Magnetic fields play a dominant role in the atmospheres of the Sun and other Sun-like stars. Outside sunspot regions, the photosphere of the so-called quiet Sun contains myriads of small-scale magnetic concentrations, with strengths ranging from the detection limit of ∼1016 Mx up to ∼ Mx. The tireless motion of these magnetic 20 3 # 10 flux concentrations, along with the continual appearance an...

This article is a continuation of the works1-4 author, devoted to elucidating physical nature dark sunspots. It has been proven that scientific paradigm cold sunspots prevailing in solar physics erroneous, since it contradicts second law thermodynamics. photosphere can only be hotter than photosphere, and their visual darkness non-thermal nature. Sunspots are hottest areas Sun's surface, temper...

Abstract The electromagnetic energy flux in the lower atmosphere of Sun is a key tool to describe balance solar atmosphere. Current investigations on focus primarily vertical through photosphere, ignoring Poynting other directions and its possible contributions local heating. Based realistic Bifrost simulation quiet-Sun (coronal hole) atmosphere, we find that total photosphere occurs mainly par...

Aims. We investigate the oscillatory properties of the quiet solar chromosphere in relation to the underlying photosphere, with particular regard to the effects of the magnetic topology. Methods. For the first time we perform a Fourier analysis on a sequence of line-of-sight velocities measured simultaneously in a photospheric (Fe I 709.0 nm) and a chromospheric line (Ca II 854.2 nm). The veloc...

We introduce and apply a method to investigate the force-free character of the photospheric magnetic fields in solar active regions. The vertical current density, inferred from vector magnetograms, is decomposed into a helical (assumed field-aligned) component, and a component perpendicular to the magnetic field. Contrary to the classical method of calculating the integrated Lorentz forces, the...

Recent progress in realistic simulations of solar convection have given us an unprecedented opportunity to evaluate the robustness of solar interior structures and dynamics obtained by methods of local helioseismology. We present results of testing the time-distance method using realistic simulations. By computing acoustic wave propagation time and distance relations for different depths of the...

Context. Chromospheres and coronae are common phenomena on solar-type stars. Understanding the energy transfer to these heated atmospheric layers requires direct access to the relevant empirical data. Study of these structures has, by and large, been limited to the Sun thus far. Aims. The region of the temperature reversal can be directly observed only in the far infrared and submillimetre spec...