Langmuir Instabilities in the Solar Wind Plasma

Details Langmuir Instabilities in the Solar Wind Plasma Langmuir Instabilities in the Solar Wind Plasma

Apr 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996apj...461..472c&link_type=abstract

Astrophysical Journal v.461, p.472

Astronomy and Astrophysics

Astronomy

Instabilities, Plasmas, Sun: Solar Wind

Scientific paper

The development of the anisotropy of the electron distribution function in the lower solar corona has been studied through a test-particle model, revealing that particles with υ∥>5re will eventually run away owing to the magnetic pumping effect. The scaling with υ∥ of the parallel distribution function and of the perpendicular temperature is also derived. The theory shows a suprathermal tail originated near the coronal base that dominates the energy flux at distances r ≃ 4 Rsun. We analyze the high-frequency instability produced by the small anisotropy in perpendicular energy of the runaway electron distribution in the magnetized plasma of the solar wind. A phenomenological description of this instability is obtained. It is also reported that the stability behavior is uncorrelated with the perpendicular temperature profile. The efficiency of Langmuir oscillations as a heating mechanism for the solar wind is discussed.

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