Ejection of Dust from Planetary Systems into Interstellar Space

Details Ejection of Dust from Planetary Systems into Interstellar Space Ejection of Dust from Planetary Systems into Interstellar Space

Apr 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003eaeja.....4264k&link_type=abstract

EGS - AGU - EUG Joint Assembly, Abstracts from the meeting held in Nice, France, 6 - 11 April 2003, abstract #4264

Computer Science

Scientific paper

Extensive observational and theoretical research of the last two decades have made it clear that young exoplanetary systems comprise not only planets themselves, but also disks of small bodies and of dust-sized material these bodies replenish. In much the same way as in the young Solar System, interaction of the solids in a circumstellar disk with planets at late stages of planet formation should hang the material on the outskirts of the system, creating exosolar Kuiper belts and Oort clouds. A portion of the material is ejected by the exoplanets from the disks into interstellar space, which may represent an important source of large interstellar dust grains in the Galaxy. Here we study how the efficiency of the ejection mechanism and the involved timescales depend on the mass and orbital parameters of the planet, as well as on the `unperturbed' spatial distribution of disk particles. We also derive the distribution of the final velocities of the ejected material. The study is done semianalytically with the aid of the Oepik-Weidenschilling statistical theory of planetary encounters and numerically with direct Monte-Carlo orbital simulations. The results may have particular implications to the beta Pictoris system: they lend further support to the idea (Krivova and Solanki 2002) that a collimated stream of interstellar radiometeors detected by Baggaley (2000) originates at beta Pic and consists of grains ejected by a presumed jovian planet orbiting this star.

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