A new cyclotron maser radiation mechanism in space plasmas

R Bingham, R A Cairns

Research output: Contribution to journalArticle

Abstract

In this paper, we discuss a new cyclotron maser type instability driven by a crescent or horseshaped electron distribution function. Such distribution functions are easily created by an electron beam moving into a stronger magnetic field region, where conservation of the first adiabatic invariant causes an increase in their pitch angle. This produces a broad region on the distribution function where ∂fe/∂v⊥ > 0. Planetary dipole magnetic fields are examples of where these types of distributions can be found. We examine the stability of these electron horseshoe distribution functions for right-hand extraordinary mode (R–X mode) radiation close to the electron cyclotron frequency propagating perpendicular to the magnetic field using both non-relativistic and relativistic beams.
LanguageEnglish
Pages160-162
Number of pages3
JournalPhysica Scripta
VolumeT98
DOIs
Publication statusPublished - 2002

Fingerprint

space plasmas
masers
cyclotrons
Distribution Function
Plasma
distribution functions
Radiation
Magnetic Field
radiation
Electron
Crescent
magnetic fields
Adiabatic Invariant
Horseshoe
pitch (inclination)
cyclotron frequency
Electron Beam
electron distribution
Perpendicular
Dipole

Keywords

  • microinstabilities
  • plasma interactions
  • radiation mechanisms
  • polarization

Cite this

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A new cyclotron maser radiation mechanism in space plasmas. / Bingham, R; Cairns, R A.

In: Physica Scripta, Vol. T98, 2002, p. 160-162.

Research output: Contribution to journalArticle

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AU - Cairns, R A

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AB - In this paper, we discuss a new cyclotron maser type instability driven by a crescent or horseshaped electron distribution function. Such distribution functions are easily created by an electron beam moving into a stronger magnetic field region, where conservation of the first adiabatic invariant causes an increase in their pitch angle. This produces a broad region on the distribution function where ∂fe/∂v⊥ > 0. Planetary dipole magnetic fields are examples of where these types of distributions can be found. We examine the stability of these electron horseshoe distribution functions for right-hand extraordinary mode (R–X mode) radiation close to the electron cyclotron frequency propagating perpendicular to the magnetic field using both non-relativistic and relativistic beams.

KW - microinstabilities

KW - plasma interactions

KW - radiation mechanisms

KW - polarization

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