The loopy Sun: resolving the small-scale solar magnetism
Solar magnetism may look deceptively boring (a rather common star with relatively low activity). As it turns out, even the most quiet areas of the Sun (away...
The Magnetic Sensitivity of the (250-278 nm) Fe II Polarization Spectrum
This paper presents a theoretical investigation of the polarization and magnetic sensitivity of the near-ultraviolet (near-UV) solar spectral lines of Fe II...
The Plasma β in Quiet Sun Regions: Multi-instrument View
A joint campaign of several spaceborne and ground-based observatories, such as the GREGOR solar telescope, the Extreme-ultraviolet Imaging Spectrometer (EIS)...
The Potential of the Wavelength-integrated Scattering Polarization of the Hydrogen Lyα Line for Probing the Solar Chromosphere
The intensity and the linear scattering polarization profiles of the hydrogen Lyα line encode valuable information on the thermodynamic and magnetic structure...
The chromosphere is the interface between the photospheric solar surface and the outer corona and wind. In this complex domain thesolar gas becomes transparent...
The stochastic, intermittent nature of quiet Sun magnetism
The quiet Sun (the 99%, or more, of the solar surface not covered by sunspots or active regions) is receiving increased attention in recent years; its role on...
Tomography of a Solar Plage with the Tenerife Inversion Code
We apply the Tenerife Inversion Code (TIC) to the plage spectropolarimetric observations obtained by the Chromospheric LAyer SpectroPolarimeter (CLASP2). These...
Using the Hanle Effect in Mg II k to Quantify the Open Flux above the Solar Poles
We test the use of the Mg II resonant lines for measurement of the magnetic field at the top of the chromosphere of polar coronal holes (CHs). The Hanle effect...
Magnetic fields break through the solar surface in a hierarchy of magnetic elements ranging from Earth-sized sunspots down to tiny concentrations that are...