Mass loss from stars

This article discusses the different mass-loss processes of stars and how mass-loss rates determine the fate of stars in advanced stages of stellar evolution. Main sequence stars have their atmospheric structure dominated by radiation pressure. The pressure exerted by energetic photons is sufficient to drive gases off into space. This process can impact enormous turbulence to the local interstellar medium. Evolutionary effects keep these stars from fully evaporating, but the very course of their evolution is determined by this mass shedding process. Lower main sequence stars, like the sun, have a turbulent atmosphere enveloped in hot, thin coronal gas, blowing off a light stellar breeze. As the main sequence star evolves to a giant, its corona dissipates and the breeze turns into a strong stellar wind. Intermitten sputters combined with pulsational instabilities can lead to partial ejection of the atmosphere and envelope of a red giant, i.e. a planetary nebula results. The mass-loss from stars through planetary nebule combined with other mass-loss processes such as stellar winds returns a substantial amount of material to the interstellar environment. Mass-loss in binary systems is also discussed