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Numerical 2D MHD simulations of the collapse of magnetic rotating protostellar clouds with the Enlil code

Published online by Cambridge University Press:  20 January 2023

Sergey Khaibrakhmanov Open the ORCID record for Sergey Khaibrakhmanov [Opens in a new window] ,
Sergey Zamozdra ,
Natalya Kargaltseva ,
Andrey Zhilkin Open the ORCID record for Andrey Zhilkin [Opens in a new window]  and
Alexander Dudorov
Sergey Khaibrakhmanov
Affiliation:
Ural Federal University, 51 Lenina str., Ekaterinburg, 620000, Russia email: mailto:[email protected] [email protected] Chelyabinsk State University, 129 Br. Kashirinykh str., Chelyabinsk, 454001, Russia
Sergey Zamozdra
Affiliation:
Chelyabinsk State University, 129 Br. Kashirinykh str., Chelyabinsk, 454001, Russia
Natalya Kargaltseva
Affiliation:
Ural Federal University, 51 Lenina str., Ekaterinburg, 620000, Russia email: mailto:[email protected] [email protected] Chelyabinsk State University, 129 Br. Kashirinykh str., Chelyabinsk, 454001, Russia
Andrey Zhilkin
Affiliation:
Institute of Astronomy of the Russian Academy of Sciences (INASAN), Moscow, 119017, Russia
Alexander Dudorov
Affiliation:
Chelyabinsk State University, 129 Br. Kashirinykh str., Chelyabinsk, 454001, Russia
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Abstract

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We numerically investigate the gravitational collapse of rotating magnetic protostellar clouds. The simulations are performed using 2D MHD code ‘Enlil’. The code is based on TVD scheme of increased order of accuracy. We developed a model of the initially non-uniform cloud, which self-consistently treats gas density and large-scale magnetic field distribution. Simulation results for the typical parameters of a solar mass cloud are presented. In agreement with our previous results for the uniform cloud, the isothermal collapse of the non-uniform cloud results in formation of hierarchical structure of the cloud, consisting of flattened envelope and thin quasi-magnetostatic primary disk near its equatorial plane. The non-uniform cloud collapses longer than the uniform one, since the magnetic field is dynamically stronger at the periphery of the cloud in the former case.

Keywords

magnetic fieldsmagnetohydrodynamics (MHD)numerical simulationstar formationinterstellar medium
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 16 , Symposium S362: The Predictive Power of Computational Astrophysics as a Discovery Tool , June 2020 , pp. 273 - 278
Copyright
© The Author(s), 2023. Published by Cambridge University Press on behalf of International Astronomical Union

Footnotes

†

Professor Alexander Dudorov has passed away.

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