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Название: Impact of HAC evolution on the formation of small hydrocarbons in the Orion Bar and the Horsehead PDRs
Авторы: Murga, M. S.
Vasyunin, A. I.
Kirsanova, M. S.
Дата публикации: 2022
Издатель: Oxford University Press
Библиографическое описание: Murga, MS, Vasyunin, AI & Kirsanova, MS 2022, 'Impact of HAC evolution on the formation of small hydrocarbons in the Orion Bar and the Horsehead PDRs', Monthly Notices of the Royal Astronomical Society, vol. 519, no. 2, pp. 2466-2474. https://doi.org/10.1093/mnras/stac3656
Murga, M. S., Vasyunin, A. I., & Kirsanova, M. S. (2022). Impact of HAC evolution on the formation of small hydrocarbons in the Orion Bar and the Horsehead PDRs. Monthly Notices of the Royal Astronomical Society, 519(2), 2466-2474. https://doi.org/10.1093/mnras/stac3656
Аннотация: We study evolution of hydrogenated amorphous carbon (HAC) grains under harsh UV radiation in photodissociation regions (PDRs) near young massive stars. Our aim is to evaluate the impact of the HAC grains on formation of observed small hydrocarbons: C2H, C2H2, C3H+, C3H, C3H2, C4H, in PDRs. We developed a microscopic model of the HAC grains based on available experimental results. The model includes processes of photo and thermo-desorption, accretion of hydrogen and carbon atoms and subsequent formation of carbonaceous mantle on dust surface. H2, CH4, C2H2, C2H4, C2H6, C3H4, C3H6, C3H8 are considered as the main fragments of the HAC photodestruction. We simulated evolution of the HAC grains under the physical conditions of two PDRs, the Orion Bar and the Horsehead nebula. We estimated the production rates of the HAC’ fragments in gas phase chemical reactions and compared them with the production rates of fragments due to the HAC destruction. The latter rates may dominate under some conditions, namely, at AV = 0.1 in both PDRs. We coupled our model with the gas-grain chemical model MONACO and calculated abundances of observed small hydrocarbons. We conclude that the contribution of the HAC destruction fragments to chemistry is not enough to match the observed abundances, although it increases the abundances by several orders of magnitude in the Orion Bar at AV = 0.1. Additionally, we found that the process of carbonaceous mantle formation on dust surface can be an inhibitor for the formation of observed small hydrocarbons in PDRs. © 2022 The Author(s)
Ключевые слова: ASTROCHEMISTRY
DUST, EXTINCTION
INFRARED: ISM
ISM: EVOLUTION
AMORPHOUS CARBON
HYDROCARBONS
ASTROCHEMISTRY
DUST EXTINCTIONS
DUST SURFACE
HORSEHEAD
HYDROGENATED AMORPHOUS CARBON
INFRARED: ISM
ISM:EVOLUTION
PHOTO-DISSOCIATION REGIONS
PRODUCTION RATES
SMALL HYDROCARBONS
DUST
URI: http://elar.urfu.ru/handle/10995/130474
Условия доступа: info:eu-repo/semantics/openAccess
Идентификатор SCOPUS: 85159154749
Идентификатор WOS: 000910908900010
Идентификатор PURE: 34651652
ISSN: 0035-8711
DOI: 10.1093/mnras/stac3656
Сведения о поддержке: Russian Science Foundation, RSF: 18-12-00351
We are grateful to the anonymous referee for insightful comments which helped to improve the paper. We thank Javier Goicoechea who provided the profiles of physical parameters for the Orion Bar PDR. The work was supported by the grant of the Russian Science Foundation (project 18-12-00351).
Карточка проекта РНФ: 18-12-00351
Располагается в коллекциях:Научные публикации ученых УрФУ, проиндексированные в SCOPUS и WoS CC

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