Blue, white, and red ocean planets: Simulations of orbital variations in flux and polarization colors

• Published in: Astronomy and astrophysics (Berlin) 2019-06, Vol.626, p.A129
• Main Authors: Trees, V. J. H., Stam, D. M.
• Format: Article
• Language: English
• ISSN: 0004-6361; 1432-0746
• DOI: 10.1051/0004-6361/201935399

Context. An exoplanet’s habitability will depend strongly on the presence of liquid water. Flux and/or polarization measurements of starlight that is reflected by exoplanets could help to identify exo-oceans. Aims. We investigate which broadband spectral features in flux and polarization phase functions of reflected starlight uniquely identify exo-oceans. Methods. With an adding-doubling algorithm, we computed total fluxes F and polarized fluxes Q of starlight that is reflected by cloud-free and (partly) cloudy exoplanets, for wavelengths from 350 to 865 nm. The ocean surface has waves composed of Fresnel reflecting wave facets and whitecaps, and scattering within the water body is included. Results. Total flux F , polarized flux Q , and degree of polarization P of ocean planets change color from blue, through white, to red at phase angles α ranging from ~134° to ~108° for F , and from ~123° to ~157° for Q , with cloud coverage fraction f c increasing from 0.0 (cloud-free) to 1.0 (completely cloudy) for F , and to 0.98 for Q . The color change in P only occurs for f c ranging from 0.03 to 0.98, with the color crossing angle α ranging from ~88° to ~161°. The total flux F of a cloudy, zero surface albedo planet can also change color, and for f c = 0.0, an ocean planet’s F will not change color for surface pressures p s ≿ 8 bars. Polarized flux Q of a zero surface albedo planet does not change color for any f c . Conclusions. The color change of P of starlight reflected by an exoplanet, from blue, through white, to red with increasing α above 88°, appears to identify a (partly) cloudy exo-ocean. The color change of polarized flux Q with increasing α above 123° appears to uniquely identify an exo-ocean, independent of surface pressure or cloud fraction. At the color changing phase angle, the angular distance between a star and its planet is much larger than at the phase angle where the glint appears in reflected light. The color change in polarization thus offers better prospects for detecting an exo-ocean.