Fine-scale structure in the corona appears not to be well resolved by current imaging instruments. Assuming this to be true offers a simple geometric explanation for several current puzzles in coronal physics, including the apparent uniform cross section of bright threadlike structures in the corona, the low EUV contrast ( long apparent scale height) between the top and bottom of active region ...

The plasma contributing to emission from the Sun between cool chromosphere ($\le 10^4$K) and hot corona ($\ge 10^6$K) has been subjected many different interpretations. Here we look at magnetic structure of this transition region (TR) plasma, based upon implications CLASP2 data an active recently published by Ishikawa et al., earlier IRIS SDO quiet regions. al. found that large areas sunspot pl...

A kinetic model of the solar wind based on Kappa velocity distribution functions for the electrons and protons escaping out of the corona is presented. The high velocity particles forming the tail of these distribution functions have an enhanced phase space density compared to a Maxwellian. The existence of such velocity distribution functions have been introduced in the pioneering work of Scud...

The atmospheric pressure non-thermal plasma has been extensively studied for decomposing environmental pollutants such as SOx [1], NOx [2,3], and VOCs [4,5] (volatile organic compounds). Many researchers have been engaged in developing removal technique of those toxic pollutants with the non-thermal plasma. A high energy electron beam (EB) irradiation is also very effective to remove SOx, NOx i...

Solar prominences are cool 10(4) kelvin plasma clouds supported in the surrounding 10(6) kelvin coronal plasma by as-yet-undetermined mechanisms. Observations from Hinode show fine-scale threadlike structures oscillating in the plane of the sky with periods of several minutes. We suggest that these represent Alfvén waves propagating on coronal magnetic field lines and that these may play a role...

The solar corona is the hot, ionized outer atmosphere of the Sun. Coronal plasma expands into interplanetary space as a supersonic bulk outflow known as the solar wind. This tenuous and unbounded medium is a unique laboratory for the study of kinetic theory in a nearly collisionless plasma, as well as magnetohydrodynamic waves, shocks, and jets. Particle velocity distributions in the solar wind...

The heliosphere is filled with solar wind, which formed due to the expansion of plasma hot corona [...]

Electrons produced in atmospheric pressure corona discharges are used for a ûariety of beneficial purposes including the destruction of gaseous contaminants, and surface treatment. In other applications, such as electrostatic precipitators and photocopiers, unintended reactions such as ozone production and deposition of silicon dioxide are detrimental. In both situations, a kinetic description ...

The paper discusses the diagnostics of plasma jets in solar corona with use data from modern space- and ground-based telescopes observing Sun extreme ultraviolet (EUV) micro- wave bands. We examine observational parameters EUV radio emission events associated jets, depending on mechanism formation, initiation conditions, evolution jets. opportunities provided by study which relies simultaneous ...

Aims. Estimating Alfvén speeds is of interest in modelling the solar corona, studying the coronal heating problem and understanding the initiation and propagation of coronal mass ejections (CMEs). Methods. We assume here that the corona is in a magnetohydrostatic equilibrium and that, because of the low plasma β, one may decouple the magnetic forces from pressure and gravity. The magnetic field...