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B. T. Draine and B. Sutin, Collisional charging of interstellar grains, The Astrophysical Journal, vol.320, p.803, 1987.
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E. Dwek, The Evolution of the Elemental Abundances in the Gas and Dust Phases of the Galaxy, The Astrophysical Journal, vol.501, issue.2, p.643, 1998.
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D. Flower and G. Pineau-des-forêts, The influence of grains on the propagation and structure of C-type shock waves in interstellar molecular clouds, Monthly Notices of the Royal Astronomical Society, vol.343, issue.2, p.390, 2003.
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. Les and . ?u, ?h, et ?s sont respectivement l'énergie interne thermique, l'enthalpie et l'entropie par unité de

. Dans-notre-modèle, un tiers de l'énergie libérée se retrouve sous forme d'énergie cinétique de la molécule H 2 et un autre tiers sous forme d'énergie interne de H 2 . Le tiers restant contribue à chauffer le grain, mais n'est en fait pas comptabilisé car aucun bilan thermique des poussières n'est, pour l'instant, effectué

L. De-kelvin, Helmotz est générée par un cisaillement des vitesses entre deux couches de fluide, quelles que soient leurs densités. Elle conduit à l'apparition d

. Dans-cette-hypothèse, la recombinaison des ions serait si rapide que la densité locale des ions serait déterminée par les conditions locales et non pas par l'advection 2. Il s'agit de recombinaison radiative (lente)

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J. A. Cardelli, G. C. Clayton, and . Mathis, The relationship between infrared, optical, and ultraviolet extinction, The Astrophysical Journal, vol.345, p.245, 1989.
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A. Chokshi, A. G. Tielens, and D. J. Hollenbach, Dust coagulation, The Astrophysical Journal, vol.407, p.806, 1993.
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A. P. Jones, A. G. Tielens, and D. J. Hollenbach, Grain Shattering in Shocks: The Interstellar Grain Size Distribution, The Astrophysical Journal, vol.469, issue.JTH96, p.740, 1996.
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B. T. Draine and B. Sutin, Collisional charging of interstellar grains, The Astrophysical Journal, vol.320, p.803, 1987.
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