Back Asimptotiese reusetak Afrikaans عملاق مقارب Arabic Nəhənglərin Asimptotik qolu Azerbaijani Асимптотичен клон на гигантите Bulgarian Zvijezda asimptotskog divovskog ogranka BS Branca asimptòtica de les gegants Catalan Asymptotická větev obrů Czech Asymptotisk kæmpegren Danish AGB-Stern German Rama asintótica gigante Spanish
The asymptotic giant branch (AGB) is a region of the Hertzsprung–Russell diagram populated by evolved cool luminous stars. This is a period of stellar evolution undertaken by all low- to intermediate-mass stars (about 0.5 to 8 solar masses) late in their lives.
Observationally, an asymptotic-giant-branch star will appear as a bright red giant with a luminosity ranging up to thousands of times greater than the Sun. Its interior structure is characterized by a central and largely inert core of carbon and oxygen, a shell where helium is undergoing fusion to form carbon (known as helium burning), another shell where hydrogen is undergoing fusion forming helium (known as hydrogen burning), and a very large envelope of material of composition similar to main-sequence stars (except in the case of carbon stars).[1]
- ^ Lattanzio, J.; Forestini, M. (1999). "Nucleosynthesis in AGB Stars". In Le Bertre, T.; Lebre, A.; Waelkens, C. (eds.). Asymptotic Giant Branch Stars. IAU Symposium 191. p. 31. Bibcode:1999IAUS..191...31L. ISBN 978-1-886733-90-9.