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

Abstract

Using simulated data-driven three-dimensional resistive MHD simulations of the solar atmosphere, we show that magnetic reconnection can be responsible of the formation of jets with characteristic of Type II spicules. For this, 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 solar photospheric magnetoconvection model which is mimicking quiet-Sun. In this case we consider a uniform and constant value of the magnetic resistivity of $12.56\Omega \mathrm{m}$. We have found that formation of the jets depends on the Lorentz force, which helps to accelerate the plasma upwards. Analyzing various properties of the jet dynamics, we found that the jet structure shows Doppler shift near to regions with high vorticity. The morphology, upward velocity, covering a range up to 100 $\mathrm{km}$ ${\mathrm{s}}^{-1}$, and life-time of the estructure, bigger than 100 $\mathrm{s}$, are similar to those expected for Type II spicules.

11 pages, 12 figures; Accepted for publication in the Astrophysical Journal

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Cited by in corpus (10)

• Generation of Solar Spicules and Subsequent Atmospheric Heating
• Small-scale solar jet formation and their associated waves and instabilities
• Rapid Evolution of Type II Spicules Observed in Goode Solar Telescope On-Disk H-alpha Images
• Spicule jets in the solar atmosphere modeled with resistive MHD and thermal conduction
• Numerical simulations of macrospicule jets under energy imbalance conditions in the solar atmosphere
• The effect of linear background rotational flows on magnetoacoustic modes of a photospheric magnetic flux tube
• Role of magnetic arcades in explaining the puzzle of the gamma-ray emission from the solar disk
• Analysis of 3D plasma motions in a chromospheric jet formed due to magnetic reconnection
• Flows and magnetic field structures in reconnection regions of simulations of the solar atmosphere: do flux pile-up models work?
• Influence of the magnetic field topology in the evolution of small-scale two-fluid jets in the solar atmosphere