Understanding the magnetic field in the corona is key for explaining the fascinating physical processes occurring there. However, the extreme conditions in the outer solar atmosphere hamper the possibility of acquiring observations with enough quality to infer the coronal magnetic field. Analyzing observations of overdensities of cold plasma supported by coronal magnetic fields, including filaments and prominences, allows us to understand such magnetic fields and their interaction with plasma. In this study, we have analyzed an active region prominence, a type of prominence that has barely

The properties of blue supergiants are key for constraining the end of the main sequence phase, a phase during which massive stars spend most of their lifetimes. The lack of fast-rotating stars below 21.000K, a temperature around which stellar winds change in behaviour, has been proposed to be caused by enhanced mass-loss rates, which would spin down the star. Alternatively, the lack of fast-rotating stars may be the result of stars reaching the end of the main sequence. Here, we combine newly derived estimates of photospheric and wind parameters, wind terminal velocities from the literature