Mass loss is a key process in the evolution of massive stars, and must be understood
quantitatively if it is to be successfully included in broader astrophysical applications such as …

▪ Abstract This review deals with the winds from “normal” hot stars such as O-stars, B-and A-
supergiants, and Central Stars of Planetary Nebulae with O-type spectra. The advanced …

Building on results from the Magnetism in Massive Stars (MiMeS) project, this paper shows
how a two-parameter classification of massive-star magnetospheres in terms of the magnetic …

We present two-dimensional hydrodynamical simulations of corotating stream structure in
the wind from a rotating O star, together with resulting synthetic line profiles showing discrete …

Context. Recent results strongly challenge the canonical picture of massive star winds:
various evidence indicates that currently accepted mass-loss rates,, may need to be revised …

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 …

We present time-dependent hydrodynamical models of radiation driven hot star winds,
which are subject to a strong instability intrinsic to the radiative line force. The calculations …

As part of our search for the origin of stellar-wind variability, we have conducted
simultaneous ultraviolet and Hα spectroscopy of a number of bright O stars. The observed …

A quantitative analysis of time series of ultraviolet spectra from a sample of 10 bright O-type
stars (cf. Kaper et al. 1996, Paper I) is presented. The migrating discrete absorption …

Fourier analysis of two spectroscopic time series obtained with the IUE observatory confirm
that the ultraviolet stellar wind profiles of HD 64760 (B0. 5 Ib) are periodically variable. The …