The evolution of massive stars is affected by a variety physical processes including convection, rotation, mass loss and binary interaction. Because these modify the internal chemical abundance profiles in multiple ways simultaneously, it can be challenging to determine which properties stellar interior are primarily driving overall evolution. Building on previous work, we develop new modelling...

In previous work we identified a population of 38 cool and luminous variable stars in the Magellanic Clouds examined 11 detail order to classify them as either Thorne-\.Zytkow Objects (T\.ZOs, red supergiants with neutron star cores) or super-AGB (the most massive that will not undergo core collapse). This includes HV\,2112, peculiar previously considered other works be T\.ZO high-mass AGB star...

Inspired by an appeal to the community fromWalborn (these proceedings) we decided to solve the long-standing problem concerning the nature of the 4486, 4504Å emission lines, which are frequently observed in O-type spectra and which are particularly prominent in supergiants. We claim that these lines emerge from sulfur, namely by deexcitation of a highly excited S IV doublet state. We prove this...

We have obtained linear polarization measurements of the Large Magellanic Cloud B[e] supergiant S 111 using optical imaging polarimetry. The intrinsic polarization found is consistent with the presence of an axisymmetric circumstellar envelope. We have additionally estimated the electron density for S 111 using data from the literature and revisited the correlation between polarization and enve...

The massive stars that survive the phase of red supergiants (RSGs) spend rest their life in extremity. Their unstable atmospheres facilitate formation and episodic ejection shells alter stellar appearance surroundings. In present study, we revise evolutionary state eight hypergiants Magellanic Clouds, four early-A type FG type, complement short list eruptive post-RSGs termed as yellow (YHGs). W...