A ∼32-70 K formation temperature range for the ice grains agglomerated by comet 67 P/Churyumov-Gerasimenko

Abstract

Grand Canonical Monte Carlo simulations are used to reproduce the N 2 /CO ratio ranging between 1.7 × 10 -3 and 1.6 × 10 -2 observed in situ in the Jupiter-family comet 67 P/Churyumov-Gerasimenko (67 P) by the ROSINA mass spectrometer on board the Rosetta spacecraft. By assuming that this body has been agglomerated from clathrates in the protosolar nebula (PSN), simulations are developed using elaborated interatomic potentials for investigating the temperature dependence of the trapping within a multiple-guest clathrate formed from a gas mixture of CO and N 2 in proportions corresponding to those expected for the PSN. By assuming that 67 P agglomerated from clathrates, our calculations suggest the cometary grains must have been formed at temperatures ranging between ∼31.8 and 69.9 K in the PSN to match the N 2 /CO ratio measured by the ROSINA mass spectrometer. The presence of clathrates in Jupiter-family comets could then explain the potential N 2 depletion (factor of up to ∼87 compared to the protosolar value) measured in 67 P.