Chemistry and IR emission of acetylene in planet-forming regions of T Tauri disks - Impact of elemental abundances and dust properties

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Table B.5

Key reactions from KIDA explaining the difference between the chemical network based on UMIST+KIDA and UMIST only.

Reaction	α [cm³.s⁻¹]	β	γ [K]	Reference
C₂ + H₂ → C₂H + H	1.60e-10	0.0	1420	Pitts et al. (1982); Harada et al. (2010)
C₃H + H₂ → C₃H₂ + H	1.14e-11	0.0	950	Harada et al. (2010)
H₂CCC + H₂ → CH₂CCH + H	3.74e-12	2.0	1740	Harada et al. (2010)
C₄ + H₂ → C₄H + H	1.60e-10	0.0	1420	Harada et al. (2010)
C₄H + H₂ → C₄H₂ + H	1.14e-11	0.0	950	Harada et al. (2010)
N + CH₂CCH → C₂H₂ + HCN	5.00e-11	0.0	0.0	Loison et al. (2017)
$C_{4} H_{3}^{+} + e^{-} \to C_{2} H_{2} + C_{2} H$ $Mathematical equation: $\[\mathrm{C}_{4} \mathrm{H}_{3}^{+}+\mathrm{e}^{-} \rightarrow \mathrm{C}_{2} \mathrm{H}_{2}+\mathrm{C}_{2} \mathrm{H}\]$$	1.10e-07	0.0	0.0	Loison et al. (2017)

Notes. Most of these reactions are H-abstractions, revealing the crucial role of H₂ in the formation of acetylene.

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