Planet Formation at Wide Separations: Constraints from HR 8799

Details Planet Formation at Wide Separations: Constraints from HR 8799 Planet Formation at Wide Separations: Constraints from HR 8799

Sep 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009dps....41.0506m&link_type=abstract

American Astronomical Society, DPS meeting #41, #5.06

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Scientific paper

The three gas giants directly-imaged orbiting HR 8799 comprise the first planetary system detected at wide separations around a main sequence star. Core accretion scenarios, already strained at the outer limits of our solar system, have difficulty explaining planet formation at the larger distances of the HR 8799 planets, even around a central A star. Formation by gravitational instability (GI) is most plausible for massive planets at large separations. We demonstrate that for GI to form the planets around HR 8799, the protoplanetary disk must have passed through a fine-tuned region of parameter space at its transition from the Class I to the Class II phase. Orbital stability requirements imply that the HR 8799 planets occupy at least one and possibly two mean motion resonances, suggesting that they migrated toward one another and may have migrated substantially from their formation locations. We will discuss how the HR 8799 system constrains the formation and migration of distant planets.

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