We present a new insight into the propagation, attenuation and dissipation of two-fluid, torsional Alfv\'en waves in context heating lower solar atmosphere. By means numerical simulations partially-ionized plasma, we solve set two-fluid equations for ion plus electron neutral fluids three-dimensional (3D) Cartesian geometry. implement initially current-free magnetic field configuration, corresp...

The power spectra for line intensities of lower chro-mospheric lines N i 1319 A and C ii 1335 A are presented. On a number of occasions, intensity oscillations were seen to occur in N i at 3.7 mHz while C ii over the same spatial location showed oscillations close to 2.7 mHz. In a network region, the C ii line intensity was time-delayed by 1 min., compared to the N i line intensity. For network...

Coronal, transition region and chromospheric lines and centimeter radio emission of the quiet Sun have been simultaneously observed by SoHO and the VLA. The corona above the magnetic network has a higher pressure and is more variable than above the interior of supergranular cells. The Fourier transform in time is found to have steeper spectra in the corona and upper chromosphere than in the tra...

Abstract The ponderomotive force has been suggested to be the main mechanism produce so-called first ionization potential (FIP) effect—the enrichment of low-FIP elements observed in outer solar atmosphere, wind, and energetic events. It is well known that these occurs within chromosphere. Therefore, this phenomenon intimately tied plasma state chromosphere corona. For study, we combine IRIS obs...

Aims. To study the heating of solar chromospheric magnetic and nonmagnetic regions by acoustic magnetoacoustic waves, deposited acoustic-energy flux derived from observations strong lines is compared with total integrated radiative losses. Methods. A set 23 quiet-Sun weak-plage were observed in Mg II k h Interface Region Imaging Spectrograph (IRIS). The was Doppler velocities at two different g...

Abstract We present new results towards the explanation of chromospheric-heating problem and solar-wind origin, using a two-fluid model that takes into account collisional interaction between ions (protons) neutrals (hydrogen atoms). Our aim is to further reveal mechanism behind chromospheric heating plasma outflows. simulate analyse propagation evolution Alfvén waves in partially ionised solar...

With the recent advent of the Swedish 1-m Solar Telescope (SST), advanced image processing techniques, as well as numerical simulations that provide a more realistic view of the chromosphere, a comprehensive understanding of chromospheric jets such as spicules, mottles and fibrils is now within reach. In this paper, we briefly summarize results from a recent analysis of dynamic fibrils, short-l...

Aims. This paper aims to look at the propagation of synthetic photospheric oscillations from a point source into a two-dimensional non-magnetic solar atmosphere. It takes a particular interest in the leakage of 5-min global oscillations into the atmosphere, and aims to complement efforts on the driving of chromospheric dynamics (e.g. spicules and waves) by 5-min oscillations. Methods. A model s...