Vissapragada, S.
Buzard, C. F.
Miller, K. A.
O’Connor, A. P.
Ruette, N. de
Urbain, Xavier
[UCL]
Savin, D. W.
(eng)
We incorporate our experimentally derived thermal rate coefficients for C + H3+ forming CH+ and CH2 + into a commonly used astrochemical model. We find that the Arrhenius–Kooij equation typically used in chemical models does not accurately fit our data and instead we use a more versatile fitting formula. At a temperature of 10 K and a density of 104 cm−3, we find no significant differences in the predicted chemical abundances, but at higher temperatures of 50, 100, and 300 K we find up to factor of 2 changes. In addition, we find that the relatively small error on our thermal rate coefficients, ~15%, significantly reduces the uncertainties on the predicted abundances compared to those obtained using the currently implemented Langevin rate coefficient with its estimated factor of 2 uncertainty.
Bibliographic reference |
Vissapragada, S. ; Buzard, C. F. ; Miller, K. A. ; O’Connor, A. P. ; Ruette, N. de ; et. al. RECOMMENDED THERMAL RATE COEFFICIENTS FOR THE C + H3+REACTION AND SOME ASTROCHEMICAL IMPLICATIONS. In: The Astrophysical Journal : an international review of astronomy and astronomical physics, Vol. 832, no.1, p. 31 (2016) |
Permanent URL |
http://hdl.handle.net/2078.1/177916 |