The Great Escape: How Exoplanets and Smaller Bodies Desert Dying Stars

Details The Great Escape: How Exoplanets and Smaller Bodies Desert Dying Stars The Great Escape: How Exoplanets and Smaller Bodies Desert Dying Stars

Sep 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011ess.....2.1501v&link_type=abstract

American Astronomical Society, ESS meeting #2, #15.01

Astronomy and Astrophysics

Astronomy

Scientific paper

Mounting discoveries of extrasolar planets orbiting post-main sequence stars motivate studies aimed at understanding the fate of these planets. In the traditional ``adiabatic" approximation, a secondary's eccentricity remains constant during stellar mass loss. Here, we remove this approximation, investigate the full two-body point-mass problem with isotropic mass loss, and illustrate the resulting dynamical evolution. We then combine these results with stellar evolution models for stars with progenitor masses from 0.7-150 Solar masses. The magnitude and duration of a star's mass loss combined with a planet's initial orbital parameters might provoke ejection, modest eccentricity pumping, or even circularization of the planetary orbit. We find that the vast majority of planetary material which survive a supernova from a 7-20 Solar-Mass progenitor will be dynamically ejected from the system, placing limits on the existence of first-generation pulsar planets. Oort Clouds and wide-orbit planets may be dynamically ejected from 1-7 Solar Mass progenitor stars during AGB evolution; remaining bound comets are likely to assume a wide range of eccentricities. Planets orbiting black hole progenitors of at least 20 Solar masses may easily survive or readily be ejected depending on the core collapse and superwind models adopted. The consequences of this work directly relate to a wide range of "Extreme Solar Systems", as well as the free-floating planetary population. Material ejected during stellar evolution could represent the primary contribution to this population, and suggest regions of the Milky Way which are the most likely to harbor free-floaters.

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