How eruptions of a small filament feed materials to a nearby larger-scaled filament

ABSTRACT As one of the most common features in the solar atmosphere, filaments are significant not only in solar physics but also in stellar and laboratory plasma physics. With the New Vacuum Solar Telescope and the Solar Dynamics Observatory, here we report on multi-wavelength observations of eruptions of a small (30 arcsec) filament (SF) and its consequences while interacting with ambient magnetic features including a large (300 arcsec) filament (LF). The eruptions of the SF drive a two-side-loop jet that is a result of magnetic reconnection between the SF threads and an overlying magnetic channel. As a consequence of the eruption, the heating in the footpoints of the SF destabilizes the barbs of the LF rooted nearby. Supersonic chromospheric plasma flows along the barbs of the LF are then observed in the H α passband and they apparently feed materials to the LF. We suggest that they are shock-driven plasma flows or chromospheric evaporations, which can both be the consequences of heating in the chromosphere by non-thermal particles generated in the magnetic reconnection associated with the two-side-loop jet. Our observations demonstrate that the destabilization in the vicinity of the footpoints of a barb can drive chromospheric plasma feeding to the filament.

Control of Beam Halo-Chaos with Sinc Function in a Uniform-Focusing Channel

Based on the nonlinear control strategy of beam halo - chaos, this paper studies the sinc function control method of beam halo - chaos in uniform focusing magnetic channel. And we use Poincare section technology to simulate the beam envelope oscillations and single-particle trajectories. The results show that the use of this method can effectively eliminate beam halo and its regeneration, so that we can achieve effective control on beam halo - chaos.

Applied Model of Magnetization of a Granulated Material

Results of researches (of magnetic permeability) of elementary effective magnetic channel in porous (granulated) material are given. Such results permit to calculate a relative intensity of field between the grains.