Paper:	Planetary Migration in Protoplanetary Disks
Volume:	294, Scientific Frontiers in Research on Extrasolar Planets
Page:	327
Authors:	del Popolo, A.
Abstract:	In the current paper, we further develop the model for the migration of planets introduced in Del Popolo et al. (2001) and extended to time-dependent planetesimal accretion disks in Del Popolo & Ekši (2002). We use a method developed by Stepinski & Valageas (1996, 1997), that is able to simultaneously follow the evolution of gas and solid particles for up to 107 years. The disk model is coupled to the migration model introduced in Del Popolo et al. (2001) in order to obtain the migration rate of the planet in the planetesimal disk. We find that in the case of disks having total mass of 10-3-0.1 solar masses, and 0.1<α<0.0001, planets can migrate inward a large distance while if M<10-3 solar masses the planets remain almost in their initial position for 0.1<α<0.01 and only in the case α<0.001 the planets move to a minimum value of orbital radius of ∼= 2 AU. The model gives a good description of the observed distribution of planets in the period range 0-20 days.

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