Massive stars have strong stellar winds that direct their evolution through the upper
Hertzsprung–Russell diagram and determine the black hole mass function. Furthermore …

Massive stars, at least∼ 10 \sim10 times more massive than the Sun, have two key
properties that make them the main drivers of evolution of star clusters, galaxies, and the …

Double neutron star (DNS) systems represent extreme physical objects and the endpoint of
an exotic journey of stellar evolution and binary interactions. Large numbers of DNS systems …

Context. The star cluster R136 inside the Large Magellanic Cloud hosts a rich population of
massive stars, including the most massive stars known. The strong stellar winds of these …

Context. Reliable predictions of mass-loss rates are important for massive-star evolution
computations. Aims. We aim to provide predictions for mass-loss rates and wind-momentum …

Mass-loss rates and terminal wind velocities are key parameters that determine the kinetic
wind energy and momenta of massive stars. Furthermore, accurate mass-loss rates …

Context. The 30 Doradus (30 Dor) region of the Large Magellanic Cloud, also known as the
Tarantula nebula, is the nearest starburst region. It contains the richest population of …

The evolution and fate of very massive stars (VMS) is tightly connected to their mass-loss
properties. Their initial and final masses differ significantly as a result of mass loss. VMS …

Context. The spectral analysis of hot, massive stars is a fundamental astrophysical method
of determining their intrinsic properties and feedback. With their inherent, radiation-driven …

Context. Massive Wolf–Rayet (WR) stars dominate the radiative and mechanical energy
budget of galaxies and probe a critical phase in the evolution of massive stars prior to core …