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We have searched Microvariability and Oscillations of STars (MOST) satellitephotometry obtained in 2004, 2005, and 2007 of the solar-type star HD 209458for Trojan asteroid swarms dynamically coupled with the system's transiting"hot Jupiter" HD 209458b. Observations of the presence and nature of asteroidsaround other stars would provide unique constraints on migration models ofexoplanetary systems. Our results set an upper limit on the optical depth ofTrojans in the HD 209458 system that can be used to guide current and futuresearches of similar systems by upcoming missions. Using cross-correlationmethods with artificial signals implanted in the data, we find that ourdetection limit corresponds to a relative Trojan transit depth of 1\times10-4,equivalent to ~1 lunar mass of asteroids, assuming power-law Trojan sizedistributions similar to Jupiter's Trojans in our solar system. We confirm withdynamical interpretations that some asteroids could have migrated inward withthe planet to its current orbit at 0.045 AU, and that the Yarkovsky effect isineffective at eliminating objects of > 1 m in size. However, using numericalmodels of collisional evolution we find that, due to high relative speeds inthis confined Trojan environment, collisions destroy the vast majority of theasteroids in <10 Myr. Our modeling indicates that the best candidates to searchfor exoTrojan swarms in 1:1 mean resonance orbits with "hot Jupiters" are youngsystems (ages of about 1 Myr or less). Years of Kepler satellite monitoring ofsuch a system could detect an asteroid swarm with a predicted transit depth of3\times10-7.

Searching for Trojan Asteroids in the HD 209458 System: Space-based MOST Photometry and Dynamical Modeling