Chemical Evolution in the Interstellar Medium: Feedstock of Solar Systems

2008 ◽  
pp. 80-110 ◽  
Author(s):  
Louis J. Allamandola
Keyword(s):  
Interstellar Medium ◽  
Chemical Evolution ◽  
Solar Systems

Impact of the Small-Scale Spatial Distribution of Dust Particles on the Chemical Evolution of the Diffuse Interstellar Medium

2020 ◽  
Vol 64 (8) ◽  
pp. 693-710
Author(s):  
V. A. Sokolova ◽  
A. I. Vasyunin ◽  
A. B. Ostrovskii ◽  
S. Yu. Parfenov
Keyword(s):  
Spatial Distribution ◽  
Interstellar Medium ◽  
Chemical Evolution ◽  
Dust Particles ◽  
Small Scale

scholarly journals Chemical Inhomogeneities in Galaxies

1977 ◽  
Vol 45 ◽  
pp. 67-71 ◽  
Author(s):  
M. G. Edmunds
Keyword(s):  
Interstellar Medium ◽  
Chemical Evolution ◽  
Galactic Disk ◽  
Observational Evidence ◽  
Galactic Evolution ◽  
Length Scale ◽  
Galactic Chemical Evolution ◽  
Large Length ◽  
Large Length Scale

The local chemical inhomogneity of the interstellar medium at a given time is an important factor in models of galactic chemical evolution. It can affect both the G-dwarf metallicity problem (Tinsley 1975, Talbot and Arnett 1973) and the correlation of the abundances of different elements (Tinsley 1976). Observational evidence of abundance gradients in our own Galaxy, and someothergalaxies (summarised by Peimbert 1975, van den Bergh 1975), implies that in homogeneities over a large length scale must be created and survive during galactic evolution. Brief consideration of the mixing of the Galactic disk (e.g. Edmunds 1975, 1976) suggests

scholarly journals Chemical evolution of the galactic interstellar medium: abundance gradients

1979 ◽  
Vol 84 ◽  
pp. 307-316 ◽  
Author(s):  
Manuel Peimbert
Keyword(s):  
Interstellar Medium ◽  
Chemical Evolution ◽  
Planetary Nebulae ◽  
Observational Evidence ◽  
H Ii Regions

Recent abundance determinations of galactic H II regions and planetary nebulae are reviewed. The presence of O/H and N/H abundance gradients is well established; there is observational evidence indicating the presence of N/S, He/H and C/H abundance gradients. Some implications of these results are discussed.

scholarly journals Abundance ratios in stars vs. hot gas in elliptical galaxies

2009 ◽  
Vol 5 (H15) ◽  
pp. 281-281
Author(s):  
Antonio Pipino
Keyword(s):  
Interstellar Medium ◽  
Chemical Evolution ◽  
Elliptical Galaxies ◽  
Evolution Model ◽  
X Ray ◽  
Galactic Wind ◽  
Hot Gas ◽  
Self Consistent ◽  
Chemical Evolution Model ◽  
Gas Properties

AbstractI present predictions from a chemical evolution model for a self-consistent study of optical (i.e., stellar) and X-ray (i.e., gas) properties of present-day elliptical galaxies. Detailed cooling and heating processes in the interstellar medium are taken into account and allow a reliable modelling of the SN-driven galactic wind. The model simultaneously reproduces the mass-metallicity, colour-magnitude, LX - LB and LX - T relations, and the observed trend of [Mg/Fe] with σ. The "iron discrepancy" can be solved by taking into account the dust presence.

scholarly journals Mass Loss from Stars and the Chemical Evolution of the Interstellar Medium

1977 ◽  
Vol 42 ◽  
pp. 641-649
Author(s):  
P. Biermann
Keyword(s):  
Interstellar Medium ◽  
Mass Loss ◽  
Chemical Evolution ◽  
Heavy Elements

AbstractMass loss from stars returns processed as well as unprocessed material to the Interstellar medium, and thus enriches it in helium and heavy elements. In this very brief review we outline the theory of the chemical evolution of the interstellar medium.

scholarly journals On the Formation of the First Quasars

2017 ◽  
Vol 34 ◽  
Author(s):  
Rosa Valiante ◽  
Bhaskar Agarwal ◽  
Melanie Habouzit ◽  
Edwige Pezzulli
Keyword(s):  
Black Holes ◽  
Interstellar Medium ◽  
Chemical Evolution ◽  
Rapid Growth ◽  
State Of The Art ◽  
Theoretical Models ◽  
Host Galaxy ◽  
Subsequent Evolution ◽  
Review State ◽  
Fast Chemical

AbstractObservations of the most luminous quasars at redshift z > 6 reveal the existence of numerous supermasssive black holes (>199 M⊙) already in place about 12 billion years ago. In addition, the interstellar medium of the galaxies hosting these black holes are observed to be chemically mature systems, with metallicities (Z > Z⊙) and dust masses (>108 M⊙) similar to that of more evolved, local galaxies. The connection between the rapid growth of the first supermassive black holes and the fast chemical evolution of the host galaxy is one of the most puzzling issues for theoretical models. Here, we review state-of-the-art theoretical models that focus on this problem with particular emphasis on the conditions that lead to the formation of quasar seeds and their subsequent evolution at z ⩾ 6.

Final Remarks: Connections between Chemical and Dynamical Evolution

1977 ◽  
Vol 45 ◽  
pp. 309-319
Author(s):  
Beatrice M. Tinsley
Keyword(s):  
Interstellar Medium ◽  
Chemical Evolution ◽  
Dynamical Evolution ◽  
Theoretical Background ◽  
Dynamical Processes ◽  
Chemical Enrichment ◽  
The Galaxy ◽  
History Of

Dynamical processes strongly affect the chemical enrichment of gas in galaxies, so abundances in stars and the Interstellar medium can be used as probes of the dynamical history of the Galaxy. By way of tying together some diverse points, rather than summarizing the conference, I shall discuss some examples of connections between chemical and dynamical evolution. The first section of this paper mentions some of the well-known ways in which dynamical processes can affect chemical evolution, in order to outline a theoretical background to the use of abundances as clues to dynamics.

scholarly journals Theoretical models of the Planetary Nebula populations in galaxies

1997 ◽  
Vol 180 ◽  
pp. 474-474 ◽  
Author(s):  
M. G. Richer ◽  
M. L. McCall ◽  
N. Arimoto
Keyword(s):  
Star Formation ◽  
Interstellar Medium ◽  
Chemical Evolution ◽  
Planetary Nebula ◽  
Planetary Nebulae ◽  
Theoretical Models ◽  
Theoretical Modelling ◽  
Oxygen Abundance

We consider the possibility of using bright planetary nebulae to study the chemical evolution of their parent galaxies. In particular, we would like to use planetary nebulae as abundance probes in galaxies where star formation ended long ago, such as ellipticals or the bulges of spirals, and in which no other direct probes exist. However, if we are to use planetary nebulae to study the chemical evolution of their parent galaxies, we must relate the oxygen abundance in bright planetary nebulae to the oxygen abundance in the interstellar medium when star formation stopped. Obviously, only theoretical modelling can provide this information once star formation has stopped.

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