Propagation of Eccentricity Disturbances in Planetary Systems

Details Propagation of Eccentricity Disturbances in Planetary Systems Propagation of Eccentricity Disturbances in Planetary Systems

Jun 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aipc..713..257z&link_type=abstract

THE SEARCH FOR OTHER WORLDS: Fourteenth Astrophysics Conference. AIP Conference Proceedings, Volume 713, pp. 257-260 (2004).

Astronomy and Astrophysics

Astrophysics

1

Extrasolar Planetary Systems

Scientific paper

One of the remarkable features of the ~ 120 known extrasolar planets is their relatively high eccentricities. We suggest that these eccentricities arise because of secular interactions in an extended planetary disk: eccentricities are excited in the outer part of the disk, for example by a passing star, and then propagate inward through the disk, somewhat like a wave. We explore how the inward propagation of eccentricity in planetary disks depends on the number and masses of the planets and on the overall surface density distribution. We find that the main governing factor is the large-scale surface-density distribution. If the latter is approximated by a power-law Σ(r) ~ r-q, then eccentricity disturbances propagate inward efficiently for flat density distributions with q <~ 1.

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