I. Jet Formation and Evolution Due to 3D Magnetic Reconnection

González-Avilés, Jose, Guzmán, Francisco, Fedun, Viktor, Verth, Gary, Shelyag, Sergiy and Regnier, Stephane (2018) I. Jet Formation and Evolution Due to 3D Magnetic Reconnection. The Astrophysical Journal, 856 (2). p. 176. ISSN 1538-4357

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Official URL: https://doi.org/10.3847/1538-4357/aab36f


Using simulated data-driven, 3D resistive MHD simulations of the solar atmosphere, we show that 3D magnetic reconnection may be responsible for the formation of jets with the characteristics of Type II spicules. We numerically model the photosphere-corona region using the C7 equilibrium atmosphere model. The initial magnetic configuration is a 3D potential magnetic field, extrapolated up to the solar corona region from a dynamic realistic simulation of the solar photospheric magnetoconvection model that mimics the quiet-Sun. In this case, we consider a uniform and constant value of the magnetic resistivity of 12.56 Ω m. We have found that the formation of the jet depends on the Lorentz force, which helps to accelerate the plasma upward. Analyzing various properties of the jet dynamics, we found that the jet structure shows a Doppler shift close to regions with high vorticity. The morphology, the upward velocity covering a range up to 130 km s−1, and the timescale formation of the structure between 60 and 90 s, are similar to those expected for Type II spicules.

Item Type: Article
Uncontrolled Keywords: magnetic reconnection; magnetohydrodynamics (MHD) ; methods: numerical; Sun: atmosphere; Sun: magnetic fields
Subjects: F500 Astronomy
Department: Faculties > Engineering and Environment > Mathematics, Physics and Electrical Engineering
Depositing User: Becky Skoyles
Date Deposited: 30 Apr 2018 14:07
Last Modified: 01 Aug 2021 08:49
URI: http://nrl.northumbria.ac.uk/id/eprint/34111

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