MISHRA, R., Miljenko ČEMELJIĆ and Wlodzimierz KLUŹNIAK. Accretion disc backflow in resistive MHD simulations. Monthly Notices of the Royal Astronomical Society. 2023, vol. 523, No 3, p. 4708-4719. ISSN 0035-8711. Available from: https://dx.doi.org/10.1093/mnras/stad1691.
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Basic information
Original name Accretion disc backflow in resistive MHD simulations
Authors MISHRA, R., Miljenko ČEMELJIĆ (191 Croatia, belonging to the institution) and Wlodzimierz KLUŹNIAK (616 Poland).
Edition Monthly Notices of the Royal Astronomical Society, 2023, 0035-8711.
Other information
Original language English
Type of outcome Article in a journal
Field of Study 10308 Astronomy
Country of publisher United Kingdom of Great Britain and Northern Ireland
Confidentiality degree is not subject to a state or trade secret
WWW URL
RIV identification code RIV/47813059:19630/23:A0000262
Organization unit Institute of physics in Opava
Doi http://dx.doi.org/10.1093/mnras/stad1691
UT WoS 001019516400005
Keywords in English accretion; accretion discs;magnetic fields;(magnetohydrodynamics) MHD;methods: numerical
Tags RIV24, UF
Tags International impact, Reviewed
Links GX21-06825X, research and development project.
Changed by Changed by: Mgr. Pavlína Jalůvková, učo 25213. Changed: 14/2/2024 11:18.
Abstract
We investigate accretion onto a central star, with the size, rotation rate, and magnetic dipole of a young stellar object, to study the flow pattern (velocity and density) of the fluid within and outside of the disc. We perform resistive magnetohydrodynamic (MHD) simulations of thin discs, varying the parameters such as the stellar rotation rate and (anomalous) coefficients of viscosity and resistivity in the disc. To provide a benchmark for the results and to compare them with known analytic results, we also perform purely hydrodynamic (HD) simulations for the same problem. Although obtained for different situations with differing inner boundary condition, the disc structure in the HD simulations closely follows the analytic solution of Kluzniak and Kita - in particular, a region of 'mid-plane' backflow exists in the right range of radii, depending on the viscosity parameter. In the MHD solutions, whenever the magnetic Prandtl number does not exceed a certain critical value, the mid-plane backflow exists throughout the accretion disc, extending all the way down to the foot point of the accretion funnel flow where the disc transitions to a magnetic funnel flow. For values of the magnetic Prandtl number close to the critical value the backflow and the inner disc undergo a quasi-periodic radial oscillation, otherwise the backflow is steady, as is the disc solution. From our results, supplemented by our reading of the literature, we suggest that mid-plane backflow is a real, physical, and not only numerical feature of at least some accretion discs.
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