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<p>Plasmoid instability in magnetized plasmas, such as the solar corona, arises from the development of both linear and nonlinear magnetic reconnection processes. This instability releases the stored magnetic energy of the plasma in the form of kinetic and thermal energy. The phenomenon has been investigated from two perspectives: Magnetohydrodynamic (MHD) simulations and Particle-in-Cell (PIC) simulations. In MHD simulations, the Lundquist number is commonly used to estimate the threshold for the onset of this instability. In this paper, we present a new approximation for the initial magnetic power density in plasma, which defines the formation threshold of plasmoid instability in PIC simulations. According to this approximation, the initial magnetic power density depends on parameters such as the initial magnetic field strength and the width of the current sheet. A numerical value for the initial magnetic power density is derived from solar coronal simulation results. PIC simulations demonstrate that plasmoid instability occurs if the initial plasma power exceeds <InlineEquation ID="IEq1"> <EquationSource Format="MATHML"><math> <mo>∼</mo> <mn>1.71</mn> <mo>×</mo> <msup> <mrow> <mn>10</mn> </mrow> <mrow> <mn>2</mn> </mrow> </msup> <mspace width="0.3em" /> <mtext>erg</mtext> <mo>.</mo> <msup> <mtext>cm</mtext> <mrow> <mo>−</mo> <mn>3</mn> </mrow> </msup> <mo>.</mo> <msup> <mtext>s</mtext> <mrow> <mo>−</mo> <mn>1</mn> </mrow> </msup> </math></EquationSource> <EquationSource Format="TEX">$\sim 1.71 \times 10^{2}~\text{erg}.\text{cm}^{ - 3}.\text{s}^{ - 1}$</EquationSource> </InlineEquation>.</p>

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On the Formation of Collisionless Plasmoid Instability in Particle-in-Cell Simulations of the Solar Corona

  • 期刊论文

  • 发表日期：

    2025年12月15日

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  • Mahdi Shahraki pour

摘要

Plasmoid instability in magnetized plasmas, such as the solar corona, arises from the development of both linear and nonlinear magnetic reconnection processes. This instability releases the stored magnetic energy of the plasma in the form of kinetic and thermal energy. The phenomenon has been investigated from two perspectives: Magnetohydrodynamic (MHD) simulations and Particle-in-Cell (PIC) simulations. In MHD simulations, the Lundquist number is commonly used to estimate the threshold for the onset of this instability. In this paper, we present a new approximation for the initial magnetic power density in plasma, which defines the formation threshold of plasmoid instability in PIC simulations. According to this approximation, the initial magnetic power density depends on parameters such as the initial magnetic field strength and the width of the current sheet. A numerical value for the initial magnetic power density is derived from solar coronal simulation results. PIC simulations demonstrate that plasmoid instability occurs if the initial plasma power exceeds ∼ 1.71 × 10 2 erg . cm − 3 . s − 1 $\sim 1.71 \times 10^{2}~\text{erg}.\text{cm}^{ - 3}.\text{s}^{ - 1}$ .