![]() Almost all of the mass of CH + originates from unstable gas, in environments where the kinetic temperature is higher than 600 K, the density ranges between 0.6 and 10 cm −3, the electronic fraction ranges between 3 × 10 −4 and 6 × 10 −3, and the molecular fraction is smaller than 0.4. The comparison with the observations is performed taking into account an often neglected yet paramount piece of information, namely the length of the intercepted diffuse matter along the observed lines of sight. ![]() The rest of the chemistry, including the abundance of CH +, is computed in post-processing, at equilibrium, under the constraint of out-of-equilibrium H +, H, and H 2. The diffuse ISM is simulated using the magnetohydrodynamic (MHD) code RAMSES which self-consistently computes the dynamical and thermal evolution of the gas along with the time-dependent evolutions of the abundances of H +, H, and H 2. We investigate here the formation of CH + in turbulent and multiphase environments, where the heating of the gas is almost solely driven by the photoelectric effect. The high abundances of CH+ in the diffuse interstellar medium (ISM) are a long-standing issue of our understanding of the thermodynamical and chemical states of the gas. Harvard-Smithsonian Center for Astrophysics,ĭepartment of Physics, Graduate School of Science, Nagoya University,Īims. Laboratoire AIM, CEA/IRFU, CNRS/INSU, Université Paris-Diderot, CEA-Saclay, Université Paris-Saclay, CNRS, Institut d’Astrophysique Spatiale, Observatoire de Paris, Université PSL, Sorbonne Université, LERMA,Į-mail: de Physique de l’École Normale Supérieure, ENS, Université PSL, CNRS, Sorbonne Université, Université de Paris, Astronomical objects: linking to databasesī.Including author names using non-Roman alphabets.Suggested resources for more tips on language editing in the sciences Punctuation and style concerns regarding equations, figures, tables, and footnotes
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