Table 3: Calculations of the ratios of trapped masses of volatiles to the mass of H2O ice in planetesimals formed at 9.8 and 12 AU in the solar nebula. Gas-phase abundance of H2O is equal to $8.11 \times 10^{-4}$ ($\sim $4.9 times the value quoted in Table 2; see text), and gas-phase abundances of elements are assumed to be solar (Lodders 2003) with CO2:CO:CH4 = 30:10:1 and with N2:NH3 = 1 in vapor phase in the solar nebula. The abundance of H2S is subsolar (see text).
  9.8 AU 12 AU

CO2:H2O		 $8.91 \times 10^{-1}$ $9.13 \times 10^{-1}$
CO:H2O $1.46 \times 10^{-1}$ $1.45 \times 10^{-1}$
CH4:H2O $9.14 \times 10^{-3}$ $9.23 \times 10^{-3}$
N2:H2O $5.26 \times 10^{-2}$ $5.34 \times 10^{-2}$
NH3:H2O $4.67 \times 10^{-2}$ $4.66 \times 10^{-2}$
H2S:H2O $4.28 \times 10^{-2}$ $4.32 \times 10^{-2}$
Ar:H2O $9.74 \times 10^{-3}$ $9.94 \times 10^{-3}$
Kr:H2O $1.34 \times 10^{-5}$ $1.34 \times 10^{-5}$
Xe:H2O $2.44 \times 10^{-6}$ $2.45 \times 10^{-6}$


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