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

Abstract

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.

Rapid Evolution of Type II Spicules Observed in Goode Solar Telescope On-disk Hα Images

“…This also implies that the H α component of type II spicules (RBEs), considered here may appear in the FOV before any other hotter component as a result of heating of cool plasma detected in Ca II 854.2 nm (Sekse et al 2013). However, their sudden in situ appearance in the H α -0.08 nm spectral window via transformation of existing features does not seem to be consistent with any of the models that interprets these events as jets originating in the lower chromosphere (e.g., González-Avilés et al 2018).…”

Analysis of 3D plasma motions in a chromospheric jet formed due to magnetic reconnection

“…7 and the Lorentz force is also bigger than pressure gradients |J × B| > |∇p| as shown in Fig. 7 of Paper González-Avilés et al (2018). This is important as it shows that torsional waves can be generated directly in the corona and therefore the whole wave energy (i.e without any loses due to propagation from the photosphere and dynamic chromosphere to the corona, as is usually suggested can be dissipated in the corona.…”

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Within the framework of resistive MHD, implementing the C7 equilibrium atmosphere model and a 3D potential magnetic field realistic configuration, we simulate the formation of a plasm jet with the morphology, upward velocity up to 130 km/s and timescale formation between 60 and 90 s after beginning of simulation, similar to those expected for Type II spicules. Initial results of this simulation were published in Paper (e.g., González-Avilés et al 2018) and present paper is devoted to the analysis of transverse displacements and rotational type motion of the jet. Our results suggest that 3D magnetic reconnection may be responsible for the formation of the jet in Paper (González-Avilés et al 2018).

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“…Initial results of this simulation were published in Paper (e.g., González-Avilés et al 2018) and present paper is devoted to the analysis of transverse displacements and rotational type motion of the jet. Our results suggest that 3D magnetic reconnection may be responsible for the formation of the jet in Paper (González-Avilés et al 2018). In this paper, by calculating times series of the velocity components v x and v y in different points near to the jet for various heights we find transverse oscillations in agreement with spicule observations.…”

In situgeneration of coronal Alfvén waves by jets

“…In this paper, we show that the jet with characteristics of a Type II spicule, obtained in the numerical simulations presented in González-Avilés et al (2018) shows transverse displacements and rotational type motion initially clockwise and anti-clockwise afterwards, that could be a driver to excite torsional Alfvén waves directly in the corona.…”