Migration of Protoplanets Due to Orbital Repulsion and Formation of Protoplanets with Various Disk Masses

Details Migration of Protoplanets Due to Orbital Repulsion and Formation of Protoplanets with Various Disk Masses Migration of Protoplanets Due to Orbital Repulsion and Formation of Protoplanets with Various Disk Masses

Sep 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999dps....31.3605s&link_type=abstract

American Astronomical Society, DPS meeting #31, #36.05

Astronomy and Astrophysics

Astronomy

Scientific paper

Formation and evolution of protoplanets from planetesimal swarm embedded in protoplanetary nebulae are investigated, by three-dimensional N-body simulations. The surface density of the planetesimal disk is widely changed (Sigma = 1, 10, and 100 (a/1AU)(-3/2) {g cm(-2}) , where a is the semi-major axis) according to the diversity of the masses of the observed protoplanetary nebulae. We investigate the migration of evolving protoplanets due to orbital repulsion among them by letting initial planetesimal swarm distributed in the range of 0.5-1.5AU. The migration due to orbital repulsion would affect planetary growth if its time scale is short compared to the growth time of protoplanets. The criterion with which the migration is effective or not is clarified. Consequently, the migration is not so effective in the nebulae considered, and we found the scaling law about the isolation mass and the growth time of protoplanets: the growth time of the protoplanets is in proportion to a(3) and Sigma (-1) , and the isolation masses of the protoplanets are almost in proportion to Sigma (3/2) and a(3/4) .

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