Acceleration of Plasma Flows in the Solar Atmosphere Due to Magnetofluid Coupling - Simulation and Analysis
Swadesh M. Mahajan, Nana L. Shatashvili, Solomon V. Mikeladze, Ketevan I. Sigua
Abstract
Within the framework of a two-fluid description possible pathways for the generation of fast flows (dynamical as well as steady) in the lower solar atmosphere is established. It is shown that a primary plasma flow (locally sub-Alfvénic) is accelerated when interacting with emerging/ambient arcade--like closed field structures. The acceleration implies a conversion of thermal and field energies to kinetic energy of the flow. The time-scale for creating reasonably fast flows (
≳100
km/s) is dictated by the initial ion skin depth while the amplification of the flow depends on local
β
. It is shown, for the first time, that distances over which the flows become "fast" are
∼0.01
R
s
from the interaction surface; later the fast flow localizes (with dimensions
≲0.05
R
S
) in the upper central region of the original arcade. For fixed initial temperature the final speed (
≳500km/s
) of the accelerated flow, and the modification of the field structure are independent of the time-duration (life-time) of the initial flow. In the presence of dissipation, these flows are likely to play a fundamental role in the heating of the finely structured Solar atmosphere.