Magnetic Reconnection resulting from Flux Emergence: Implications for Jet Formation in the lower solar atmosphere?

Abstract

We aim at investigating the formation of jet-like features in the lower solar atmosphere, e.g. chromosphere and transition region, as a result of magnetic reconnection. Magnetic reconnection as occurring at chromospheric and transition regions densities and triggered by magnetic flux emergence is studied using a 2.5D MHD code. The initial atmosphere is static and isothermal, with a temperature of 20,000 K. The initial magnetic field is uniform and vertical. Two physical environments with different magnetic field strength (25 G and 50 G) are presented. In each case, two sub-cases are discussed, where the environments have different initial mass density. In the case where we have a weaker magnetic field (25 G) and higher plasma density ($N_e=2\times 10^{11}$ cm${}^{-3}$), valid for the typical quiet Sun chromosphere, a plasma jet would be observed with a temperature of 2--3 $\times 10^4$ K and a velocity as high as 40 km/s. The opposite case of a medium with a lower electron density ($N_e=2\times 10^{10}$ cm${}^{-3}$), i.e. more typical for the transition region, and a stronger magnetic field of 50 G, up-flows with line-of-sight velocities as high as 90 km/s and temperatures of 6 $\times$ 10${}^5$ K, i.e. upper transition region -- low coronal temperatures, are produced. Only in the latter case, the low corona Fe IX 171 Å shows a response in the jet which is comparable to the O V increase. The results show that magnetic reconnection can be an efficient mechanism to drive plasma outflows in the chromosphere and transition region. The model can reproduce characteristics, such as temperature and velocity for a range of jet features like a fibril, a spicule, an hot X-ray jet or a transition region jet by changing either the magnetic field strength or the electron density, i.e. where in the atmosphere the reconnection occurs.

11 pages, 13 figures, 2 tables

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• Generation of quasi-periodic waves and flows in the solar atmosphere by oscillatory reconnection
• Numerical Simulation of Solar Microflares in a Canopy-Type Magnetic Configuration
• Investigating the Transition Region Explosive Events and Their Relationship to Network Jets
• Imaging evidence for solar wind outflows originating from a CME footpoint
• Macrospicules and Their Connection to Magnetic Reconnection in the Lower Atmosphere
• Spicule jets in the solar atmosphere modeled with resistive MHD and thermal conduction
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• The Relation between Solar Spicules and Magnetohydrodynamic Shocks
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• Spicules in IRIS Mg II Observations: Automated Identification
• On the Relationship between Solar Spicules and Propagating Coronal Disturbances: The Role of Shocks
• Magnetic reconnection in partially ionized plasmas
• Spectroscopic Case Studies of Four Long-duration Transition-region Explosive Events