Relations between the Galactic Evolution and the Stellar Evolution

1984 ◽  
pp. 541-548
Author(s):  
Jean Audouze
Keyword(s):  
Stellar Evolution ◽  
Galactic Evolution

scholarly journals Relations between the galactic evolution and the stellar evolution

1984 ◽  
Vol 105 ◽  
pp. 541-548 ◽  
Author(s):  
Jean Audouze
Keyword(s):  
Chemical Evolution ◽  
Stellar Evolution ◽  
Galactic Evolution ◽  
Evolution Of Galaxies ◽  
The Impact

The question which has been raised in many chapters of this book is about the existence of constraints on stellar evolution coming from related topics like cosmology or in the case of the present chapter the chemical evolution of the galaxies. As it will be seen in this contribution it seems wiser to consider that chemical evolution of galaxies is indeed related to the problem of stellar evolution discussed here but is not going to provide as many constraints on it as one would expect. The purpose of this presentation is therefore to outline the principal relations between these two fields and to discuss the impact of some recent works on them.

scholarly journals Observational Evidence for Atmospheric Chemical Composition Peculiarities Relevant to Stellar Evolution

1977 ◽  
Vol 4 (2) ◽  
pp. 119-135
Author(s):  
B. E. J. Pagel
Keyword(s):  
Chemical Composition ◽  
Stellar Evolution ◽  
Supernova Remnant ◽  
Main Sequence ◽  
Observational Evidence ◽  
Galactic Evolution ◽  
Red Giants ◽  
Main Sequence Stars ◽  
Separation Processes ◽  
Cassiopeia A

Abundance peculiarities in successive stages of stellar evolution are reviewed. Main-sequence stars show anomalies in lithium and, on the upper main sequence, the Am, Ap and Bp effects, which may be largely due to separation processes, and helium and CNO anomalies to which nuclear evolution and mixing could have contributed. Red giants of both stellar Populations commonly show more or less extreme variations among the C, N, 0 isotopes, sometimes accompanied by s-process enhancement, due to mixing out in various evolutionary stages. Detailed anomalies expected from galactic evolution are also briefly considered. Novae show strong effects in C, N, 0 and synthesis of heavier elements is displayed by the supernova remnant Cassiopeia A.

scholarly journals The Macquarie–Strasbourg Connection

2010 ◽  
Vol 27 (2) ◽  
pp. 128-128
Author(s):  
Agnès Acker
Keyword(s):  
High Resolution ◽  
Stellar Evolution ◽  
Representative Sample ◽  
Galactic Plane ◽  
Planetary Nebulae ◽  
Galactic Evolution ◽  
Galactic Bulge ◽  
Late Stages ◽  
Remarkable Advance

Planetary nebulae (PN) are powerful tracers of both stellar and Galactic evolution. The capacity of PN to perform these studies is critically dependent on the size of the population, a major problem with a remarkable advance thanks to Quentin Parker and his team, who from 1997 to 2008 discovered an unprecedented sample of ∼1250 PN with the deep, high resolution AAO/UKST SuperCosmos Halpha Survey (SHS) of the Southern Galactic Plane (Parker et al. 2005), doubling the sample collected over the previous century, and leading to ∼2700 for the number of known PN today. A highly productive collaboration between Quentin and I has been established since 2001. Our complementary levels of expertise and facilities constitute the Macquarie/AAO/Strasbourg H-α Planetary Nebulae Project.The new MASH PN were added to the Centre de Données de Strasbourg as a new PN database continuously updated, and detailed in Parker et al. (2006) and Miszalski et al. (2008). In the framework of a cotutelle agreement between the Strasbourg and Macquarie universities, two PhD projects based on MASH PN have been conducted under the supervision of Quentin and myself, both projects focusing on the mysterious crowded region of the Galactic Bulge. Alan Peyaud proposed new constraints on late stages of stellar evolution and on the dynamics of the Galactic Bulge (defence 21 December 2005, Strasbourg). Brent Miszalski discovered ∼360 new PN (MASH-II) completing the largest and most representative sample of PN towards the Galactic bulge (defence 15 August 2009).

Carbon and oxygen isotopes in AGB stars. From the cores of AGB stars to presolar dust

2018 ◽  
Vol 14 (S343) ◽  
pp. 447-448
Author(s):  
Thomas Lebzelter ◽  
Kenneth Hinkle ◽  
Oscar Straniero
Keyword(s):  
Solar System ◽  
Stellar Evolution ◽  
Galactic Evolution ◽  
Isotopic Ratios ◽  
Red Giants ◽  
Agb Stars ◽  
Carbon And Oxygen Isotopes ◽  
Different Types ◽  
Red Giant ◽  
Final Evolution

AbstractIsotopic ratios are a powerful tool for gaining insights into stellar evolution and nucleosynthesis. The isotopic ratios of the key elements carbon and oxygen are perfectly suited to investigate the pristine composition of red giants, the conditions in their interiors, and the mixing in their extended atmospheres. Of course the dust ejected from red giants in their final evolution also contains isotopically tagged material. This red giant dust is present in the solar system as presolar dust grains. We have measured isotopic ratios of carbon and oxygen in spectra from a large sample of AGB stars including both Miras and semiregular variables. We show how the derived ratios compare with expectations from stellar models and with measurements in presolar grains. Comparison of isotopes that are affected by different types of nucleosynthesis provides insights into galactic evolution.

scholarly journals Carbon Stars and Nucleosynthesis in Galaxies

2000 ◽  
Vol 177 ◽  
pp. 481-496 ◽  
Author(s):  
Bengt Gustafsson ◽  
Nils Ryde
Keyword(s):  
Stellar Evolution ◽  
Chemical Elements ◽  
Galactic Evolution ◽  
Agb Stars ◽  
Carbon Stars ◽  
Abundance Trends ◽  
Solar Type

The role of carbon stars in the build-up of chemical elements in galaxies is discussed on the basis of stellar evolution calculations and estimated stellar yields, abundance analyses of AGB stars, galactic-evolution models and abundance trends among solar-type disk stars. We conclude that the AGB stars in general, and carbon stars in particular, probably are main contributors of s-elements, that their contributions of flourine and carbon are quite significant, and that possibly their contributions of lithium, 13C and 22Ne are of some importance. Also contributions of N, Na and Al are discussed. The major uncertainties that characterize almost any statement concerning these issues are underlined.

Stellar Evolution

1962 ◽  
Vol 11 (02) ◽  
pp. 137-143
Author(s):  
M. Schwarzschild
Keyword(s):  
Solar System ◽  
Stellar Evolution ◽  
Space Craft ◽  
New Techniques ◽  
Substantial Body ◽  
Individual Stars ◽  
The Past ◽  
Evolution Of Galaxies ◽  
History Of ◽  
Fast Flow

It is perhaps one of the most important characteristics of the past decade in astronomy that the evolution of some major classes of astronomical objects has become accessible to detailed research. The theory of the evolution of individual stars has developed into a substantial body of quantitative investigations. The evolution of galaxies, particularly of our own, has clearly become a subject for serious research. Even the history of the solar system, this close-by intriguing puzzle, may soon make the transition from being a subject of speculation to being a subject of detailed study in view of the fast flow of new data obtained with new techniques, including space-craft.

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