Abstract—
The paper considers a three-dimensional gas-dynamic model of a protoplanetary disk that revolves around a gravitating center. The dynamics of small perturbations in a rotational shear flow are modeled. The development of the initial azimuthal perturbations of the rotation speed leads to the formation of spiral density arms, while self-gravity increases its local maxima and creates gravitational instability as well as disk fragmentation. The obtained results are of interest for the theory explaining the formation of protoplanetary systems.
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Translated by I. Pertsovskaya
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Strakhovskaya, L.G. Three-Dimensional Numerical Modeling of the Hydrodynamic and Gravitational Instability of a Protoplanetary Disk. Math Models Comput Simul 13, 522–531 (2021). https://doi.org/10.1134/S2070048221030169
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DOI: https://doi.org/10.1134/S2070048221030169