PDF
PDF

Keywords

stars: magnetic fields
stars: mass loss
stars: oscillations (including pulsations)
stars: rotation

How to Cite

Hydrodynamic Wind Theory. (2010). Revista Mexicana De Astrofísica Y Astronomía Serie De Conferencias, 38(1), 44-47. https://astronomia.unam.mx/journals/rmxac/article/view/2010rmxac..38...44u
hola

Abstract

All main sequence stars lose mass via stellar winds. The winds of cool stars like the sun are driven by gas pressure gradient. However, the winds of hot massive stars which tend to be luminous are driven by the star radiation pressure. In this talk, I describe the nature of such radiative driving and show that the continuum and line opacities in the wind determine how large the stellar atmosphere may appear in an interferometer. Currently, interferometers can detect only relatively large scale structures. I will describe how these structures are induced by rotation, pulsations, magnetic fields or wind-wind interactions.