Open AccessInfluence of the magnetic field on the formation of protostellar disks
Author(s) -
N. S. Kargaltseva,
Sergey A. Khaibrakhmanov,
A. E. Dudorov,
S. N. Zamozdra,
А. Г. Жилкин
Publication year - 2022
Publication title -
astronomy at the epoch of multimessenger studies. proceedings of the vak-2021 conference, aug 23–28, 2021
Language(s) - English
Resource type - Conference proceedings
DOI - 10.51194/vak2021.2022.1.1.045
Subject(s) - ambipolar diffusion , magnetic cloud , physics , magnetic field , gravitational collapse , magnetic energy , dissipation , cloud computing , astrophysics , mechanics , computational physics , coronal mass ejection , thermodynamics , magnetization , plasma , quantum mechanics , solar wind , computer science , operating system
We present the results of the numerical simulations of the collapse of magnetic rotating protostellar clouds with mass 10M ⊙ . The hierarchical structure of the cloud formed at the isothermal stage of the collapse is investigated for various initialratios of the magnetic energy of the cloud to the modulus of its gravitational energy, ε m . It is shown that the size of thequasi-magnetostatic primary disk and the region of ecient magnetic braking increase with ε m . In the case ε m ≥ 0.6,practically the entire cloud evolves into the state of quasi-magnetostatic equilibrium. A ‘dead’ zone forms inside the rsthydrostatic core and in the area of the outow formation, where Ohmic dissipation and ambipolar diusion become essential.