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Table 19

Photoionisation rates of atoms and molecules and parameterised dust.

ISRF dust shielding
Species ISRF Mathis ’83 4000 K 10 000 K Lyman-α Solar TW-Hydra γexp,ISM γE2,ISM γE2,growth
H – – – – – 1.6E–12 5.4E–12 3.00 – –
Li 3.4E–10 2.3E–10 3.1E–09 7.1E–10 2.1E–10 4.9E–09 3.3E–10 2.45 1.68 0.32
C 3.5E–10 2.6E–10 5.7E–15 2.8E–11 – 1.0E–11 8.3E–11 3.76 2.77 0.45
N – – – – – 1.6E–12 7.8E–12 – – –
O – – – – – 1.4E–12 6.2E–12 – – –
Na 1.4E–11 9.1E–12 1.3E–10 1.5E–11 1.7E–11 1.4E–10 1.5E–11 2.62 1.81 0.37
Mg 6.6E–11 4.3E–11 8.1E–12 5.3E–11 1.1E–11 7.3E–12 4.2E–11 2.43 1.67 0.43
Al 4.4E–09 3.0E–09 2.1E–08 1.0E–08 1.4E–09 2.1E–08 3.7E–09 2.36 1.62 0.31
Si 4.5E–09 2.9E–09 9.3E–11 2.0E–09 5.7E–09 2.9E–10 4.4E–09 2.61 1.81 0.45
P 1.9E–09 1.4E–09 1.4E–13 2.1E–10 – 3.3E–11 3.6E–10 3.45 2.51 0.45
S 1.1E–09 8.5E–10 8.3E–14 1.2E–10 1.1E–16 2.4E–11 2.3E–10 3.52 2.57 0.45
Cl 4.7E–11 5.5E–11 – 2.5E–12 – 1.1E–11 4.9E–11 4.30 3.21 0.45
K 3.9E–11 2.6E–11 3.7E–10 5.9E–11 3.5E–11 4.2E–10 4.0E–11 2.48 1.70 0.35
Ca 3.5E–10 2.3E–10 8.0E–10 6.2E–10 1.4E–10 7.9E–10 2.9E–10 2.34 1.60 0.34
Ti 2.4E–10 1.6E–10 9.8E–12 7.7E–11 4.2E–10 2.6E–11 2.9E–10 2.81 1.96 0.44
Cr 1.6E–09 1.1E–09 1.7E–09 2.1E–09 1.2E–09 1.9E–09 1.4E–09 2.39 1.63 0.35
Mn 3.3E–11 2.2E–11 6.8E–12 3.4E–11 7.0E–12 5.8E–12 2.6E–11 2.35 1.61 0.41
Fe 4.7E–10 3.1E–10 1.2E–11 2.1E–10 7.7E–10 3.9E–11 5.9E–10 2.62 1.81 0.45
Co 5.3E–11 3.4E–11 3.3E–12 3.7E–11 2.8E–11 3.5E–12 4.5E–11 2.47 1.70 0.45
Ni 9.8E–11 6.3E–11 9.5E–12 7.5E–11 4.9E–11 9.5E–12 7.7E–11 2.43 1.67 0.44
Zn 4.1E–10 2.9E–10 3.1E–14 3.8E–11 9.2E–12 2.9E–12 6.6E–11 3.25 2.35 0.45
Rb 2.7E–11 1.8E–11 1.6E–09 4.8E–11 2.3E–11 2.2E–09 3.0E–11 2.33 1.54 0.34
Ca+ 2.4E–12 2.0E–12 – 1.7E–13 – 5.2E–14 6.0E–13 4.09 3.04 0.45
H− 1.5E–07 1.6E–08 1.6E–03 2.5E–07 7.5E–10 1.4E–05 2.3E–06 1.24 0.74 0.22
H2 – – – – – 4.9E–13 3.2E–12 – – –
CH 7.6E–10 5.6E–10 2.3E–14 6.8E–11 – 9.6E–12 1.4E–10 3.67 2.70 0.45
CH3 3.3E–10 2.3E–10 8.6E–14 4.5E–11 8.4E–10 3.6E–11 5.5E–10 3.26 2.36 0.45
CH4 1.0E–11 1.2E–11 – 5.5E–13 – 9.3E–12 3.8E–11 4.31 3.21 0.45
C2 4.1E–10 3.4E–10 1.4E–15 2.7E–11 – 6.7E–12 8.7E–11 4.19 3.12 0.45
C2H2 5.3E–10 4.1E–10 5.2E–15 4.0E–11 – 2.4E–11 1.7E–10 3.92 2.91 0.45
C2H4 4.1E–10 3.2E–10 1.7E–14 3.7E–11 – 6.2E–12 8.1E–11 3.63 2.67 0.45
C2H6 2.3E–10 2.0E–10 7.9E–16 1.5E–11 – 2.3E–11 1.2E–10 4.17 3.10 0.45
C3 1.4E–10 1.1E–10 9.0E–16 9.7E–12 – 3.5E–12 3.3E–11 4.03 3.00 0.45
H2O 2.7E–11 2.6E–11 – 1.7E–12 – 4.2E–12 2.2E–11 4.27 3.18 0.45
O2 5.1E–11 4.5E–11 1.3E–16 3.4E–12 – 3.4E–12 2.2E–11 4.22 3.14 0.45
H2O2 2.5E–10 2.0E–10 3.2E–15 1.9E–11 – 1.2E–11 7.7E–11 3.88 2.88 0.45
O3 3.3E–11 3.4E–11 – 2.1E–12 – 7.5E–12 3.5E–11 4.28 3.19 0.45
CO – – – – – 6.5E–12 2.5E–11 – – –
CO2 – – – – – 5.2E–12 2.2E–11 – – –
H2CO 4.0E–10 3.1E–10 1.1E–14 3.5E–11 – 1.3E–11 1.1E–10 3.66 2.69 0.45
NH 1.9E–12 3.0E–12 – – – 2.8E–12 1.0E–11 4.34 3.24 0.45
NH2 1.9E–10 1.5E–10 1.7E–15 1.4E–11 – 8.7E–12 5.8E–11 3.97 2.94 0.45
NH3 2.7E–10 2.0E–10 1.7E–14 2.8E–11 4.8E–11 9.6E–12 9.0E–11 3.49 2.54 0.45
N2 – – – – – 1.3E–12 8.8E–12 – – –
NO 2.6E–10 1.9E–10 7.4E–14 3.1E–11 3.3E–10 1.9E–11 2.6E–10 3.38 2.46 0.45
NO2 1.5E–10 1.2E–10 4.2E–15 1.3E–11 1.7E–11 3.1E–12 4.1E–11 3.75 2.77 0.45
N2O 1.7E–10 1.9E–10 1.8E–16 1.0E–11 – 3.8E–12 3.7E–11 4.30 3.20 0.45
CN – – – – – 2.0E–12 5.9E–12 – – –
HCN 4.4E–13 7.0E–13 – 4.2E–15 – 7.5E–12 2.8E–11 4.34 3.24 0.45
HC3N 2.3E–10 1.8E–10 1.3E–15 1.6E–11 – 1.2E–11 7.7E–11 4.07 3.02 0.45
CH3OH 3.1E–10 2.5E–10 5.5E–15 2.5E–11 – 1.6E–11 1.1E–10 3.78 2.80 0.45
CH3CN 1.2E–10 1.1E–10 3.8E–16 7.8E–12 – 1.6E–11 7.7E–11 4.19 3.12 0.45
CH3SH 1.9E–09 1.3E–09 8.1E–13 2.9E–10 3.7E–09 1.6E–10 2.5E–09 3.18 2.29 0.45
CH3CHO 8.3E–10 6.0E–10 8.3E–14 9.4E–11 1.9E–10 2.4E–11 2.8E–10 3.42 2.49 0.45
CH3NH2 1.6E–09 1.2E–09 6.9E–13 2.3E–10 3.8E–09 1.7E–10 2.5E–09 3.21 2.31 0.45
NH2CHO 5.2E–10 4.0E–10 2.8E–14 4.9E–11 3.0E–11 2.0E–11 1.5E–10 3.57 2.62 0.45
C2H5OH 4.9E–10 3.9E–10 1.4E–14 4.1E–11 – 2.8E–11 1.8E–10 3.72 2.75 0.45
C3H7OH 7.7E–10 6.0E–10 2.7E–14 6.6E–11 4.4E–11 4.3E–11 2.9E–10 3.71 2.74 0.45
SH 5.0E–11 3.7E–11 5.3E–16 3.9E–12 – 8.9E–13 1.1E–11 3.92 2.90 0.45
H2S 7.8E–10 5.9E–10 4.6E–14 7.8E–11 – 2.6E–11 2.0E–10 3.53 2.58 0.45
CS 2.6E–11 1.8E–11 7.3E–16 2.4E–12 – 1.9E–13 3.6E–12 3.59 2.63 0.45
CS2 3.6E–10 2.6E–10 2.0E–14 3.4E–11 1.6E–10 2.1E–11 2.0E–10 3.57 2.62 0.45
OCS 7.7E–10 6.1E–10 1.1E–14 6.1E–11 – 3.0E–11 2.2E–10 3.85 2.86 0.45
S2 1.3E–10 9.2E–11 6.5E–14 1.8E–11 2.8E–10 1.3E–11 2.0E–10 3.27 2.36 0.45
SO 5.3E–10 3.7E–10 3.2E–14 5.7E–11 – 6.1E–12 9.8E–11 3.46 2.52 0.45
SO2 1.3E–10 1.2E–10 2.7E–16 8.4E–12 – 1.7E–11 8.4E–11 4.25 3.17 0.45
HCl 4.5E–11 4.3E–11 – 2.8E–12 – 1.2E–11 5.1E–11 4.27 3.18 0.45
AlH 1.5E–10 9.9E–11 1.2E–12 5.6E–11 3.4E–10 1.4E–11 2.3E–10 2.67 1.86 0.45

Notes. In units of s-1. These rates are for unshielded atoms and molecules exposed to the full three-dimensional interstellar radiation field, with various wavelength dependences described in Sect. 2. Dust shielding functions, θ, for an infinite-slab interstellar cloud are fit to functions of the visual extinction, AV, according to two formulae: θ(AV) = exp(−γexpAV) and θ(AV) = E2(γE2AV) (where E2 is the 2nd-order exponential integral), both assuming incident radiation at the cloud edge with the wavelength dependence of our standard ISRF radiation field (Eqs. (12) and (13) in Sect. 6.2). Values for γE2 are given assuming an interstellar dust size distribution (ISM), and following the growth of dust grains in a protoplanetary disk (growth), as described in Sect. 8.1.

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