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|Title:||Optical properties and dust temperatures in clumpy diffuse medium|
|Authors:||Ostrovskii, A. B.|
Parfenov, S. Y.
Vasyunin, A. I.
Ivlev, A. V.
Sokolova, V. A.
|Publisher:||Oxford University Press|
|Citation:||Optical properties and dust temperatures in clumpy diffuse medium / A. B. Ostrovskii, S. Y. Parfenov, A. I. Vasyunin, et al. — DOI 10.1093/MNRAS/STAA1460 // Monthly Notices of the Royal Astronomical Society. — 2020. — Vol. 495. — Iss. 4. — P. 4314-4325.|
|Abstract:||In this study, we explore the impact of inhomogeneities in the spatial distribution of interstellar dust on spatial scales of ≤1 au caused by ion shadowing forces on the optical properties of diffuse interstellar medium (ISM) as well as on the dust temperature. We show that recently proposed possibility that interstellar dust grains in the diffuse ISM are grouped in spherical cloudlets (clumps) may significantly affect the observed optical properties of the diffuse ISM in comparison to that calculated under the commonly accepted assumption on the uniform dust/gas mixture if the size of clumps ≳0.1 au. We found that opacity of an arbitrary region of diffuse ISM quickly decreases with growth of dusty clumps. We also studied the dependence of opacity and dust temperature inside the dusty clumps on their size. We show that the clumps larger than 0.1 au are opaque for far-ultraviolet radiation. Dust temperature exhibits a gradient inside a clump, decreasing from the edge to the centre by several degrees for a clump of a size of 0.1 au and larger. We argue that dust temperatures and high opacity within clumps larger than 0.1 au may facilitate somewhat more efficient synthesis of molecules on surfaces of interstellar grains in the diffuse ISM than it was anticipated previously. On the other hand, the presence of clumps with sizes below 0.1 au makes small or negligible influence on the optical properties of the diffuse ISM in comparison to the case with uniform dust/gas mixture. © 2020 The Author(s).|
|metadata.dc.description.sponsorship:||The authors are thankful to Prof. Paola Caselli and Dr. Yaroslav Pavlyuchenkov for critical reading of the manuscript and suggestions on its improvement. The authors are also thankful to the anonymous referee for suggestions that helped to improve the manuscript. ABO, AIV, and AVI were supported by the Russian Science Foundation via the project 18-12-00351. AIV and VAS are members of the Max Planck Partner Group at the Ural Federal University. Monte Carlo simulations were made by SYP. SYP acknowledges support by the Ministry of Science and Higher Education of the Russian Federation, FEUZ-2020-0030.|
|RSCF project card:||18-12-00351|
|Appears in Collections:||Научные публикации, проиндексированные в SCOPUS и WoS CC|
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