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August 1, 2026Solar PhysicsOpen Access

Magnetic Reconnection Process in Partially Ionized Fluids: Insights from the Solar Chromosphere

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Authors

AMAdrian R. Montañez-LoboFLF. D. Lora-Clavijo

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Overview

Numerical simulation demonstrates enhanced magnetic reconnection and plasma heating in the solar chromosphere, indicating charged-neutral collisions drive energy release.

Key Points

  • To investigate the morphology and energy release of magnetic reconnection in the partially ionized solar chromosphere, focusing on the effects of elastic collisions, ionization, and recombination.
  • Simulated 2.5D resistive magnetohydrodynamics with two-fluid (charged and neutral) interactions using an updated version of the MAGNUS code.
  • Applied a mixed explicit-implicit numerical scheme to handle the stiffness of collision, ionization, and recombination terms.
  • Modeled quiet Sun chromosphere conditions across three magnetic field strengths: 100 G, 110 G, and 120 G.
  • Reconnection heated plasma components by 18% to 110%, yielding maximum reconnection rates of 0.226, 0.253, and 0.279 for 100 G, 110 G, and 120 G fields, respectively.
  • Released total energy between 10^22 and 10^23 erg within a chromospheric volume of 0.4 × 0.01 × 0.4 Mm³, driven primarily by charged-neutral collisions rather than plasma beta increases.
  • Ionization and recombination effects peaked in zones of maximum temperature where particle acceleration occurs.

Cite This Study

Montañez-Lobo et al. (2026) studied this question.

synapsesocial.com/papers/6ab083dc8954ddecfffab5dehttps://doi.org/10.1007/s11207-026-02714-1
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