Oligarchic planetesimal accretion and giant planet formation II

A. FORTIER O. G. BENVENUTO A. BRUNINI1

ASTRONOMY AND ASTROPHYSICS

EDP SCIENCES S A

Lugar: Paris; Año: 2009 vol. 500 p. 1249 - 1252

0004-6361

Aims. The equation of state calculated by Saumon and collaborators has been adopted in most core-accretion simulations of giantplanetformation performed to date. Since some minor errors have been found in their original paper, we present revised simulationsof giant-planet formation that considers a corrected equation of state.Methods. We employ the same code as Fortier and collaborators in repeating our previous simulations of the formation of Jupiter.Results. Although the general conclusions of Fortier and collaborators remain valid, we obtain significantly lower core masses andshorter formation times in all cases considered.Conclusions. The minor errors in the previously published equation of state have been shown to affect directly the adiabatic gradientand the specific heat, causing an overestimation of both the core masses and formation times.