Interstellar bromine abundance is consistent with cometary ices from Rosetta

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Table 3

Chemical reaction network for bromine.


#	R₁	R₂	P₁	P₂	k(T) [cm³s⁻¹]	Reference





(1)	Br	H₂	HBr	H	8.3 × 10⁻¹¹ × exp(−8812 K/T)	Fettis et al. (1960)
(2)	HBr	H	Br	H₂	8.9 × 10⁻¹¹ × exp(−684 K/T)	White & Thompson (1974)
(3)	HBr	H′	H′Br	H	4.0 × 10⁻¹⁰ × exp(−1140 K/T)	White & Thompson (1974)
(4)	Br⁺	H₂	HBr⁺	H	10⁻⁹ × exp(−6200 K/T)	Mayhew & Smith (1990), Neufeld & Wolfire (2009)^a,c
(5)	HBr⁺	e⁻	Br	H		Neufeld & Wolfire (2009)^a
(6)	HBr⁺	H₂	H₂Br⁺	H	(13.2 ± 1.6) × 10⁻¹⁰	Belikov & Smith (2008)
(7)	H₂Br⁺	e⁻	HBr	H		Neufeld & Wolfire (2009)^a,b
(8)	H₂Br⁺	e⁻	Br	2H		Neufeld & Wolfire (2009)^a
(9)	HBr	hν	Br	H	1.7 × 10⁻⁷ × χ_UV	Neufeld & Wolfire (2009)^a
(10)	HBr	hν	HBr⁺	e⁻	10⁻¹⁰ × χ_UV	Neufeld & Wolfire (2009)^a

Notes.R_i and P_i denote the reactants and products. ^(a) Assumed order-of-magnitude similar to corresponding Cℓ, F reactions from Neufeld & Wolfire (2009); ^(b)upper limit based on H₂ Cl⁺ + e⁻ branching ratio (see text); ^(c)see Sect. 5.

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