169 research outputs found
Triggering an aurora
Ambient ionospheric electron density studied as triggering mechanism of aurora
Experiments with Magnetohydrodynamically Supported Shock Layers
Shock tube experiments to determine interaction of hypersonic flow with magnetic fiel
A limit on stably trapped particle fluxes
Limits of stably trapped particle fluxes - behavior of Whistler and ion cyclotron noise mode
Investigation of magnetospheric physics Technical status report, period ending 31 Mar. 1967
Magnetospheric physics - auroral zone structur
The production of BeV potential wells
Production of billion electron volt potential wells by cloud of electrons suspended in magnetic fiel
Collisionless shocks in plasmas
Collisionless shocks in plasmas, dissipation and dispersion in determining shock structur
Collisionless Magnetic Reconnection via Alfven Eigenmodes
We propose an analytic approach to the problem of collisionless magnetic
reconnection formulated as a process of Alfven eigenmodes' generation and
dissipation. Alfven eigenmodes are confined by the current sheet in the same
way that quantum mechanical waves are confined by the tanh^2 potential. The
dynamical time scale of reconnection is the system scale divided by the
eigenvalue propagation velocity of the n=1 mode. The prediction of the n=1 mode
shows good agreement with the in situ measurement of the
reconnection-associated Hall fields
Self-Regulation of Solar Coronal Heating Process via Collisionless Reconnection Condition
I propose a new paradigm for solar coronal heating viewed as a
self-regulating process keeping the plasma marginally collisionless. The
mechanism is based on the coupling between two effects. First, coronal density
controls the plasma collisionality and hence the transition between the slow
collisional Sweet-Parker and the fast collisionless reconnection regimes. In
turn, coronal energy release leads to chromospheric evaporation, increasing the
density and thus inhibiting subsequent reconnection of the newly-reconnected
loops. As a result, statistically, the density fluctuates around some critical
level, comparable to that observed in the corona. In the long run, coronal
heating can be represented by repeating cycles of fast reconnection events
(nano-flares), evaporation episodes, and long periods of slow magnetic stress
build-up and radiative cooling of the coronal plasma.Comment: 4 pages; Phys. Rev. Lett., in pres
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