Abstract
The work is aimed at studying the formation mechanisms of straightened segments (rows) in spiral galactic arms, which are found in approximately 5% of S-galaxies. We use the Smoothed Particles Hydrodynamics (SPH) numerical algorithm, which is adapted for parallel computing on the GPUs to simulate the gas component. N-body model is used to simulate the dynamics of collisionless stellar disk. Graphic processors allow you to apply the “Particle-Particle” algorithm (each particle interacts with every other particle), which is the most accurate method to account for self-gravity. Our numerical model demonstrates the formation of a rows system with a pronounced transient character.
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