HAO Colloquium - Stan Owocki, Bartol Research Institute, University of Delaware

Radiation hydrodynamics in complex media: the Sun vs. massive-star winds

Realistic treatments of radiation transport in astrophysical media need to account efficiently for their often complex spatial structure. Beginning with a brief summary of my own early work on 2D transport in the solar atmosphere, this talk will focus mainly on methods developed for radiation hydrodynamical modeling of the highly unstable, and spatially complex mass outflows from massive stars. While radiation plays a key role in the energy transport in the sun, in luminous massive stars its momentum is central to driving mass loss. After summarizing simulations of  the unstable line-driving of quasi-steady stellar winds, I will discuss radiation hydrodynamical modeling of super-Eddington mass loss that occurs during giant eruptions of Luminous Blue Variable (LBV) stars, with emphasis on how the `porosity’ of a complex medium can reduce the effective opacity and so help regulate the initiation of mass outflows.

 

Building:

Room Number: 
2126

Type of event:

Will this event be webcast to the public by NCAR|UCAR?: 
Calendar Timing: 
Wednesday, March 28, 2018 - 2:00pm to 3:00pm