Transit Detectability of Ring Systems Around Extrasolar Giant Planets

Details Transit Detectability of Ring Systems Around Extrasolar Giant Planets Transit Detectability of Ring Systems Around Extrasolar Giant Planets

2004-09-21

arxiv.org/abs/astro-ph/0409506v2

Astrophys.J. 616 (2004) 1193-1203

Astronomy and Astrophysics

Astrophysics

13 pages, to appear in the 2004 December 1 Astrophysical Journal

Scientific paper

10.1086/425067

We investigate whether rings around extrasolar planets could be detected from those planets' transit lightcurves. To this end we develop a basic theoretical framework for calculating and interpreting the lightcurves of ringed planet transits based on the existing framework used for stellar occultations, a technique which has been effective for discovering and probing ring systems in the solar system. We find that the detectability of large, Saturn-like ring systems is largest during ingress and egress, and that reasonable photometric precisions of $\sim 1-3 \times 10^{-4}$ with 15-minute time resolution should be sufficient to discover such ring systems. For some ring particle sizes, diffraction around individual particles leads to a detectable level of forward-scattering that can be used to measure modal ring particle diameters. An initial census of large ring systems can be carried out using high-precision follow-up observations of detected transits and by the upcoming NASA \emph{Kepler} mission. The distribution of ring systems as a function of stellar age and as a function of planetary semimajor axis will provide empirical evidence to help constrain how rings form and how long rings last.

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