ﻻ يوجد ملخص باللغة العربية
We present a method to study the penumbral fine structure using data obtained by the spectropolarimeter onboard HINODE. For the first time, the penumbral filaments can be considered as resolved in spectropolarimetric measurements. This enables us to use inversion codes with only one-component model atmospheres, and thus assign the obtained stratifications of plasma parameters directly to the penumbral fine structure. This approach is applied to the limb-side part of the penumbra in active region NOAA 10923. The preliminary results show a clear dependence of the plasma parameters on continuum intensity in the inner penumbra, i.e. weaker and horizontal magnetic field along with increased line-of-sight velocity are found in the low layers of the bright filaments. The results in the mid penumbra are ambiguous and future analyses are necessary to unveil the magnetic field structure and other plasma parameters there.
We studied the physical parameters of the penumbra in a large and fully-developed sunspot, one of the largest over the last two solar cycles, by using full-Stokes measurements taken at the photospheric Fe I 617.3 nm and chromospheric Ca II 854.2 nm l
Given the piecewise approach to modeling intermolecular interactions for force fields, they can be difficult to parameterize since they are fit to data like total energies that only indirectly connect to their separable functional forms. Furthermore,
We perform the scanning tunneling spectroscopy based superconductor-vacuum-superconductor analogue to the seminal McMillan and Rowell superconductor-insulator-superconductor device study of phonons in the archetypal elemental superconductor Pb [W. L.
Penumbral microjets (PMJs) are short-lived, jet-like objects found in the penumbra of sunspots. They were first discovered in chromospheric lines and have later also been shown to exhibit signals in transition region (TR) lines. Their origin and mann
In this paper, the photon stationary transport equation has been extended from $mathbb{R}^3$ to $mathbb{C}^3$. A solution of the inverse problem is obtained on a hyper-sphere and a hyper-cylinder as X-ray and Radon transform, respectively. We show th