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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 literatureAdvertised on -
It’s been decades since the need to study other stars to understand the past, present and future of the Sun was realized. One important aspect that has been investigated is the magnetic activity of stars for which we cannot fully grasp the mechanisms involved. Indeed, the origin of stellar magnetic cycles or the dependence of the magnetic activity on the stellar properties are not completely understood. This knowledge improves not only our understanding of the physics involved in stellar evolution but also affects the study of the Sun to better predict high-energy events and the betterAdvertised on -
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 barelyAdvertised on