The next generation of solar observatories aim to understand the magnetism of the solar chromosphere. Therefore, it is crucial to understand the polarimetric signatures of chromospheric spectral lines. For this purpose, we here examine the suitability of the three Fraunhofer Mg I b1, b2, and b4 lines at 5183.6, 5172.7, and 5167.3 Å, respectively

Wie bei menschlichen Zwillingen können sich auch Sternzwillinge durchaus starkvoneinander unterscheiden. Wie sehr, das hängt in erster Linie von der jeweiligen Masse der Geschwistersterne und deren Massenverhältnis zueinander ab. Doppelsterne werden meist gemeinsam geboren. Es ist dann ihre jeweilige Masse, die über deren

Wie bei menschlichen Zwillingen kännen sich auch Sternzwillinge durchaus stark voneinander unterscheiden. Wie sehr, das hängt in erster Linie von der jeweiligen Masse der Geschwistersterne und deren Massenverhältnis zueinander ab.

We explore the stellar structure of the Large Magellanic Cloud (LMC) disk using data from the Survey of the MAgellanic Stellar History and the Dark Energy Survey. We detect a ring-like stellar overdensity in the red clump star count map at a radius of ∼6° (∼5.2 kpc at the LMC distance) that is continuous over ∼270° in position angle and is only

The number of ultra-diffuse galaxies (UDGs) in clusters is of significant importance to constrain models of their formation and evolution. Furthermore, their distribution inside clusters may tell us something about their interactions with their environments. In this work, we revisit the abundance of UDGs in a more consistent way than in previous

The quality of images of the Sun obtained from the ground are severely limited by the perturbing effect of the Earth's turbulent atmosphere. The post-facto correction of the images to compensate for the presence of the atmosphere require the combination of high-order adaptive optics techniques, fast measurements to freeze the turbulent atmosphere