Other
Scientific paper
Sep 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011ess.....2.3606h&link_type=abstract
American Astronomical Society, ESS meeting #2, #36.06
Other
Scientific paper
Massive planets likely form as a consequence of rapid migration of planetesimals and low mass cores into specific trapping sites in protoplanetary discs. We show that a complete analysis of how planet traps arise and move during disk evolution coupled with an analysis of how planets "drop-out" of such traps to undergo Type II migration, provides deep insight into architecture of planetary systems as represented in the observed mass-period relation. We present analytical modeling of inhomogeneities in Protoplanetary discs around a variety of young stars and show how they give rise to planet traps. We investigate both corotation and Lindblad torques, and show that a new trap arises from the (entropy-related) corotation torque. This arises at that disc radius where disc heating changes from viscous to stellar irradiation dominated processes. We demonstrate that up to three traps (heat transitions, ice lines and dead zones) can exist in a single disc. The radial positions of these traps are sensitive to stellar masses and accretion rates. These traps move differently as disc accretion rates decrease with time as a consequence of viscous evolution of disks. We can predict when planets become massive enough that they cease to follow the motion of their traps and undergo slower type II migration. In a number of systems, the planets in their traps converge upon one another during the later phases of disk evolution - to the point that planet-planet interaction occurs. We have combined all of these physical effects together with photoevaporation of disks, and find that planet traps together with trap-induced planet-planet interaction are crucial ingredients for understanding the mass-period relation. We demonstrate that the structure of the mass-period relations also depends on the mass of the host stars which ultimately regulate the positions of planet traps as well as the efficiency of photoevaporation.
Hasegawa Yasuhiro
Pudritz Ralph E.
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