Ion-Ion Two-Stream Instability in Relativistic Solar and Astrophysical Phenomena

Details Ion-Ion Two-Stream Instability in Relativistic Solar and Astrophysical Phenomena Ion-Ion Two-Stream Instability in Relativistic Solar and Astrophysical Phenomena

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agufmsh52a0493k&link_type=abstract

American Geophysical Union, Fall Meeting 2002, abstract #SH52A-0493

Astronomy and Astrophysics

Astrophysics

7514 Energetic Particles (2114), 7519 Flares, 7815 Electrostatic Structures, 7843 Numerical Simulation Studies, 7871 Waves And Instabilities

Scientific paper

One of the proposed mechanisms for heating and particle acceleration in solar flares is through the action of a DC electric field upon a thermal plasma. Using numerical particle simulations, we show that the action of the electric fields in relativistic situations (produced either through long-acting fields or sufficiently high field strengths) leads both to direct electron and ion acceleration and to further acceleration due, initially, to the electron two-stream instability. A direct consequence of the electron two stream instability in the relativistic regime is the excitation of the ion-ion two-stream instability. This arises through electron-depletion in the phase space occupied by the ions while simultaneously the generation of relativistic electrons also acts to hinder electrons from canceling out the collective electric field fluctuations of the ion distribution. Thus the ion distribution becomes unstable under the action of the electric field and through wave-particle interactions. We show under what conditions such an ion-ion two-stream instability can arise and the conditions that could produce high-energy ions such as are observed in solar flares and in astrophysical phenomena.

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