scholarly journals The stellar spectral features of nearby galaxies in the near infrared: tracers of thermally pulsing asymptotic giant branch stars?

2015 ◽  
Vol 450 (3) ◽  
pp. 3069-3079 ◽  
Author(s):  
Rogério Riffel ◽  
Rachel E. Mason ◽  
Lucimara P. Martins ◽  
Alberto Rodríguez-Ardila ◽  
Luis C. Ho ◽  
...  
Keyword(s):  
Near Infrared ◽  
Asymptotic Giant Branch ◽  
Spectral Features ◽  
Asymptotic Giant Branch Stars ◽  
Nearby Galaxies ◽  
Giant Branch Stars

scholarly journals Near-infrared photometric properties of asymptotic giant branch stars in the dwarf irregular galaxy IC 1613

2015 ◽  
Vol 578 ◽  
pp. A51 ◽  
Author(s):  
Sang-Hyun Chun ◽  
MiYoung Jung ◽  
Minhee Kang ◽  
Jae-Woo Kim ◽  
Young-Jong Sohn
Keyword(s):  
Near Infrared ◽  
Asymptotic Giant Branch ◽  
Asymptotic Giant Branch Stars ◽  
Irregular Galaxy ◽  
Giant Branch Stars

scholarly journals Extremely Metal-Poor Asymptotic Giant Branch Stars

Universe ◽  
2022 ◽  
Vol 8 (1) ◽  
pp. 44
Author(s):  
Mario Cirillo ◽  
Luciano Piersanti ◽  
Oscar Straniero
Keyword(s):  
Physical Structure ◽  
Asymptotic Giant Branch ◽  
Chemical Pollution ◽  
Asymptotic Giant Branch Stars ◽  
Chemical Abundances ◽  
First Stars ◽  
Convective Mixing ◽  
Nearby Galaxies ◽  
Complete Set ◽  
Giant Branch Stars

Little is known about the first stars, but hints on this stellar population can be derived from the peculiar chemical composition of the most metal-poor objects in the Milky Way and in resolved stellar populations of nearby galaxies. In this paper, we review the evolution and nucleosynthesis of metal-poor and extremely metal-poor (EMP) stars with low and intermediate masses. In particular, new models of 6 M⊙ with three different levels of metallicity, namely Z=10−4, 10−6 and 10−10, are presented. In addition, we illustrate the results obtained for a 2 M⊙, Z=10−5 model. All these models have been computed by means of the latest version of the FuNS code. We adopted a fully coupled scheme of solutions for the complete set of differential equations describing the evolution of the physical structure and the chemical abundances, as modified by nuclear processes and convective mixing. The scarcity of CNO in the material from which these stars formed significantly affects their evolution, their final fate and their contribution to the chemical pollution of the ISM in primordial galaxies. We show the potential of these models for the interpretation of the composition of EMP stars, with particular emphasis on CEMP stars.

scholarly journals Obscured asymptotic giant branch stars in the Magellanic Clouds -- II. Near-infrared and mid-infrared counterparts

1996 ◽  
Vol 279 (1) ◽  
pp. 32-62 ◽  
Author(s):  
A. A. Zijlstra ◽  
C. Loup ◽  
L. B. F. M. Waters ◽  
P. A. Whitelock ◽  
J. Th. van Loon ◽  
...  
Keyword(s):  
Near Infrared ◽  
Magellanic Clouds ◽  
Asymptotic Giant Branch ◽  
Asymptotic Giant Branch Stars ◽  
Mid Infrared ◽  
Giant Branch Stars

Observations of High Rotational CO Lines in Post–Asymptotic Giant Branch Stars and Planetary Nebulae

1997 ◽  
Vol 476 (1) ◽  
pp. 319-326 ◽  
Author(s):  
K. Justtanont ◽  
A. G. G. M. Tielens ◽  
C. J. Skinner ◽  
Michael R. Haas
Keyword(s):  
Planetary Nebulae ◽  
Asymptotic Giant Branch ◽  
Asymptotic Giant Branch Stars ◽  
Giant Branch Stars

scholarly journals Carbon stars as standard candles – II. The median J magnitude as a distance indicator

2020 ◽  
Vol 501 (1) ◽  
pp. 933-947
Author(s):  
Javiera Parada ◽  
Jeremy Heyl ◽  
Harvey Richer ◽  
Paul Ripoche ◽  
Laurie Rousseau-Nepton
Keyword(s):  
Luminosity Function ◽  
Asymptotic Giant Branch ◽  
Distance Modulus ◽  
Asymptotic Giant Branch Stars ◽  
Luminosity Functions ◽  
Best Fitting ◽  
Distance Indicator ◽  
Ngc 6822 ◽  
The Given ◽  
Giant Branch Stars

ABSTRACT We introduce a new distance determination method using carbon-rich asymptotic giant branch stars (CS) as standard candles and the Large and Small Magellanic Clouds (LMC and SMC) as the fundamental calibrators. We select the samples of CS from the ((J − Ks)0, J0) colour–magnitude diagrams, as, in this combination of filters, CS are bright and easy to identify. We fit the CS J-band luminosity functions using a Lorentzian distribution modified to allow the distribution to be asymmetric. We use the parameters of the best-fitting distribution to determine if the CS luminosity function of a given galaxy resembles that of the LMC or SMC. Based on this resemblance, we use either the LMC or SMC as the calibrator and estimate the distance to the given galaxy using the median J magnitude ($\overline{J}$) of the CS samples. We apply this new method to the two Local Group galaxies NGC 6822 and IC 1613. We find that NGC 6822 has an ‘LMC-like’ CS luminosity function, while IC 1613 is more ‘SMC-like’. Using the values for the median absolute J magnitude for the LMC and SMC found in Paper I we find a distance modulus of μ0 = 23.54 ± 0.03 (stat) for NGC 6822 and μ0 = 24.34 ± 0.05 (stat) for IC 1613.

Finite Temperature Behavior of Carbon Atom Doped Silicon Clusters: Depressed Thermal Stabilities, Co-existing isomers, Reversible Dynamical Pathways and Fragmentation Channels

2021 ◽  
Author(s):  
Krati Joshi ◽  
Ashakiran Maibam ◽  
Sailaja Krishnamurty
Keyword(s):  
Silicon Carbide ◽  
Carbon Atom ◽  
Finite Temperature ◽  
Asymptotic Giant Branch ◽  
Temperature Behavior ◽  
Asymptotic Giant Branch Stars ◽  
Silicon Clusters ◽  
Thermal Stabilities ◽  
Doped Silicon ◽  
Giant Branch Stars

Silicon carbide clusters are significant due to their predominant occurrence in meteoric star dust, particularly in carbon rich asymptotic giant branch stars. Of late, they have also been recognized as...

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