Please use this identifier to cite or link to this item: http://hdl.handle.net/10995/103352
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dc.contributor.authorMurga, M. S.en
dc.contributor.authorKirsanova, M. S.en
dc.contributor.authorVasyunin, A. I.en
dc.contributor.authorPavlyuchenkov, Ya. N.en
dc.date.accessioned2021-08-31T15:09:10Z-
dc.date.available2021-08-31T15:09:10Z-
dc.date.issued2020-
dc.identifier.citationImpact of PAH photodissociation on the formation of small hydrocarbons in the Orion Bar and the horsehead PDRs / M. S. Murga, M. S. Kirsanova, A. I. Vasyunin, et al. — DOI 10.1093/mnras/staa2026 // Monthly Notices of the Royal Astronomical Society. — 2020. — Vol. 497. — Iss. 2. — P. 2327-2339.en
dc.identifier.issn358711-
dc.identifier.otherFinal2
dc.identifier.otherAll Open Access, Green3
dc.identifier.otherhttps://www.scopus.com/inward/record.uri?eid=2-s2.0-85095455153&doi=10.1093%2fmnras%2fstaa2026&partnerID=40&md5=783b6174495ce2e1c5a6c9abfc7ab9be
dc.identifier.otherhttp://arxiv.org/pdf/2007.06568m
dc.identifier.urihttp://hdl.handle.net/10995/103352-
dc.description.abstractWe study whether polycyclic aromatic hydrocarbons (PAHs) can be a weighty source of small hydrocarbons in photodissociation regions (PDRs). We modelled the evolution of 20 specific PAH molecules in terms of dehydrogenation and destruction of the carbon skeleton under the physical conditions of two well-studied PDRs, the Orion Bar, and the Horsehead nebula that represent prototypical examples of PDRs irradiated by 'high' and 'low' ultraviolet radiation field. PAHs are described as microcanonical systems. The acetylene molecule is considered as the main carbonaceous fragment of the PAH dissociation, as it follows from laboratory experiments and theory. We estimated the rates of acetylene production in gas phase chemical reactions and compared them with the rates of the acetylene production through the PAH dissociation. It is found that the latter rates can be higher than the former rates in the Orion Bar at AV < 1 and also at AV > 3.5. In the Horsehead nebula, the chemical reactions provide more acetylene than the PAH dissociation. The produced acetylene participate in the reactions of the formation of small hydrocarbons (C2H, C3H, C3H+, C3H2, C4H). Acetylene production via the PAH destruction may increase the abundances of small hydrocarbons produced in gas phase chemical reactions in the Orion Bar only at AV > 3.5. In the Horsehead nebula, the contribution of PAHs to the abundances of the small hydrocarbons is negligible. We conclude that the PAHs are not a major source of small hydrocarbons in both PDRs except some locations in the Orion Bar. © 2020 The Author(s).en
dc.description.sponsorshipThe work was supported by the grant of the Russian Science Foundation (project 18-12-00351). We thank Javier Goicoechea who provided the profiles of parameters in the Orion Bar. We are grateful to the anonymous referee for constructive suggestions that allowed us to improve the manuscript.en
dc.format.mimetypeapplication/pdfen
dc.language.isoenen
dc.publisherOxford University Pressen
dc.relationinfo:eu-repo/grantAgreement/RSF//18-12-00351en
dc.rightsinfo:eu-repo/semantics/openAccessen
dc.sourceMon. Not. R. Astron. Soc.2
dc.sourceMonthly Notices of the Royal Astronomical Societyen
dc.subjectASTROCHEMISTRYen
dc.subjectDUST, EXTINCTIONen
dc.subjectINFRARED: ISMen
dc.subjectISM: EVOLUTIONen
dc.titleImpact of PAH photodissociation on the formation of small hydrocarbons in the Orion Bar and the horsehead PDRsen
dc.typeArticleen
dc.typeinfo:eu-repo/semantics/articleen
dc.typeinfo:eu-repo/semantics/publishedVersionen
dc.identifier.doi10.1093/mnras/staa2026-
dc.identifier.scopus85095455153-
local.contributor.employeeMurga, M.S., Institute of Astronomy, Russian Academy of Sciences, Pyatnitskaya str 48, Moscow, 119017, Russian Federation
local.contributor.employeeKirsanova, M.S., Institute of Astronomy, Russian Academy of Sciences, Pyatnitskaya str 48, Moscow, 119017, Russian Federation, Institute of Natural Sciences and Mathematics, Ural Federal University, 19 Mira Str, Ekaterinburg, 620075, Russian Federation
local.contributor.employeeVasyunin, A.I., Institute of Natural Sciences and Mathematics, Ural Federal University, 19 Mira Str, Ekaterinburg, 620075, Russian Federation, Visiting Leading Researcher, Eng. Res. Inst. 'Ventspils Intl. Radio Astronomy Centre' of Ventspils University of Applied Sciences, Inzenieru 101, Ventspils, LV-3601, Latvia
local.contributor.employeePavlyuchenkov, Ya.N., Institute of Astronomy, Russian Academy of Sciences, Pyatnitskaya str 48, Moscow, 119017, Russian Federation
local.description.firstpage2327-
local.description.lastpage2339-
local.issue2-
local.volume497-
local.contributor.departmentInstitute of Astronomy, Russian Academy of Sciences, Pyatnitskaya str 48, Moscow, 119017, Russian Federation
local.contributor.departmentInstitute of Natural Sciences and Mathematics, Ural Federal University, 19 Mira Str, Ekaterinburg, 620075, Russian Federation
local.contributor.departmentVisiting Leading Researcher, Eng. Res. Inst. 'Ventspils Intl. Radio Astronomy Centre' of Ventspils University of Applied Sciences, Inzenieru 101, Ventspils, LV-3601, Latvia
local.identifier.pure14174009-
local.identifier.eid2-s2.0-85095455153-
local.fund.rsf18-12-00351-
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