Waves and oscillations have been observed in the Sun's atmosphere for over half a century.
While such phenomena have readily been observed across the entire electromagnetic …

The evolution of active regions (AR) from their emergence through their long decay process
is of fundamental importance in solar physics. Since large-scale flux is generated by the …

An overview is given of the observational and the theoretical methods used to investigate
solar magnetic fields. It includes an introduction to the Stokes parameters, their radiative …

This publication provides an overview of magnetic fields in the solar atmosphere with the
focus lying on the corona. The solar magnetic field couples the solar interior with the visible …

Context. CHROMIS, a new imaging spectrometer at the Swedish 1-m Solar Telescope
(SST), can observe the chromosphere in the H and K lines of Ca II at high spatial and …

We analyze observations from the Interface Region Imaging Spectrograph of the Mg ii k line,
the Mg ii UV subordinate lines, and the O i 135.6$\mathrm {nm} $ line to better understand …

Magnetic fields on the surface of the Sun and stars in general imprint or modify the
polarization state of the electromagnetic radiation that is leaving from the star. The inference …

The intensities of submillimeter and millimeter continua, which are formed in LTE and
depend linearly on temperature, may be able to provide a test of models of the Solar …

Context. The role of magnetic fields in the chromospheric heating problem remains greatly
unconstrained. Most theoretical predictions from numerical models rely on a magnetic …

Solar carbon monoxide spectra indicate the existence of a cool (less than 4000 kelvin)
component to the solar chromosphere coexisting with the hot, bright gas at 6000 to 7000 …