Asymptotic giant branch

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Evolution of stars of different masses are represented in the Hertzsprung–Russell diagram. The asymptotic giant branch is marked AGB in the case of a star of 2 solar masses.

The asymptotic giant branch is the region of the Hertzsprung–Russell diagram populated by evolving low- to medium-mass stars. This is a period of stellar evolution undertaken by all low- to intermediate-mass stars (0.6–10 solar masses) late in their lives.

Observationally, an asymptotic-giant-branch (AGB) star will appear as a bright red giant with a luminosity thousands of times the Sun. Its interior structure is characterized by a central and 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.[1]

Stellar evolution[edit]

When a star exhausts the supply of hydrogen by nuclear fusion processes in its core, the core contracts and its temperature increases, causing the outer layers of the star to expand and cool. The star's luminosity increases greatly, and it becomes a red giant, following a track leading into the upper-right hand corner of the HR diagram.[2]

Eventually, once the temperature in the core has reached approximately 3×108 K, helium burning (fusion of helium nuclei) begins. The onset of helium burning in the core halts the star's cooling and increase in luminosity, and the star instead moves down and leftwards in the HR diagram. This is the horizontal branch (for population II stars) or red clump (for population I stars). After the completion of helium burning in the core, the star again moves to the right and upwards on the diagram. Its path is almost aligned with its previous red-giant track, hence the name asymptotic giant branch. Stars at this stage of stellar evolution are known as AGB stars.[3]

AGB stage[edit]

Formation of a planetary nebula at the end of the Asymptotic Giant Branch phase

The AGB phase is divided into two parts, the early AGB (E-AGB) and the thermally pulsing AGB (TP-AGB). During the E-AGB phase, the main source of energy is helium fusion in a shell around a core consisting mostly of carbon and oxygen. During this phase, the star swells up to giant proportions to become a red giant again. The star's radius may become as large as one astronomical unit (~215 R).[3]

After the helium shell runs out of fuel, the TP-AGB starts. Now the star derives its energy from fusion of hydrogen in a thin shell, which restricts the inner helium shell to a very thin layer and prevents it fusing stably. However, over periods of 10,000 to 100,000 years, helium from the hydrogen shell burning builds up and eventually the helium shell ignites explosively, a process known as a helium shell flash. The luminosity of the shell flash peaks at thousands of times the total luminosity of the star, but decreases exponentially over just a few years. The shell flash causes the star to expand and cool which shuts off the hydrogen shell burning and causes strong convection in the zone between the two shells.[3] When the helium shell burning nears the base of the hydrogen shell, the increased temperature reignites hydrogen fusion and the cycle begins again. The large but brief increase in luminosity from the helium shell flash produces an increase in the visible brightness of the star of a few tenths of a magnitude for several hundred years, a change unrelated to the brightness variations on periods of tens to hundreds of days that are common in this type of star.[4]

During the thermal pulses, which last only a few hundred years, material from the core region may be mixed into the outer layers, changing the surface composition, a process referred to as dredge-up. Because of this dredge-up, AGB stars may show S-process elements in their spectra and strong dredge-ups can lead to the formation of carbon stars. All dredge-ups following thermal pulses are referred to as third dredge-ups, after the first dredge-up, which occurs on the red-giant branch, and the second dredge up, which occurs during the E-AGB. In some cases there may not be a second dredge-up but dredge-ups following thermal pulses will still be called a third dredge-up. Thermal pulses increase rapidly in strength after the first few, so third dredge-ups are generally the deepest and most likely to circulate core material to the surface.[5][6]

AGB stars are typically long-period variables, and suffer mass loss in the form of a stellar wind. Thermal pulses produce periods of even higher mass loss and may result in detached shells of circumstellar material. A star may lose 50 to 70% of its mass during the AGB phase.[7]

Circumstellar envelopes of AGB stars[edit]

The extensive mass loss of AGB stars means that they are surrounded by an extended circumstellar envelope (CSE). Given a mean AGB lifetime of one Myr and an outer velocity of 10 km/s, its maximum radius can be estimated to be roughly 3×1014 km (30 light years). This is a maximum value since the wind material will start to mix with the interstellar medium at very large radii, and it also assumes that there is no velocity difference between the star and the interstellar gas. Dynamically, most of the interesting action is quite close to the star, where the wind is launched and the mass loss rate is determined. However, the outer layers of the CSE show chemically interesting processes, and due to size and lower optical depth, are easier to observe.[8]

The temperature of the CSE is determined by heating and cooling properties of the gas and dust, but drops with radial distance from the photosphere of the stars which are 2,0003,000 K. A chemical picture of an AGB CSE outwards is something like this:[9]

  1. Photosphere: Local thermodynamic equilibrium chemistry;
  2. Pulsating stellar envelope: Shock chemistry;
  3. Dust formation zone;
  4. Chemically quiet;
  5. Interstellar UV radiation and photodissociation of molecules – complex chemistry

Here, the dichotomy between oxygen-rich and carbon-rich stars will have an initial say as to whether the first condensates are oxides or carbides, since the least abundant of these two elements will likely remain in the gas phase as COx.

For more details on this topic, see List of interstellar and circumstellar molecules.

In the dust formation zone, refractory elements and compounds (Fe, Si, MgO, etc.) are removed from the gas phase and end up in dust grains. The newly formed dust will immediately assist in surface catalyzed reactions. The stellar winds from AGB stars are sites of cosmic dust formation, and are believed to be the main production sites of dust in the universe.[10]

The stellar winds of AGB stars (Mira variables and OH/IR stars) are also often the site of maser emission. The masering molecules are SiO, H2O, and OH.[11]

After these stars have lost nearly all of their envelopes, and only the core regions remain, they evolve further into short-lived preplanetary nebulae. The final fate of the AGB envelopes are represented by planetary nebulae (PNe).[12]

Late thermal pulse[edit]

As many as a quarter of all post-AGB stars undergo what is dubbed a born-again episode. The carbon–oxygen core is now surrounded by helium with an outer shell of hydrogen. If the helium is re-ignited a thermal pulse occurs and the star quickly returns to the AGB, becoming a helium-burning, hydrogen-deficient stellar object.[13] If the star still has a hydrogen-burning shell when this thermal pulse occurs, it is termed a late thermal pulse. Otherwise it is called a very late thermal pulse.[14]

The outer atmosphere of the born-again star develops a stellar wind and the star once more follows an evolutionary track across the Hertzsprung–Russell diagram. However, this phase is very brief, lasting only about 200 years before the star again heads toward the white dwarf stage. Observationally, this late thermal pulse phase appears almost identical to a Wolf–Rayet star in the midst of its own planetary nebula.[13]

Super-AGB stars[edit]

Stars close to the upper mass limit to still qualify as AGB stars show some interesting properties and have been dubbed super-AGB stars. They have masses above 7 M and up to 9 or 10 M (or more[15]). They represent a transition to the more massive supergiant stars that undergo full fusion of elements heavier than helium. During the triple-alpha process, some elements heavier than carbon are also produced: mostly oxygen, but also some magnesium, neon, and even heavier elements. Super-AGB stars develop partially degenerate carbon–oxygen cores that are large enough to ignite carbon in a flash analogous to the earlier helium flash. The second dredge-up is very strong in this mass range and that keeps the core size below the level required for burning of neon as occurs in higher-mass supergiants. The size of the thermal pulses and third dredge-ups are reduced compared to lower-mass stars, while the frequency of the thermal pulses increases dramatically. Some super-AGB stars may explode as an electron capture supernova, but most will end as an oxygen–neon white dwarf.[16] Since these stars are much more common than higher-mass supergiants, they could form a high proportion of observed supernovae. Detecting examples of these supernovae would provide valuable confirmation of models that are highly dependent on assumptions.

See also[edit]


  1. ^ Lattanzio, J.; Forestini, M. (1999). "Nucleosynthesis in AGB Stars". In Le Bertre, T.; Lebre, A.; Waelkens, C. Asymptotic Giant Branch Stars. IAU Symposium 191. p. 31. Bibcode:1999IAUS..191...31L. ISBN 978-1-886733-90-9. 
  2. ^ Iben, I. (1967). "Stellar Evolution.VI. Evolution from the Main Sequence to the Red-Giant Branch for Stars of Mass 1 M, 1.25 M, and 1.5  M". The Astrophysical Journal 147: 624. Bibcode:1967ApJ...147..624I. doi:10.1086/149040.  line feed character in |title= at position 180 (help)
  3. ^ a b c Vassiliadis, E.; Wood, P. R. (1993). "Evolution of low- and intermediate-mass stars to the end of the asymptotic giant branch with mass loss". The Astrophysical Journal 413 (2): 641. Bibcode:1993ApJ...413..641V. doi:10.1086/173033. 
  4. ^ Marigo, P.; et al. (2008). "Evolution of asymptotic giant branch stars. II. Optical to far-infrared isochrones with improved TP-AGB models". Astronomy and Astrophysics 482 (3): 883. arXiv:0711.4922. Bibcode:2008A&A...482..883M. doi:10.1051/0004-6361:20078467. 
  5. ^ Gallino, R.; et al. (1998). "Evolution and Nucleosynthesis in Low‐Mass Asymptotic Giant Branch Stars. II. Neutron Capture and thes‐Process". The Astrophysical Journal 497 (1): 388. Bibcode:1998ApJ...497..388G. doi:10.1086/305437. 
  6. ^ Mowlavi, N. (1999). "On the third dredge-up phenomenon in asymptotic giant branch stars". Astronomy and Astrophysics 344: 617. arXiv:astro-ph/9903473. Bibcode:1999A&A...344..617M. 
  7. ^ Wood, P. R.; Olivier, E. A.; Kawaler, S. D. (2004). "Long Secondary Periods in Pulsating Asymptotic Giant Branch Stars: An Investigation of Their Origin". The Astrophysical Journal 604 (2): 800. Bibcode:2004ApJ...604..800W. doi:10.1086/382123. 
  8. ^ Habing, H. J. (1996). "Circumstellar envelopes and Asymptotic Giant Branch stars". The Astronomy and Astrophysics Review 7 (2): 97. Bibcode:1996A&ARv...7...97H. doi:10.1007/PL00013287. 
  9. ^ Klochkova, V. G. (2014). "Circumstellar envelope manifestations in the optical spectra of evolved stars". Astrophysical Bulletin 69 (3): 279. arXiv:1408.0599. Bibcode:2014AstBu..69..279K. doi:10.1134/S1990341314030031. 
  10. ^ Woitke, P. (2006). "Too little radiation pressure on dust in the winds of oxygen-rich AGB stars". Astronomy and Astrophysics 460 (2): L9. arXiv:astro-ph/0609392. Bibcode:2006A&A...460L...9W. doi:10.1051/0004-6361:20066322. 
  11. ^ Deacon, R. M.; Chapman, J. M.; Green, A. J.; Sevenster, M. N. (2007). "H2O Maser Observations of Candidate Post‐AGB Stars and Discovery of Three High‐Velocity Water Sources". The Astrophysical Journal 658 (2): 1096. arXiv:astro-ph/0702086. Bibcode:2007ApJ...658.1096D. doi:10.1086/511383. 
  12. ^ Werner, K.; Herwig, F. (2006). "The Elemental Abundances in Bare Planetary Nebula Central Stars and the Shell Burning in AGB Stars". Publications of the Astronomical Society of the Pacific 118 (840): 183. arXiv:astro-ph/0512320. Bibcode:2006PASP..118..183W. doi:10.1086/500443. 
  13. ^ a b Aerts, C.; Christensen-Dalsgaard, J.; Kurtz, D. W. (2010). Asteroseismology. Springer. pp. 37–38. ISBN 978-1-4020-5178-4. 
  14. ^ Duerbeck, H. W. (2002). "The final helium flash object V4334 Sgr (Sakurai's Object) - an overview". In Sterken, C.; Kurtz, D. W. Observational aspects of pulsating B and A stars. ASP Conference Series. San Francisco: Astronomical Society of the Pacific. p. 237–248. Bibcode:2002ASPC..256..237D. ISBN 1-58381-096-X. 
  15. ^ Siess, L. (2006). "Evolution of massive AGB stars". Astronomy and Astrophysics 448 (2): 717. Bibcode:2006A&A...448..717S. doi:10.1051/0004-6361:20053043. 
  16. ^ Eldridge, J. J.; Tout, C. A. (2004). "Exploring the divisions and overlap between AGB and super-AGB stars and supernovae". Memorie della Società Astronomica Italiana 75: 694. arXiv:astro-ph/0409583. Bibcode:2004MmSAI..75..694E. 

Further reading[edit]