Detectability of Oort cloud objects using Kepler

TL;DR

This paper evaluates Kepler's potential to detect Oort Cloud objects via star occultations, providing estimates of detection rates, and discusses statistical methods to verify and analyze these events, informing future exoplanet search strategies.

Contribution

It introduces a method to estimate occultation detection rates of Oort Cloud objects by Kepler and proposes statistical techniques to confirm and analyze such events.

Findings

Kepler could detect up to ~100 Oort Cloud occultations

Detection likelihood depends on Oort Cloud mass and object size distribution

Kepler unlikely to detect Kuiper Belt or main belt occultations

Abstract

The size distribution and total mass of objects in the Oort Cloud have important implications to the theory of planets formation, including the properties of, and the processes taking place in the early solar system. We discuss the potential of space missions like Kepler and CoRoT, designed to discover transiting exo-planets, to detect Oort Cloud, Kuiper Belt and main belt objects by occultations of background stars. Relying on published dynamical estimates of the content of the Oort Cloud, we find that Kepler's main program is expected to detect between 0 and ~100 occultation events by deca-kilometer-sized Oort Cloud objects. The occultations rate depends on the mass of the Oort cloud, the distance to its "inner edge", and the size distribution of its objects. In contrast, Kepler is unlikely to find occultations by Kuiper Belt or main belt asteroids, mainly due to the fact that it is observing a high ecliptic latitude field. Occultations by Solar System objects will appear as a photometric deviation in a single measurement, implying that the information regarding the time scale and light-curve shape of each event is lost. We present statistical methods that have the potential to verify the authenticity of occultation events by Solar System objects, to estimate the distance to the occulting population, and to constrain their size distribution. Our results are useful for planning of future space-based exo-planet searches in a way that will maximize the probability of detecting solar system objects, without hampering the main science goals.