Simulation of Molecular Cloud Collision Dynamics Using Heterogeneous Systems

The results of computer simulation of the process of collision of rotating molecular clouds in the interstellar medium are presented. As matter is compressed, the gas density in the area of their collision increases; this leads to local changes in the shape and fragmentation of clouds. The gas densi...

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Bibliographic Details
Published inJournal of applied and industrial mathematics Vol. 17; no. 1; pp. 168 - 175
Main Authors Rybakin, B. P., Goryachev, V. D.
Format Journal Article
LanguageEnglish
Published Moscow Pleiades Publishing 01.03.2023
Springer Nature B.V
Subjects
Collision dynamics
Compressed gas
Computational grids
Computer simulation
Domains
Evolution
Gas density
Interstellar chemistry
Interstellar gas
Interstellar matter
Mathematics
Mathematics and Statistics
Molecular clouds
Optimization
Protostars
Simulation
Star & galaxy formation
Star clusters
Star formation
fragmentation of neoformations
computational astrophysics
collision of molecular clouds
parallel programming
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Summary:The results of computer simulation of the process of collision of rotating molecular clouds in the interstellar medium are presented. As matter is compressed, the gas density in the area of their collision increases; this leads to local changes in the shape and fragmentation of clouds. The gas density in the resulting condensations increases by many orders of magnitude, and gravitationally bound domains appear where star clusters can form. The process of star formation is accompanied by considerable spatial and temporal changes in the interstellar gas in these domains, turbulence of the interstellar medium, gravity, and a sharp change in magnetic and radiation fields at the prestellar stage of the evolution of new formations. The rotation of colliding molecular clouds has a great influence on the ongoing processes. The evolution of the matter of protostellar regions from the moment when they begin to form until the moment when they reach stellar density covers a huge range of scales. Simulation of such astrophysical processes on ultra-high resolution computational grids requires a substantial increase in computer power, and optimization of parallel computing on heterogeneous computing systems is required.
ISSN:1990-4789
1990-4797
DOI:10.1134/S1990478923010192