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Modeling the formation of dense clumps during molecular clouds collisionстатья
Статья опубликована в высокорейтинговом журнале
Информация о цитировании статьи получена из
Web of Science,
Scopus
Статья опубликована в журнале из списка Web of Science и/или Scopus
Дата последнего поиска статьи во внешних источниках: 10 августа 2021 г.
- Авторы: Rybakin B.P., Goryachev V.D., Stamov L.I., Mikhalchenko E.V., Tyurenkova V.V., Smirnova M.N., Shamina A.A., Kolenkina E.I., Pestov D.A.
- Журнал: Acta Astronautica
- Том: 170
- Год издания: 2020
- Издательство: Pergamon Press Ltd.
- Местоположение издательства: United Kingdom
- Первая страница: 586
- Последняя страница: 591
- DOI: 10.1016/j.actaastro.2020.02.026
- Аннотация: The paper presents the results of numerical modeling of the collision process of two molecular clouds (MC). The process of formation and growth of dense clumps and filament is investigated. The density distribution along the MC radius is modeling according to various laws, and the density at the center of molecular clouds also changes. The processes of deformation, fragmentation, and the formation of superdense clumps zones are analyzed. Calculations are carried out according to different scenarios of collision of two spherical clouds that are heterogeneous in size, displacement, and internal distribution. The Euler numerical code created by the authors is used to conduct a numerical experiment on high-performance computers. The appearance of zones with a high degree of compression of the substance during the formation of new clouds and the oscillations arising from this strongly depend on the initial momentum of the colliding molecular clouds. The paper presents an analysis of the redistribution of gas density that occurs during local compression in bow-shock core and outer layers of clouds. The mechanism of substance turbulization, fragmentation, and the creation of dense regions was analyzed and interpreted. Compressions arising in the gas core and wave-like rarefaction in the interstellar medium are interpreted as Kelvin-Helmholtz instability aftereffects.
- Добавил в систему: Стамов Любен Иванович