On the Electron-Cyclotron Maser Instability. II. Pulsations in the Quasi-stationary State

Details On the Electron-Cyclotron Maser Instability. II. Pulsations in the Quasi-stationary State On the Electron-Cyclotron Maser Instability. II. Pulsations in the Quasi-stationary State

Sep 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...332..466a&link_type=abstract

Astrophysical Journal v.332, p.466

Astronomy and Astrophysics

Astronomy

32

Instabilities, Masers, Plasmas, Sun: Radio Radiation

Scientific paper

In the previous paper we have studied the electron-cyclotron maser instability of a source in quasi-equilibrium. In a situation of weak diffusion such a state will remain for a limited time regardless of the particular loss-cone instability involved. Here our major interest is in oscillations set up by small disturbances around the steady state. Both the linear growth as well as the coupled diffusion rate are subject to a common oscillation period, since wave growth and diffusion are interlocked by a Lotka-Volterra type of coupled equations. Periods in the limit of small amplitude (limit cycle) of the self-organizing wave-particle system are investigated for the magnetoionic X- and O-mode and for harmonic numbers s = 1, 2 of the maser instability. Pulsation periods in the order of 1 s, as observed in the decimetric range of solar flare emission are found exist for (1) fundamental (s = 1) O-mode for 0.3 < ωp/Ωe ≲ 1.0, and (2) harmonic (s = 2) X-mode (for 1.0 ≲ ωp/Ωe 1.4). The period is sensitive to variations of the shape of the loss-cone and therefore not stable. The proposed model provides an interpretation of the observed quasi-periodic decimetric solar pulsations as well as some of similar stellar phenomena.

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