phase, separation, and metallicity

Details Exoplanet albedo spectra and colors as a function of orbital phase, separation, and metallicity Exoplanet albedo spectra and colors as a function of orbital phase, separation, and metallicity

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufm.b13b0513c&link_type=abstract

American Geophysical Union, Fall Meeting 2009, abstract #B13B-0513

Biology

[0343] Atmospheric Composition And Structure / Planetary Atmospheres, [5210] Planetary Sciences: Astrobiology / Planetary Atmospheres, Clouds, And Hazes, [5704] Planetary Sciences: Fluid Planets / Atmospheres, [6296] Planetary Sciences: Solar System Objects / Extra-Solar Planets

Scientific paper

In this work, we model how exoplanet albedo spectra and colors change as a function of orbital phase, separation, and metallicity for Jupiter and Neptune analogs from 0.35 to 5 microns. These reflected light radiative transfer simulations model albedo changes due to varying phase angle and disk illumination, which are a function of planetary phase. Simulations are performed at all orbital phase angles for Jupiters with 1 and 3 times solar metallicity at separations of 1, 2.5, 5, and 10 AU as well as for Neptunes with 10 and 30 times solar metallicity. The resulting planetary albedos, scaled by stellar spectra, are useful for understanding the range of variability in observations of reflected light and for deriving direct imaging instrument requirements. These results are also used to compute the colors of exoplanets for comparison with direct imaging observations.

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