The Polarization Signature of Extrasolar Planets Transiting Cool Dwarfs

Abstract

We investigate the linear polarization in the light of extrasolar planetary systems that may arise as a result of an occultation of the star by a transiting planet. Such an occultation breaks any spherical symmetry over the projected stellar disk and thus results in a non-vanishing linear polarization. This polarization will furthermore vary as the occultation progresses. We present both analytical and numerical results for the occultation of G-K-M-T dwarf stars by planets with sizes ranging from the one of Earth to two times the size of Jupiter. We find that the occultation polarization may result in an observable signal and provide additional means to characterize various parameters of the system. A particularly interesting result is that, for the later spectral types (i.e., smaller stellar radii), this polarization signature may be observable even for Earth-like planets. This suggests polarization as a possible tool to detect such planets. Departs from symmetry around mid-transit in the time dependence of the polarization signature may provide an estimate of the orbital eccentricity.

arXiv comment27 pages, 12 figures

References in corpus (5)

• Detection of Thermal Emission from an Extrasolar Planet
• Infrared radiation from an extrasolar planet
• TrES-1: The Transiting Planet of a Bright K0V Star
• Photometric Light Curves and Polarization of Close-in Extrasolar Giant Planets
• Dust in the Photospheric Environment: Unified Cloudy Models of M, L, and T Dwarfs

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