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(Reference retrieved automatically from Web of Science through information on FAPESP grant and its corresponding number as mentioned in the publication by the authors.)

Solar Vortex Tubes. II. On the Origin of Magnetic Vortices

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Author(s):
Silva, Suzana S. A. [1, 2] ; Verth, Gary [3] ; Rempel, Erico L. [4] ; Shelyag, Sergiy [5] ; Schiavo, Luiz A. C. A. [6] ; Fedun, Viktor [2]
Total Authors: 6
Affiliation:
[1] Aeronaut Inst Technol, Dept Phys, Sao Jose Dos Campos - Brazil
[2] Univ Sheffield, Dept Automat Control & Syst Engn, Plasma Dynam Grp Dept, Sheffield, S Yorkshire - England
[3] Univ Sheffield, Sch Math & Stat, Plasma Dynam Grp, Sheffield, S Yorkshire - England
[4] Aeronaut Inst Technol, Dept Math, Sao Jose Dos Campos - Brazil
[5] Deakin Univ, Sch Informat Technol, Geelong, Vic - Australia
[6] Sao Paulo State Univ UNESP, Sao Joao Do Boa Vista - Brazil
Total Affiliations: 6
Document type: Journal article
Source: ASTROPHYSICAL JOURNAL; v. 915, n. 1 JUL 2021.
Web of Science Citations: 0
Abstract

The solar atmosphere presents a wealth of dynamics due to a constant interplay between the plasma flows and magnetic fields. Twisted flux tubes are an essential magnetic structure, believed to be driven by the rotational surface's motions and linked to plasma heating, jets, and eruptive phenomena. Despite extensive investigations, twisted magnetic flux tubes lack a proper mathematical definition, precluding their automatic detection. This work addresses this issue by defining them as magnetic vortices and introduces a formal definition that is based on a recently developed magnetic vortex detection technique, the integrated averaged current deviation method. We applied this method and a kinetic vortex identification technique to realistic magnetoconvection simulations obtained from the MURaM code. The preferential site for these two types of vortices is the intergranular downflow, but while the magnetic vortices are found mostly in the small areas where plasma-beta > 1, the rotational flow structures (the kinetic vortices), were detected in locations where plasma-beta < 1. The magnetic vortices locally concentrate the magnetic field's vertical components and current, lasting, on average, around a minute. Two types of magnetic vortices are introduced based on their magnetic-to-kinetic energy ratio. For the first type, the magnetic energy prevails, and the magnetic vortices are mostly vertical. The second type of magnetic vortex presents distinct shapes and a lower magnetic-to-kinetic energy ratio. We have found that magnetic vortices may appear if two conditions are simultaneously present: (i) shear flow and (ii) plasma-beta > 1. The presence of rotational motion is not necessary. (AU)

FAPESP's process: 16/24970-7 - The Scintillation Prediction Observation Research Task (SPORT)
Grantee:Mangalathayil Ali Abdu
Support Opportunities: Research Projects - Thematic Grants