Superwind
Topic: Astronomy
From HandWiki - Reading time: 1 min
A superwind is an extremely dense wind emanating from asymptotic giant branch (AGB) stars towards the end of their lives.[1] While the exact origin of the superwind is unknown, it is believed that it causes the AGB star to appear as an OH/IR star. [2] At the latest stages of the star's life, an AGB star can lose around solar masses per year to the superwind. [2] This mass loss is so high that it causes nuclear fusion in AGB stars to be extinguished earlier than was predicted in early theories. After nuclear fusion has ceased, the star becomes a white dwarf, and the dense wind envelope becomes its planetary nebula. [3]
See also
References
- ↑ Marshall, Jonathan R; Van Loon, Jacco Th; Matsuura, Mikako; Wood, Peter R; Zijlstra, Albert A; Whitelock, Patricia A (2004). "Asymptotic giant branch superwind speed at low metallicity". Monthly Notices of the Royal Astronomical Society 355 (4): 1348. doi:10.1111/j.1365-2966.2004.08417.x. Bibcode: 2004MNRAS.355.1348M.
- ↑ 2.0 2.1 Carroll, Bradley W.; Ostlie, Dale A. (2017-09-07). An Introduction to Modern Astrophysics. Cambridge: Cambridge University Press. ISBN 978-1-108-42216-1.
- ↑ Prialnik, Dina (2009-10-29). An Introduction to the Theory of Stellar Structure and Evolution. Cambridge University Press. ISBN 978-0-521-86604-0.
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