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To escape the Earth's gravity, an object near the top of the atmosphere at an altitude of 100 km must travel away from Earth at 11.1 km/s. This speed is called the escape velocity. The temperature at which gas molecules attain the rms speed, which is equal to the escape velocity, can be estimated by using the equation for the average kinetic energy of the gas molecules. According to the kinetic theory of gas, the average kinetic energy of the gas molecules is proportional to its...
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An object absorbing an electromagnetic wave would experience a force in the direction of propagation of the wave. This force occurs because electromagnetic waves contain and transport momentum. The force accounts for the wave's radiation pressure exerted on the object. Maxwell's prediction was confirmed in 1903 by Nichols and Hull by precisely measuring radiation pressures with a torsion balance. The measuring instrument had mirrors suspended from a fiber kept inside a glass container.
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The escape velocity of an object is defined as the minimum initial velocity that it requires to escape the surface of another object to which it is gravitationally bound and never to return. For example, what would be the minimum velocity at which a satellite should be launched from the Earth's surface such that it just escapes the Earth's gravitational field?
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No object with a finite mass can travel faster than the speed of light in a vacuum. This fact has an interesting consequence in the domain of extremely high gravitational fields.
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The radiation pressure applied by an electromagnetic wave on a perfectly absorbing surface equals the energy density of the wave. The wave's momentum also gets transferred to the surface when an electromagnetic wave is entirely absorbed by it. The rate at which momentum is transmitted to an absorbing surface perpendicular to the propagation direction equals the force on the surface.
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Leaking Outside the Box: Kinetic Turbulence with Cosmic-Ray Escape.

Evgeny A Gorbunov1, Daniel Grošelj1, Fabio Bacchini1,2

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Particle acceleration in turbulent pair plasmas reaches steady states, forming nonthermal particle distributions. Higher plasma magnetization increases cosmic ray energy fraction, exceeding 50% in some cases.

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Area of Science:

  • Plasma Physics
  • Astrophysics
  • Computational Physics

Background:

  • Turbulent plasmas are crucial in astrophysical phenomena.
  • Understanding particle acceleration mechanisms is key to explaining high-energy cosmic phenomena.

Purpose of the Study:

  • To investigate particle acceleration in strongly turbulent pair plasmas.
  • To explore the formation of steady-state, nonthermal particle distributions.
  • To determine the impact of plasma magnetization on acceleration efficiency and energy partitioning.

Main Methods:

  • Utilizing novel 3D particle-in-cell simulations.
  • Incorporating particle injection from an external heat bath.
  • Modeling diffusive particle escape from the system.

Main Results:

  • Demonstrated the formation of steady-state, nonthermal particle distributions.
  • Observed maximum particle energies reaching the Hillas limit.
  • Identified plasma pressure equilibration as a limiting factor for acceleration rate.
  • Found harder nonthermal power-law spectra with increasing cold plasma magnetization (σ₀).
  • Showed that escaping cosmic rays can account for over 50% of dissipated energy at σ₀≳1.

Conclusions:

  • Steady-state particle acceleration is achievable in turbulent pair plasmas.
  • Plasma magnetization significantly influences the characteristics of accelerated particles and energy distribution.
  • The developed simulation method enables kinetic studies of particle acceleration in astrophysical systems.