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An electric field suffers a discontinuity at a surface charge. Similarly, a magnetic field is discontinuous at a surface current. The perpendicular component of a magnetic field is continuous across the interface of two magnetic mediums. In contrast, its parallel component, perpendicular to the current, is discontinuous by the amount equal to the product of the vacuum permeability and the surface current. Like the scalar potential in electrostatics, the vector potential is also continuous...
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In electrostatics, the electric field can be written as the negative gradient of the potential. In magnetostatics, the zero divergence of the magnetic field ensures that the magnetic field can be expressed as the curl of a vector potential. This potential is known as the magnetic vector potential.
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Relativistic Asymmetric Magnetic Reconnection.

Rostom Mbarek1, Colby Haggerty2, Lorenzo Sironi3

  • 1Department of Astronomy and Astrophysics, University of Chicago, Chicago, Illinois 60637, USA; Kavli Institute for Cosmological Physics, The University of Chicago, Chicago, Illinois 60637, USA and Enrico Fermi Institute, The University of Chicago, Chicago, Illinois 60637, USA.

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Area of Science:

  • Plasma Physics
  • Astrophysical Phenomena
  • Computational Physics

Background:

  • Relativistic magnetic reconnection is a key process in high-energy astrophysical systems.
  • Asymmetric inflow conditions are common but less understood in these phenomena.

Purpose of the Study:

  • Derive scaling equations for relativistic magnetic reconnection under asymmetric inflows.
  • Predict outflow Lorentz factor and reconnection rate.
  • Understand the impact of asymmetry on particle acceleration and emission.

Main Methods:

  • Developed theoretical scaling equations for asymmetric relativistic magnetic reconnection.
  • Performed kinetic particle-in-cell simulations to validate theoretical predictions.

Main Results:

  • Scaling equations accurately predict outflow speeds and nonthermal spectral index.
  • Outflow characteristics are constrained by the weaker inflowing plasma.
  • Simulations confirm agreement with theoretical scaling predictions.

Conclusions:

  • Asymmetry plays a critical role in relativistic magnetic reconnection dynamics.
  • The derived scaling provides a quantitative framework for asymmetric reconnection.
  • Essential for modeling nonthermal emission in magnetically dominated astrophysical environments.