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http://elar.urfu.ru/handle/10995/141574
Название: | The influence of accretion bursts on methanol and water in massive young stellar objects |
Авторы: | Guadarrama, R. Vorobyov, E. I. Rab, C. Güdel, M. Caratti, O, Garatti, A. Sobolev, A. M. |
Дата публикации: | 2024 |
Издатель: | EDP Sciences |
Библиографическое описание: | Guadarrama, R., Vorobyov, E., Rab, C., Gudel, M., Garatti, A., & Sobolev, A. (2024). The influence of accretion bursts on methanol and water in massive young stellar objects. Astronomy and Astrophysics, 684, [A51]. https://doi.org/10.1051/0004-6361/202245694 |
Аннотация: | Context. The effect of accretion bursts on massive young stellar objects (MYSOs) represents a new research field in the study of young stars and their environment. The impact of such bursts on the disk and envelope has been observed and plays the role of a smoking gun providing information about the properties of the burst itself. Aims. We aim to investigate the impact of an accretion burst on massive disks with different types of envelopes and to study the effects of an accretion burst on the temperature structure and the chemistry of the disk. We focus on water and methanol as chemical species for this paper. Methods. The thermochemical code of ProDiMo (PROtoplanetary DIsk MOdel) is used to perform simulations of high-mass protoplanetary-disk models with different types of envelopes in the presence of an accretion burst. The models in question represent different evolutionary stages of protostellar objects. We calculated and show the chemical abundances in three phases of the simulation (pre-burst, burst, and post-burst). Results. More heavily embedded disks show higher temperatures. The impact of the accretion burst is mainly characterized by the desorption of chemical species present in the disk and envelope from the dust grains to the gas phase. When the post-burst phase starts, the sublimated species freeze out again. The degree of sublimation depends strongly on the type of envelope the disk is embedded in. An accretion burst in more massive envelopes produces stronger desorption of the chemical species. However, our models show that the timescale for the chemistry to reach the pre-burst state is independent of the type of envelope. Conclusions. The study shows that the disk s temperature increases with a more massive envelope enclosing it. Thus, the chemistry of MYSOs in earlier stages of their evolution reacts stronger to an accretion burst than at later stages where the envelope has lost most of its mass or has been dissipated. The study of the impact of accretion bursts could also provide helpful theoretical context to the observation of methanol masers in massive disks. © 2024 EDP Sciences. All rights reserved. |
Ключевые слова: | ASTROCHEMISTRY METHODS: NUMERICAL PROTOPLANETARY DISKS STARS: MASSIVE STARS: PROTOSTARS METHANOL NUMERICAL METHODS STARS SUBLIMATION ASTROCHEMISTRY CHEMICAL SPECIES DISK MODEL METHOD: NUMERICAL PROTOPLANETARY DISKS RESEARCH FIELDS STARS: MASSIVE STARS: PROTOSTARS YOUNG STARS YOUNG STELLAR OBJECTS DESORPTION |
URI: | http://elar.urfu.ru/handle/10995/141574 |
Условия доступа: | info:eu-repo/semantics/openAccess cc-by |
Идентификатор SCOPUS: | 85193924030 |
Идентификатор WOS: | 001198904700011 |
Идентификатор PURE: | 56692710 |
ISSN: | 0004-6361 1432-0746 |
DOI: | 10.1051/0004-6361/202245694 |
Сведения о поддержке: | Max-Planck-Institut für Astronomie, MPIA; Max-Planck-Gesellschaft, MPG; Austrian Science Fund, FWF, (P31635-N27); Austrian Science Fund, FWF; Deutsche Forschungsgemeinschaft, DFG, (325594231); Deutsche Forschungsgemeinschaft, DFG; Ministry of Education and Science of the Russian Federation, Minobrnauka, (FEUZ-2023-0019); Ministry of Education and Science of the Russian Federation, Minobrnauka We thank the anonymous referee whose comments helped to improve the quality of the manuscript. The computational results presented have been achieved using the Vienna Scientific Cluster (VSC). This work was supported by the Austrian Science Fund (FWF) under research grant P31635-N27. Ch. Rab is grateful for support from the Max Planck Society and acknowledges funding by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) 325594231. M.G. acknowledges support from the Max-Planck-Institute for Astronomy (Heidelberg) during his sabbatical visit. A.C.G. has been supported by PRIN-INAF MAIN-STREAM 2017 Protoplanetary disks seen through the eyes of new-generation instruments and PRIN-INAF 2019 Spectroscopically tracing the disk dispersal evolution (STRADE). A.M.S. acknowledges support from the Ministry of Science and Higher Education of the Russian Federation by an agreement FEUZ-2023-0019 |
Карточка проекта РНФ: | Max-Planck-Institut fur Astronomie, MPIA; Max-Planck-Gesellschaft, MPG; Austrian Science Fund, FWF, (P31635-N27); Austrian Science Fund, FWF; Deutsche Forschungsgemeinschaft, DFG, (325594231); Deutsche Forschungsgemeinschaft, DFG; Ministry of Education and Science of the Russian Federation, Minobrnauka, (FEUZ-2023-0019); Ministry of Education and Science of the Russian Federation, Minobrnauka We thank the anonymous referee whose comments helped to improve the quality of the manuscript. The computational results presented have been achieved using the Vienna Scientific Cluster (VSC). This work was supported by the Austrian Science Fund (FWF) under research grant P31635-N27. Ch. Rab is grateful for support from the Max Planck Society and acknowledges funding by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) 325594231. M.G. acknowledges support from the Max-Planck-Institute for Astronomy (Heidelberg) during his sabbatical visit. A.C.G. has been supported by PRIN-INAF MAIN-STREAM 2017 Protoplanetary disks seen through the eyes of new-generation instruments and PRIN-INAF 2019 Spectroscopically tracing the disk dispersal evolution (STRADE). A.M.S. acknowledges support from the Ministry of Science and Higher Education of the Russian Federation by an agreement FEUZ-2023-0019 |
Располагается в коллекциях: | Научные публикации ученых УрФУ, проиндексированные в SCOPUS и WoS CC |
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