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• W2963694713 abstract "Chemical reactions in the interstellar medium (ISM) are powered by cosmic rays: Atoms and molecules (mainly molecular hydrogen) are ionized by the radiation that provides sufficient energy to initiate a chain of chemical reactions in interstellar clouds leading to the synthesis of polyatomic molecules. Many positive ions have been found and identified in ISM. In particular, the simplest positive ion, H3 plays an important role in chemistry and evolution of interstellar clouds [1, 2], mainly due to its stability and abundance of molecular hydrogen in ISM. On the other hand, only a few negative ions have been detected so far in ISM: C3N− [3], C4H− [4] , C6H− [5], and C8H− [6].The simplest negative triatomic ion, H3 is also stable although its binding energy is significantly lower than in H3 and it has not been detected so far in ISM. In this article we consider spectroscopy, formation and destruction of H3 in ISM. We argue that the ion is indeed formed in cold ISM with a relatively high degree of ionization of molecular hydrogen and can be observed. Formation and destruction in ISM. The chemistry of interstellar clouds is initiated by ionization of molecular hydrogen by cosmic rays. The rate constant for such ionization is ζ ∼ 3 × 10−17 s−1[2] in diffuse (densities about 10 cm−3) and dense (densities about 10 cm−3) interstellar clouds. The ionized molecular hydrogen H2 quickly forms H3 in collisions with H2. The escaped electron has a large kinetic energy and, therefore, before its rethermalization should undergo many elastic collisions with environmental H2. Possible inelastic e−+H2 collisions should lead to a vibrational excitation of H2 and the dissociative attachment (e−+H2 → H+H−) [7, 8]. The cross-section of the dissociative attachment at collision energies above 3.7 eV is of order of σDA ∼ 10−21 cm [7, 8]. Therefore, if we assume that electrons ejected from H2 by a cosmic ray have large enough initial kinetic energy, they will form H− with a high probability. Moreover, because the reaction rate (per one H2 molecule) for dissociative attachment, which is of order of veσDAn(H2), is larger than the rate of electron production ζ, the rate of production of H− is determined by ζn(H2) similarly to the production of H3 . [2]. However, the observation of H− is more difficult in ISM than the observation of H3 , because there is only one stable bound state of H−. Similarly to H3 (proton donor), the H − ion is chemically active (electron donor) and should initiate its own chain of chemical reactions in space. First collisions that H− would experience if formed are H−+H2. In this study we consider formation of the H3 ion in such collisions. An observation of H3 in ISM would indicate that H − is indeed formed in interstellar clouds. The H3 ion is well described as a van der Waals complex consisting of H2 and H−. The molecule has several relatively weekly bound rovibrational states and a number of predissociated resonances. The binding energy of the lowest rovibrational state is about 100 cm−1 (see Table I). The predissociated H3 resonances can be considered as excited rovibrational states (j, vd) of H2 coupled to the vibrational continuum correlated to a H2(j′, v′ d)+H − dissociation limit with energy of the dimer state (j′, v′ d) lower than the (j, vd) state. Lowest bound states of H3 are listed in Table I. The widths of the broadest resonances are in the range of 0.2 − 1.5 cm−1, which corresponds to lifetimes of 3.5− 26 ps. In order to form a bound H3 molecule in H2+H − collisions in ISM two mechanisms are possible: Three-body recombination (TBR) or radiative association (RA):" @default.
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• W2963694713 date "2010-05-29" @default.
• W2963694713 modified "2023-09-27" @default.
• W2963694713 title "Formation of the simplest stable negative molecular ion H$_3^-$ in interstellar medium" @default.
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