On planet formation including update type I migration rates

MARCELO MIGUEL MILLER BERTOLAMI; MARÍA PAULA RONCO; OCTAVIO MIGUEL GUILERA; MATÍAS MONTESINOS; NICOLÁS CUELLO; JORGE CUADRA

La Serena

Congreso; Second Binational Meeting SOCHIAS - AAA; 2018

Sociedad Chilena de Astronomía

As planets grow the exchange of angular momentum with the gaseous component of the protoplanetary disc produces a net torque resulting in a variation of the semimajor axis of the planet. For low-mass planets not able to open a gap in the gaseous disc this regime is known as type I migration. Pioneer works studied this mechanism in isothermal discs finding fast inward type I migration rates that were unable to reproduce the observed properties of extrasolar planets. In the last years, several improvements have been made in order to extend the study of type I migration rates to non-isothermal discs. Moreover, it was recently shown that if the planet´s luminosity due to solid accretion is taken into account, inward migration could be slowed down and even reversed. In this work, we study the planet formation process incorporating, and comparing, updated type I migration rates for non-isothermal discs and the role of planet´s luminosity over such rates. We find that the latter has dramatic effects on planetary evolution, and hence on the resulting planets. We conclude that predictions and conclusions of works based on previous type I migration rates need to be revised.