ABSTRACT The development of a nova eruption is well known to be determined by the white dwarf (WD) mass and rate at which it accretes from its donor. One advancements in this field understanding that occurrence depends on presence heavy elements envelope, concentration these highly dependent time allotted for accretion. This results many features being correlated with fractions ejected material...

Aims. In the context of the core instability model, we present calculations of in situ giant planet formation. The oligarchic growth regime of solid protoplanets is the model adopted for the growth of the core. This growth regime for the core has not been considered before in full evolutionary calculations of this kind. Methods. The full differential equations of giant planet formation were num...

We use the evolutionary turbulent model of Jupiter’s subnebula described by Alibert et al. (2005a) to constrain the composition of ices incorporated in its regular icy satellites. We consider CO2, CO, CH4, N2, NH3, H2S, Ar, Kr, and Xe as the major volatile species existing in the gas-phase of the solar nebula. All these volatile species, except CO2 which crystallized as a pure condensate, are a...