Asymptotic Giant Branch Evolution and Beyond

Iben, Icko; Renzini, A.

doi:10.1146/annurev.aa.21.090183.001415

Cited by 1,286 publications

(1,046 citation statements)

References 0 publications

Supporting

Mentioning

1,013

Contrasting

Unclassified

Order By: Relevance

“…Iben & Renzini 1983). We investigate this phase by computing a 3 M evolutionary model with Z = 0.02, starting at the zero age main sequence (Langer et al 1999).…”

Section: Helium Shell Burning On the Agbmentioning

confidence: 99%

On the stability of thermonuclear shell sources in stars

Yoon

Langer

Sluys

2004

A&A

View full text Add to dashboard Cite

Abstract. We present a quantitative criterion for the thermal stability of thermonuclear shell sources. We find that the thermal stability of shell sources depends on exactly three factors: they are more stable when they are geometrically thicker, less degenerate and hotter. This confirms and unifies previously obtained results in terms of the geometry, temperature and density of the shell source, by a simplified but quantitative approach to the physics of shell nuclear burning. We present instability diagrams in the temperature-density plane for hydrogen and helium shell burning, which allow a simple evaluation of the stability conditions of such shell sources in stellar models. The performance of our stability criterion is demonstrated in various numerical models: in a 3 M AGB star, in helium accreting CO white dwarfs, in a helium white dwarf which is covered by a thin hydrogen envelope, and in a 1.0 M giant.

show abstract

“…Iben & Renzini 1983). We investigate this phase by computing a 3 M evolutionary model with Z = 0.02, starting at the zero age main sequence (Langer et al 1999).…”

Section: Helium Shell Burning On the Agbmentioning

confidence: 99%

On the stability of thermonuclear shell sources in stars

Yoon

Langer

Sluys

2004

A&A

View full text Add to dashboard Cite

show abstract

“…Send offprint requests to: M.-R. L. Cioni, e-mail: mcioni@eso.org Iben & Renzini (1983) explain the correlation between metallicity and the C/M ratio by three factors: (1) for lower metallicity the O-rich stars will turn into C-type AGB stars more easily and stay so for a longer time on the AGB because less carbon atoms need to be dredgedup for the transformation; (2) at lower metallicity the evolutionary tracks for AGB stars move to higher temperatures and the number of M5+ 1 stars drops considerably; the abundance of TiO molecules is lower and the atmosphere is more transparent; (3) in very-low metallicity environments a posthorizontal-branch star may become a white dwarf without becoming first an AGB star ("AGB-manqué stars").…”

Section: Introductionmentioning

confidence: 99%

AGB stars in the Magellanic Clouds

Cioni

Habing

2003

A&A

112

136

View full text Add to dashboard Cite

Abstract.Regions of different metallicity have been identified in the Magellanic Clouds by using the ratio between Asymptotic Giant Branch stars of spectral type C and M. In the Large Magellanic Cloud the ratio appears to decrease radially while in the Small Magellanic Cloud (SMC) there is no clear trend, reflecting either the large extension of the SMC along the line of sight or a more complex star formation history. The distribution of the C/M ratio is clumpy and corresponds to a spread in [Fe/H] of 0.75 dex in both Clouds. There is an indication of increasing C/M ratio, thus decreasing metallicity, towards the Bridge region connecting the two Clouds.

show abstract

“…In 1983, surprisingly in the same year, theory (Iben & Renzini 1983) and observations (Weidemann & Koester 1983) concluded, that all stars with a main sequence mass 8M will become Planetary Nebulae (PNe) ending as a white dwarf. The progenitor star will eject all mass but the stellar degenerate core into the interstellar medium (ISM).…”

Section: Introductionmentioning

confidence: 98%

The frontier of ground-based observations

Käufl¹

2011

Proc. IAU

View full text Add to dashboard Cite

Abstract. The ESO VLT on Paranal is in transition from first generation instrumentation to second generation, or at least to substantially upgraded instrumentation. The new instrumentation shall establish multipicity gain, high image definition or integral field imaging spectroscopy. Starting from observational highlights, status and trends for groundbased instrumentation will be revisited with emphasis on the field of PNe in all evolutionary phases. This review will concentrate on spectroscopy and scientific cases where groundbased observations offer a particular advantage. To the extent possible, a projection will be given as to the potential of the extremely large telescopes on the horizon, which will work best in the (near-)infrared.

show abstract

Asymptotic Giant Branch Evolution and Beyond

Cited by 1,286 publications

References 0 publications

On the stability of thermonuclear shell sources in stars

On the stability of thermonuclear shell sources in stars

AGB stars in the Magellanic Clouds

The frontier of ground-based observations

Contact Info

Product

Resources

About