Found 3 talks width keyword winds

Thursday February 28, 2019
Prof. Alex Fullerton
Space Telescope Science Institute


The growth of astrophysical understanding typically results fromthe constructive interplay between theoretical ideas andobservational insights, with each mode of exploration drivingprogress at different times. The result is invariably a morecomplicated but richer picture of the phenomenon than initiallyenvisaged, as well as deeper appreciation of the behavior ofcomplex systems.In this talk, I will use the development of our understanding ofthe structure of outflows from massive O- and B-type stars toillustrate this collaborative “dance”. Starting from the smooth,spherically symmetric models for radiatively driven windsdeveloped in the late 1960s, our view of these outflows hasevolved to include the growth of inhomogeneities on a variety ofspatial scales. Explanations for the origin of this structure havein turn prompted the realization that non-radiative processesmust also shape the emergence of the wind from the stellarphotosphere. Consequently, O- and B-type stars are morecomplicated – and interesting! – objects than often thought.While many fruitful avenues of research remain to be explored,the current paradigm provides a (mostly) self-consistent pictureof massive stars and their outflows.

Thursday March 1, 2012
Dr. Selma de Mink
Space Telescope Science Institute, Baltimore


Although they are rare and short-lived, massive stars play a major role in Universe. With their large luminosities, strong stellar winds and spectacular explosions they act as cosmic engines, heating and enriching their surroundings, where the next generation of stars are forming. 
The latest stellar evolutionary models show that rotation can have drastic effects, which has been suggested as a evolutionary path for the progenitors of long gamma-ray bursts. I will discuss the recent efforts of theorists and observers to understand the effects of rotation including some highlights of the ongoing "VLT-FLAMES Tarantula Survey of Massive Stars". A further challenge arises from the preference of massive stars to come in close pairs. Interaction with a companion leads to spectacular phenomena such as runaways, X-ray binaries and stellar mergers. I will present new results on the true close binary fraction for massive stars, which imply that only a minority evolve undisturbed towards their death.

Thursday January 19, 2012
Dr. Stan Owocki
Bartol Research Institute, University of Delaware, USA


Massive stars lose mass through powerful, radiatively driven stellar winds. Building on the original "CAK" model for steady, spherical winds driven by line-scattering, this talk will review recent research on the multi-faceted nature of such wind mass loss under varied conditions, for example due to rapid rotation, magnetic channeling, binary interaction, or a luminosity near the Eddington limit. An overall theme is that wind mass loss can in this way lead to a wide variety of astrophysical phenomena, including bipolar nebulae, massive star magnetospheres, colliding winds or compact companion accretion, and luminous blue variable eruption. The discussion here will summarize these with an emphasis on their varied observational signatures.

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