Results 51 to 60 of about 21,784 (251)
Asymptotic Giant Branch Stars [PDF]
, 2004 Preface Chapter 1: Introduction: H.J. Habing and H. Olofsson N.B.: This chapter is not yet completed! 1.1 Bits of history 1.2 The structure of AGB stars 1.3 Observational characteristics of AGB stars 1.4 Distinctive properties of AGB stars Chapter 2: Evolution, Nucleosynthesis and Pulsation: P. Wood and J. Lattanzio 2.1 Basic observational properties 2.
Harm J. Habing, Hans Olofsson
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The shock-heated atmosphere of an asymptotic giant branch star resolved by ALMA [PDF]
, 2017 Our current understanding of the chemistry and mass-loss processes in Sun-like stars at the end of their evolution depends critically on the description of convection, pulsations and shocks in the extended stellar atmosphere1.
W. Vlemmings +10 more
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Comparing Tip of the Red Giant Branch Distance Scales: An Independent Reduction of the Carnegie-Chicago Hubble Program and the Value of the Hubble Constant [PDF]
, 2021 The tip of the red giant branch has been used to measure distances to 500 nearby galaxies with the Hubble Space Telescope (HST) which are available in the Color–Magnitude Diagrams and Tip of the Red Giant Branch (CMDs/TRGB) catalog on the Extragalactic ...
G. Anand +4 more
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Evolution of Asymptotic Giant Branch Stars [PDF]
Annual Review of Astronomy and Astrophysics, 2005 ▪ Abstract The current status of modeling the evolution and nucleosynthesis of asymptotic giant branch (AGB) stars is reviewed. The principles of AGB evolution have been investigated in recent years leading to improved and refined models, for example with regard to hot-bottom burning or the third dredge-up.
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Defining the Termination of the Asymptotic Giant Branch [PDF]
The Astrophysical Journal, 2008 I suggest a theoretical quantitative definition for the termination of the asymptotic giant branch (AGB) phase and the beginning of the post-AGB phase. I suggest that the transition will be taken to occur when the ratio of the dynamical time scale to the the envelope thermal time scale, Q, reaches its maximum value. Time average values are used for the
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The puzzle of the CNO isotope ratios in asymptotic giant branch carbon stars [PDF]
, 2016 Context. The abundance ratios of the main isotopes of carbon, nitrogen and oxygen are modified by the CNO-cycle in the stellar interiors. When the different dredge-up events mix the burning material with the envelope, valuable information on the ...
C. Abia +3 more
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Frontiers in Astronomy and Space Sciences, 2021 Among presolar grains, oxide ones are made of oxygen, aluminum, and a small fraction of magnesium, produced by the 26Al decay. The largest part of presolar oxide grains belong to the so-called group 1 and 2, which have been suggested to form in Red Giant
S. Palmerini +11 more
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LOST AND FOUND: EVIDENCE OF SECOND-GENERATION STARS ALONG THE ASYMPTOTIC GIANT BRANCH OF THE GLOBULAR CLUSTER NGC 6752 [PDF]
, 2016 We derived chemical abundances for C, N, O, Na, Mg, and Al in 20 asymptotic giant branch (AGB) stars in the globular cluster (GC) NGC 6752. All these elements (but Mg) show intrinsic star-to-star variations and statistically significant correlations or ...
E. Lapenna +9 more
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Multiple populations along the asymptotic giant branch of the globular cluster M 4 [PDF]
, 2016 Nearly all Galactic globular clusters host stars that display characteristic abundance anti-correlations, like the O-rich/Na-poor pattern typical of field halo stars, together with O-poor/Na-rich additional components.
C. Lardo +5 more
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A Population of Binaries in the Asymptotic Giant Branch of 47 Tucanae? [PDF]
The Astrophysical Journal, 2006 We have used a set of archived Hubble Space Telescope/ACS images to probe the evolved populations of the globular cluster 47 Tucanae. We find an excess of Asymptotic Giant Branch (AGB) stars in the cluster core. We interpret this feature as the signature of an extra-population likely made by the progeny of massive stars originated by the evolution of ...
Michele Bellazzini +4 more
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