Table 2
Initial abundances following Aikawa et al. (2001), except for the inclusion of ortho and para spin-states of H2.
| Species | Abundance (/nH) | Species | Abundance (/nH) |
|---|---|---|---|
| o-H2 | 4.5(−1) | S+ | 9.14(−8) |
| p-H2 | 4.5(−2) | Mg+ | 1.09(−8) |
| He | 9.75(−2) | Si+ | 9.74(−9) |
| HD | 1.5(−5) | Fe+ | 2.74(−9) |
| O | 1.8(−4) | Na+ | 2.25(−9) |
| C+ | 7.86(−5) | P+ | 1(−9) |
| H | 5(−5) | Cl+ | 2.16(−10) |
| N | 2.47(−5) |
Notes.Theinitial ortho/para ratio is motivated by the results of Furuya et al. (2016), who found that a ratio of 0.1 best reproduced the observed D/H ratios in hot corinos toward low-mass protostars in their models. A(B) = A × 10B.
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