C.D.S. - SIMBAD4 rel 1.7 - 2020.07.11CEST18:34:44

2013A&A...550A...8G - Astronomy and Astrophysics, volume 550A, 8-8 (2013/2-1)

A complete model of CH+ rotational excitation including radiative and chemical pumping processes.


Abstract (from CDS):

Excitation of far-infrared and submillimetric molecular lines may originate from nonreactive collisions, chemical formation, or far infrared, near-infrared, and optical fluorescences. As a template, we investigate the impact of each of these processes on the excitation of the methylidyne cation CH+ and on the intensities of its rotational transitions recently detected in emission in dense photodissociation regions (PDRs) and in planetary nebulae. We have developed a nonlocal thermodynamic equilibrium excitation model that includes the entire energy structure of CH+, i.e. taking into account the pumping of its vibrational and bound and unbound electronic states by near-infrared and optical photons. The model includes the theoretical cross-sections of nonreactive collisions with H, H2, He, and e, and a Boltzmann distribution is used to describe the probability of populating the excited levels of CH+ during its chemical formation by hydrogenation of C+. To confirm our results we also performed an extensive analytical study, which we use to predict the main excitation process of several diatomic molecules, namely HF, HCl, SiO, CS, and CO. At densities nH=104cm3, the excitation of the rotational levels of CH+ is dominated by the radiative pumping of its electronic, vibrational, and rotational states if the intensities of the radiation field at ∼0.4, ∼4, and ∼300µm are stronger than 105, 108, and 104 times those of the local interstellar radiation field (ISRF). Below these values, the chemical pumping is the dominant source of excitation of the J>1 levels, even at high kinetic temperatures (∼1000 K). The far-infrared emission lines of CH+ observed in the Orion Bar and the NGC 7027 PDRs are consistent with the predictions of our excitation model assuming an incident far-ultraviolet (FUV) radiation field of ∼3x104 (in Draine's unit) and densities of ∼5x104 and ∼2x105cm3. In the case of NGC 7027, the estimate of the density is 10 to 100 times lower than those deduced by traditional excitation codes. Applying our model to other X1Σ+ ground state diatomic molecules, we find that HF, and SiO and HCl are the species the most sensitive to the radiative pumping of their vibrational and bound electronic states. In both cases, the minimal near-infrared and optical/ultraviolet radiation field intensities required to modify their rotational level populations are ∼103 times those of the local ISRF at densities nH=104cm3. All these results point towards interstellar and circumstellar media with densities lower than previously established and cast doubts on the clumpiness of well-studied molecular clouds.

Abstract Copyright:

Journal keyword(s): line: formation - molecular processes - radiative transfer - ISM: molecules

Simbad objects: 9

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Number of rows : 9

N Identifier Otype ICRS (J2000)
ICRS (J2000)
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
1 RAFGL 618 pA* 04 42 53.6245215366 +36 06 53.397219192   16.32   12.59   C-rich 954 0
2 NAME Orion Bright Bar reg 05 35 22.30 -05 24 33.0           ~ 716 0
3 NAME ORI MOL CLOUD MoC 05 56 -01.8           ~ 848 1
4 IRC +10216 C* 09 47 57.40632 +13 16 43.5648     10.96     C9,5e 2134 0
5 HD 100546 Be* 11 33 25.4404858122 -70 11 41.239343121   6.71 6.30   6.64 A0VaekB8_lB 651 1
6 NAME Sgr B2 MoC 17 47 20.4 -28 23 07           ~ 1909 1
7 NGC 7027 PN 21 07 01.8 +42 14 10   9.1 10.9     ~ 2323 1
8 HD 210121 * 22 08 11.9025501667 -03 31 52.770012247   7.84 7.68     B7II 149 0
9 SH 2-140 OpC 22 19 07.8 +63 17 07           ~ 634 2

    Equat.    Gal    SGal    Ecl

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