Astronomy and Astrophysics – Astronomy
Scientific paper
Sep 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011ess.....2.2201j&link_type=abstract
American Astronomical Society, ESS meeting #2, #22.01
Astronomy and Astrophysics
Astronomy
Scientific paper
There has been a long-standing discussion in the literature concerning whether planets form by core accretion or disk instabilities. Over the past decade, accumulating evidence has shown that core accretion is most likely the dominant mode of planet formation for close-in planets. However, this does not by itself mean that the majority of the total planet population formed in this manner, since disk instabilities may conceivably form a large numbers of planets farther out in the disk. Here, we present an imaging survey around most massive stars in the Solar neighborhood (B-stars), which should provide very favorable conditions for such planets to form. We find that less than 30% of the stars form and retain planets through gravitational instability. We also extend this analysis down to lower masses, through Sun-like stars and all the way down to M-stars. The results imply that core accretion is most likely the dominant formation mechanism for the total population of planets.
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