2024/05/05 by I. M. Sultanov, Sultanov, I. M., S. A. Khaibrakhmanov +1
Earth and Planetary Sciences · Engineering · Physics and Astronomy · #Astrophysics of Galaxies (astro-ph.GA) #FOS: Physical sciences #High-pressure geophysics and materials #Phase Equilibria and Thermodynamics #Quantum, superfluid, helium dynamics #Solar and Stellar Astrophysics (astro-ph.SR)
paper · pdf · doi:10.48550/arxiv.2405.02930
openalex publication_date 2024/05/05 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
We perform numerical magnetohydrodynamic (MHD) simulations of the gravitational collapse and fragmentation of a cylindrical molecular cloud with the help of the FLASH code. The cloud collapses rapidly along its radius without any signs of fragmentation in the simulations without magnetic field. The radial collapse of the cloud is stopped by the magnetic pressure gradient in the simulations with parallel magnetic field. Cores with high density form at the cloud ends during further evolution. The core densities are n ≈ 1.7 ⋅ 108 and 2 ⋅ 107 cm-3 in the cases with initial magnetic field strengths B = 1.9 ⋅ 10-4 and 6 ⋅ 10-4 G, respectively. The cores move toward the cloud center with supersonic speeds |vz|=3.6 and 5.3 km⋅s-1. The sizes of the cores along the filaments radius and filament main axis are dr = 0.0075 pc and dz = 0.025 pc, dr = 0.03 pc and dz = 0.025 pc, respectively. The masses of the cores increase during the filament evolution and lie in range of ≈ 10-20 M_\odot. According to our results, the cores observed at the edges of molecular filaments can be a result of the filament evolution with parallel magnetic field.