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On Low Mass AGB Stars

Published online by Cambridge University Press:  19 July 2016

I.-Juliana Sackmann  and
Arnold I. Boothroyd
I.-Juliana Sackmann
Affiliation:
W. K. Kellogg Radiation Laboratory 106-38 California Institute of Technology Pasadena, CA 91125 U. S. A.
Arnold I. Boothroyd
Affiliation:
Canadian Institute for Theoretical Astrophysics University of Toronto Toronto, Ontario M5S 1A1 Canada

Abstract

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Recent results on low mass AGB stars are presented. Observed amounts of AGB mass loss imply that thermal pulses will only be encountered for stars of initial mass less than about 4M⊙ for Pop I and 3 M⊙ for Pop II. Mc – L, Me – τif, and Mc – Tb relations are summarized. Carbon dredge-up has been found in low mass stars of both Pop I and Pop II; the mixing length parameter α is crucial to dredge-up, and its value must be normalized according to each author's opacities and mixing length treatment (e.g., via the Sun's Te and L). The “carbon star mystery” is nearing a solution, but a new “s-process mystery” has appeared: only in a narrow range of mass and metallicity have theoretical models been found that encounter the semiconvective 13C s-process mechanism.

Type
The AGB
Information
Symposium - International Astronomical Union , Volume 145: Evolution of Stars: The Photospheric Abundance Connection , 1991 , pp. 275 - 285
Copyright
Copyright © Kluwer 1991 

References

Aaronson, M. and Mould, J. (1985) “The Extended Giant Branches of Intermediate Age Globular Clusters in the Magellanic Clouds. IV.”, Astrophys. J. 288, 551–557.CrossRefGoogle Scholar
Alexander, D. R. (1975) ‘Low-Temperature Rosseland Opacity Tables’, Astrophys. J. Suppl. 29, 363–374.Google Scholar
Alexander, D. R. (1981), private communication to D. VandenBerg.Google Scholar
Arnould, M. (1990), ‘s-process Nucleosynthesis in AGB Stars’, IAU Symposium 145. CrossRefGoogle Scholar
Becker, S. A. and Iben, I. Jr. (1979) “The Asymptotic Giant Branch Evolution of Intermediate-Mass Stars as a Function of Mass and Composition. I. Through the Second Dredge-Up Phase”, Astrophys. J. 232, 831–853.Google Scholar
Bertelli, G., Bressan, A., Chiosi, C., and Angerer, K. (1986) ‘Evolutionary Models for Low and Intermediate Mass Stars with Convective Overshooting’, Astron. Astrophys. Suppl. 66, 191–234.Google Scholar
Boothroyd, A. I., and Sackmann, I.-J. (1988a) ‘Low Mass Stars. I. Flash-Driven Luminosity and Radius Variations’, Astrophys. J. 328, 632–640.CrossRefGoogle Scholar
Boothroyd, A. I., and Sackmann, I.-J. (19886) ‘Low Mass Stars. II. The Core Mass-Luminosity Relation’, Astrophys. J. 328, 641–652.CrossRefGoogle Scholar
Boothroyd, A. I., and Sackmann, I.-J. (1988c) ‘Low Mass Stars. III. Low-Mass Stars with Steady Mass Loss: Up to the Asymptotic Giant Branch and Through the Final Thermal Pulses’, Astrophys. J. 328, 653–670.CrossRefGoogle Scholar
Boothroyd, A. I., and Sackmann, I.-J. (1988d) ‘The Production of Low Mass Stars. IV. Carbon Stars’, Astrophys. J. 328, 671–679.CrossRefGoogle Scholar
Caughlan, G. R. and Fowler, W. A. (1988) ‘Thermonuclear Reaction Rates V’, Atomic Data Nucl. Data Tables 40, 283–334.Google Scholar
Chiosi, C. (1986) ‘Advancements in the Stellar Evolution Theory: The Role of Convective Overshooting All Across the H-R Diagram’, in Chiosi, C. and Renzini, A. (eds.), Spectral Evolution of Galaxies , Reidel, Dordrecht, pp. 171–181.CrossRefGoogle Scholar
Chiosi, C., Bertelli, G., Bressan, A., and Nasi, E. (1986) ‘Magellanic Cloud Clusters: the Problems of Age Determination, Metallicity - Age Relationship and AGB Star Luminosity Function’, Astron. Astrophys. 165, 84–94.Google Scholar
Cox, A. N., and Stewart, J. N. (1970) ‘Rosseland Opacity Tables for Population I Compositions’, Astrophys. J. Suppl. 19, 243–259.CrossRefGoogle Scholar
Dorman, B., Nelson, L. A., and Chau, W. Y. (1989) ‘Theoretical Models of Low-Mass Stars and Brown Dwarfs. I. The Lower Main Sequence’, Astrophys. J. 342, 1003–1018.Google Scholar
Guenther, D. B., Jaffe, A., and Demarque, P. (1989) ‘The Standard Solar Model: Composition, Opacities, and Seismology’, Astrophys. J. 345, 1022–1033.Google Scholar
Havazelet, D. and Barkat, Z. (1979) ‘On the Core Mass-Luminosity Relations for Shell Helium Burning Stages of Stellar Evolution’, Astrophys. J. 233, 589–595.Google Scholar
Hollowell, D. (1987) ‘Mixing at the Carbon-Hydrogen Discontinuity During the Dredge-Up Phase in Low-Mass AGB Stars’, in Kwok, S. and Pottasch, S. R. (eds.), Late Stages of Stellar Evolution , Reidel, Dordrecht, pp. 239–240.Google Scholar
Hollowell, D. and Iben, I. Jr. (1988) ‘Nucleosynthesis of Solar System Material in a Low-Mass, Low-Metallicity Asymptotic Giant Branch Star’, Astrophys. J. (Lett.) 333, L25–L28.CrossRefGoogle Scholar
Hollowell, D. and Iben, I. Jr. (1989) ‘Neutron Production and Neutron-Capture Nucleosynthesis in a Low-Mass, Low-Metallicity Asymptotic Giant Branch Star’, Astrophys. J. 340, 966–984.Google Scholar
Iben, I. Jr. (1976) ‘Further Adventures of a Thermally Pulsing Star’, Astrophys. J. 208, 165–176.Google Scholar
Iben, I. Jr. (1977) ‘Thermal Pulse and Interpulse Properties of Intermediate-Mass Stellar Models with Carbon-Oxygen Cores of Mass 0.96, 1.16, and 1.36 M ô’, Astrophys. J. 217, 788–798.Google Scholar
Iben, I. Jr. (1981) ‘The Carbon Star Mystery: Why Do the Low Mass Ones Become Such, and Where Have All the High Mass Ones Gone?’, Astrophys. J. 246, 278–291.Google Scholar
Iben, I. Jr. (1982) ‘Low Mass Asymptotic Giant Branch Evolution I.’, Astrophys. J. 260, 821–837.Google Scholar
Iben, I. Jr. (1983) ‘Carbon Star Formation and Neutron-Rich Isotope Formation in Low-Mass Asymptotic Giant Branch Stars’, Astrophys. J. (Lett.) 275, L65–L69.Google Scholar
Iben, I. Jr. and Renzini, A. (1982a) ‘The Role of Semiconvection in Bringing Carbon to the Surface of Asymptotic Giant Branch Stars’, Astrophys. J. (Lett.) 259, L79–L83.Google Scholar
Iben, I. Jr. and Renzini, A. ((1982b) ‘On the Formation of Carbon Star Characteristics and the Production of Neutron-Rich Isotopes in Asymptotic Giant Branch Stars of Small Core Mass’, Astrophys. J. (Lett) 263, L23–L27.Google Scholar
Iben, I. Jr. and Renzini, A. ((1983) ‘Asymptotic Giant Branch Evolution and Beyond’, Ann. Rev. Astron. Astrophys. 21, 271–342.Google Scholar
Iben, I. Jr. and Truran, J. W. (1978) ‘On the Surface Composition of Thermally Pulsing Stars of High Luminosity and On the Contribution of Such Stars to the Element Enrichment of the Interstellar Medium’, Astrophys. J. 220, 980–995.Google Scholar
Keady, J. (1985), private communication.Google Scholar
Lattanzio, J. C. (1986) ‘The Asymptotic Giant Branch Evolution of 1.0 − 3.0 M ⊚ Stars as a Function of Mass and Composition’, Astrophys. J. 311, 708–730.Google Scholar
Lattanzio, J. C. (1987) ‘The Formation of a 1.5 M ô Carbon Star With M bol = −4.4’, Astrophys. J. (Lett.) 313, L15–L18.Google Scholar
Lattanzio, J. C. (1990), in Wallerstein, G. (ed.), Cool Stars, Stellar Systems, and the Sun , Astronomical Society of the Pacific (BookCrafters), San Francisco, pp. 396–400.Google Scholar
Malaney, R. A., and Boothroyd, A. I. (1987) ‘On the Origin of the Solar System s-Process Abundances’, Astrophys. J. 320, 866–870.Google Scholar
Paczynaki, B. (1970) ‘Evolution of Single Stars. I. Stellar Evolution from Main Sequence to White Dwarf or Carbon Ignition’, Acta Astr. 20, 47–58.Google Scholar
Paczynaki, B. (1975) ‘Core Mass-Interflash Period Relation for Double Shell Source Stars’, Astrophys. J. 202, 558–560.Google Scholar
Renzini, A. (1981) ‘Evolutionary Effects of Mass Loss in Low-Mass Stars’, in Chiosi, C. and Stalio, R. (eds.), Effects of Mass Loss on Stellar Evolution , Reidel, Dordrecht, pp. 319–338.CrossRefGoogle Scholar
Renzini, A. (1987) ‘Some Embarrassments in Current Treatments of Convective Overshooting’, Astron. Astrophys. 188, 49–54.Google Scholar
Sackmann, I.-J. (1976) ‘Convective Penetrations and Observable Consequences of Helium Shell Flashes in 3 and 6 M ô Red Supergiants’, preprint OAP-463.Google Scholar
Sackmann, I.-J. (1978) ‘A Shortlived, Deep Convective Envelope for Highly Evolved, Blue Stars?’, in Terzian, Y. (ed.), IAU Symposium 76: Planetary Nebulae, Observations and Theory , Reidel, Dordrecht, pp. 207–208.Google Scholar
Sackmann, I.-J. (1980) ‘A New Flash Mixing’, Astrophys. J. (Lett.) 241, L37–L40.Google Scholar
Sackmann, I.-J. and Boothroyd, A. I. (1990) ‘Mixing Length and Opacity Effects: Deep Convective Envelopes on the Asymptotic Giant Branch’, Astrophys. J. , in press.Google Scholar
Sackmann, I.-J., Boothroyd, A. I., and Fowler, W. A. (1990) ‘Our Sun. I. The Standard Model: Successes and Failures’, Astrophys. J. 360, 727–736.Google Scholar
Uus, U. (1970), Nauch. Inform. Acad. Nauk. 17, 3.Google Scholar
VandenBerg, D. A. (1983) ‘Star Clusters and Stellar Evolution. I. Improved Synthetic Color-Magnitude Diagrams for the Oldest Clusters’, Astrophys. J. Suppl. 51, 29–66.Google Scholar
Weidemann, V. (1984) ‘The Shape of the Initial-Final Mass Relation for Low and Intermediate Mass Stars’, Astron. Astrophys. (Lett.) 134, L1-L3.Google Scholar
Weidemann, V. and Koester, D. (1983) ‘The Upper Mass Limit for White Dwarf Progenitors and the Initial-Final Mass Relation for Low and Intermediate Mass Stars’, Astron. Astrophys. 121, 77–84.Google Scholar
Wood, P. R. (1981) ‘The Conditions for Dredge-Up of Carbon During the Helium Shell Flash and the Production of Carbon Stars’, in Iben, I. Jr. and Renzini, A. (eds.), Physical Processes in Red Giants , Reidel, Dordrecht, pp. 135–139.Google Scholar
Wood, P. R. and Zarro, D. M. (1981) ‘Helium-Shell Flashing in Low-Mass Stars and Period Changes in Mira Variables’, Astrophys. J. 247, 247–256.CrossRefGoogle Scholar