[Previous] | [Session 40] | [Next]
O. Mousis, Y. Alibert (University of Bern)
We study the evolution of C and N chemistry in the evolutionary turbulent model of the Jovian subnebula proposed by Alibert & Mousis (DPS Meeting, 2004) and Alibert et al. (A& A, 2004, submitted). We show that the conversion of N2 to NH3 and that of CO to CH4 were inhibited in the Jovian subnebula in agreement with the previous work of Mousis & Gautier (PSS, 2004, 52, 361) and in conflict with the conclusions of Prinn & Fegley (ApJ, 1981, 249, 308). We assume that solids that formed the Jovian regular icy satellites were initially produced in the feeding zone of the proto-Jupiter prior to the formation of its surrounding subdisk. NH3 hydrate, as well as CO, CH4, N2, Xe, Kr, Ar clathrate hydrates and pure ice of CO2 were condensed in the feeding zone of Jupiter prior to be embedded in the Jovian subnebula under the forms of icy planetesimals. Taking into account the regular satellite formation scenario proposed by Alibert & Mousis (DPS Meeting, 2004), it is possible to assess the per mass abundances of CO2, CO, CH4, N2, NH3, Xe, Ar, and Kr with respect to H2O in the interiors of the Jovian regular icy satellites.
[Previous] | [Session 40] | [Next]
Bulletin of the American Astronomical Society, 36 #4
© 2004. The American Astronomical Soceity.