Abstract
In the current study, the vortex structures that occur in accretion disks are investigated using mathematical modeling methods. The simulation of the processes of formation of large-scale vortex structures in stellar accretion disks is carried out by two methods with different numerical schemes. The first numerical technique is based on conservative difference scheme with “upwind” approximation for fluxes. The second numerical technique is based on an explicit, conservative, monotone in the linear approximation Godunov-type Roe–Einfeldt–Osher scheme, which approximates, with order no higher than the third, the conservation laws in the form of Euler equations. Visualized pictures of the vortex structure are given by both methods for accretion disks. The qualitative similarity of the obtained results is discussed. Evolutionary calculations are carried out on the basis of parallel algorithms implemented on the supercomputing complex of the cluster architecture.
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Acknowledgements
The authors are grateful to A.G. Aksenov for helpful discussions of the setting of the initial field for the modeling of fast-rotating stellar accretion disks.
The work is performed in the framework of state assignments of the ICAD RAS and KIAM RAS.
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Babakov, A.V., Lugovsky, A.Y., Chechetkin, V.M. (2020). Modeling of Some Astrophysical Problems on Supercomputers Using Gas-Dynamic Model. In: Jain, L., Favorskaya, M., Nikitin, I., Reviznikov, D. (eds) Advances in Theory and Practice of Computational Mechanics. Smart Innovation, Systems and Technologies, vol 173. Springer, Singapore. https://doi.org/10.1007/978-981-15-2600-8_3
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