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Dissociative recombination of BeH+ in theinterstellar medium

Published online by Cambridge University Press:  13 February 2013

S. Niyonzima ,
F. Lique ,
K. Chakrabarti ,
Å. Larson ,
A.E. Orel  and
I.F. Schneider
S. Niyonzima
Affiliation:
LOMC-UMR 6294, CNRS-Université du Havre, 76058 Le Havre, France Département de Physique, Faculté des Sciences, Université du Burundi, 2700 Bujumbura-Burundi
F. Lique
Affiliation:
LOMC-UMR 6294, CNRS-Université du Havre, 76058 Le Havre, France
K. Chakrabarti
Affiliation:
LOMC-UMR 6294, CNRS-Université du Havre, 76058 Le Havre, France Dept. of Mathematics, Scottich Church College, 1&3 Urquhart Sq., Kolkata 700006, India
Å. Larson
Affiliation:
Dept. of Physics, Stockholm University, AlbaNova University Center, 106 91 Stockholm, Sweden
A.E. Orel
Affiliation:
Dept. of Chemical Engineering and Materials Science, University of California, Davis, California 95616, USA
I.F. Schneider
Affiliation:
LOMC-UMR 6294, CNRS-Université du Havre, 76058 Le Havre, France

Abstract

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We report a theoretical study of dissociative recombination (DR) of BeH+ bylow energy electron impact, using previously computed molecular data as input for aMultichannel Quantum Defect Theory (MQDT) approach. Three electronic symmetries of BeH,2Π, 2Σ+, and 2Δ have been included in thecalculations. We present cross sections and thermal rate coefficients ready to be used inthe modelling of the BeH+ abundance in the interstellar medium and stellaratmosphere.

References

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