Volume 607, November 2017
|Number of page(s)||6|
|Section||Interstellar and circumstellar matter|
|Published online||13 November 2017|
Search for hydrogen-helium molecular species in space
1 Sorbonne Universités, UPMC Univ. Paris 06, UMR – CNRS 7616, Laboratoire de Chimie Théorique, 75005 Paris, France
2 Univ. Lyon, Université Claude Bernard Lyon 1, CNRS, Institut Lumière Matière, 69622 Villeurbanne, France
3 Sorbonne Universités, UPMC Univ. Paris 06 et CNRS, UMR 7095, Institut d’Astrophysique de Paris, 75014 Paris, France
Received: 25 June 2017
Accepted: 27 July 2017
Context. Helium, the second most abundant element in the Universe, with a relative abundance of He/H ~ 1/10, has never been observed in any other form than that of a neutral atom (He) or an ion (He+) in the interstellar medium. Since He is a noble gas its non-observation as part of neutral molecular systems is understandable, but it is very surprising for a positively charged species such as HeH+ that is a stable diatomic ion whose spectral signatures are well known in the laboratory.
Aims. This non-observation, even in hydrogen rich regions, could imply that HeH+ is not a proper target and that alternatives have to be considered, such as small HeHn+ clusters. The present study aims at finding whether the leading term HeH3+ fulfills the conditions required.
Methods. We addressed the question with state-of-the-art numerical simulations. We determined a two-dimension ab initio potential energy surface (PES) of the HeH3+ cluster along the He...H3+ and HeH+...H2 reaction coordinates. The calculations rely on complete active space configuration interaction followed by a second order perturbation treatment (CAS-PT2). This surface was used for the evaluation of the two radiative associations rate constants by means of a quantum treatment of the collision between the interacting fragments.
Results. These calculations show unambiguously that HeH3+ is the most stable point on the corresponding global PES. Then, we determined the rate constants of the radiative associations HeH+ + H2 and He + H3+ leading to HeH3+.
Conclusions. Significative values were obtained that reach up to 2 × 10-18 cm3 s-1, which should stimulate new tentatives to detect molecular helium in astrophysical objects.
Key words: ISM: molecules / ISM: abundances
© ESO, 2017
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