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We present results of numerical simulations of the flux (irradiance), F, andthe degree of polarization (i.e. the ratio of polarized to total flux), P, oflight that is reflected by Earth-like extrasolar planets orbiting solar-typestars, as functions of the wavelength (from 0.3 to 1.0 micron, with 0.001micron spectral resolution) and as functions of the planetary phase angle. Weuse different surface coverages for our model planets, including vegetation anda Fresnel reflecting ocean, and clear and cloudy atmospheres. Ouradding-doubling radiative transfer algorithm, which fully includes multiplescattering and polarization, handles horizontally homogeneous planets only; wesimulate fluxes and polarization of horizontally inhomogeneous planets byweighting results for homogeneous planets. Like the flux, F, the degree ofpolarization, P, of the reflected starlight is shown to depend strongly on thephase angle, on the composition and structure of the planetary atmosphere, onthe reflective properties of the underlying surface, and on the wavelength, inparticular in wavelength regions with gaseous absorption bands. The sensitivityof P to a planet's physical properties appears to be different than that of F.Combining flux with polarization observations thus makes for a strong tool forcharacterizing extrasolar planets. The calculated total and polarized fluxeswill be made available through the CDS.

Spectropolarimetric signatures of Earth-like extrasolar planets