Stellar mass loss
Stellar mass loss is a phenomenon observed in some massive stars. It occurs when a triggering event causes the ejection of a large portion of the star's mass. Stellar mass loss can also occur when a star gradually loses material to a binary companion or into interstellar space.
A number of factors can contribute to the loss of mass in giant stars, including:
- Gravitational attraction of a binary companion
- Coronal mass ejection-type events
- Ascension to red giant or red supergiant status
Gravitational mass lossEdit
Often when a star is a member of a pair of close-orbiting binary stars, the tidal attraction of the gasses near the center of mass are sufficient to pull gas from one star onto its partner. This effect is especially prominent when the partner is a white dwarf, neutron star, or black hole.
Certain classes of stars, especially Wolf-Rayet stars are sufficiently massive and distended that their hold on their upper layers is rather weak. Often, events such as solar flares and coronal mass ejections will then be sufficiently powerful to blast some of the upper material into space.
Red giant mass lossEdit
Stars which have entered the red giant phase are notorious for rapid mass loss. As above, the gravitational hold on the upper layers is weakened, and they may be shed into space by violent events such as the beginning of a helium flash in the core. The final stage of a red giant's life will also result in prodigious mass loss as the star loses its outer layers to form a planetary nebula.
- Seeds, Michael A., Astronomy: The Solar System and Beyond, Brooks/Cole 2005