Atmospheric Lensing and Oblateness Effects During an Extrasolar Planetary Transit

Abstract

Future high precision photometric measurements of transiting extrasolar planets promise to tell us much about the nature of these systems. We examine how atmospheric lensing and (projected) planet oblateness/ellipticity modify transit light curves. The large density gradients expected in planet atmospheres can offset the unfavorably large observer-lens to source-lens distance ratio, and allow the existence of caustics. Under such conditions, starlight from all points in the planet's shadow is refracted into view producing a characteristic slowing down of the dimming at ingress (vice versa for egress). A search over several parameters, the planet radius etc., cannot produce a nonlensed transit light curve that can mimic a lensed light curve. The fractional change in the diminution of starlight is approximately the ratio of atmospheric scale height to planet radius, expected to be 1 % or less. Planet oblateness induces an asymmetry to the transit light curve about the point of minimum flux, depending on the planet orientation. The fractional asymmetry is around 0.5 % for a projected ellipticity of 10 %, independent of lensing. For favorable ratios of planet to star radius, the above effects are potentially observable with future space-based missions. This will allow us to constrain the planet shape, and its atmospheric scale height, density and refractive coefficient, providing information on its rotation, temperature and composition. For HD 209458b, the only currently known transiting extrasolar planet, caustics are absent because of the very small lens-source separation. Finally, we provide estimates of other variations to transit light curves that could be of comparable importance, including rings, satellites, stellar oscillations, star spots, and weather.