Elemental Abundance Variations and Chemical Enrichment from Massive Stars in Starbursts. I. NGC 4214

1996 ◽  
Vol 471 (1) ◽  
pp. 211-236 ◽  
Author(s):  
Henry A. Kobulnicky ◽  
Evan D. Skillman
Keyword(s):  
Massive Stars ◽  
Elemental Abundance ◽  
Chemical Enrichment

scholarly journals Supernova Yields for Chemical Evolution Modeling

2013 ◽  
Vol 9 (S298) ◽  
pp. 154-166
Author(s):  
Ken'ichi Nomoto ◽  
Tomoharu Suzuki
Keyword(s):  
Chemical Evolution ◽  
Massive Stars ◽  
Elemental Abundance ◽  
Solar Abundance ◽  
Abundance Pattern ◽  
Chemical Enrichment ◽  
Abundance Patterns ◽  
Yield Table ◽  
Supernova Explosions ◽  
Evolution Modeling

AbstractWe review the recent results of the nucleosynthesis yields of massive stars. We examine how those yields are affected by some hydrodynamical effects during the supernova explosions, namely, explosion energies from those of hypernovae to faint supernovae, mixing and fallback of processed materials, asphericity, etc. Those parameters in the supernova nucleosynthesis models are constrained from observational data of supernovae and metal-poor stars. The elemental abundance patterns observed in extremely metal-poor stars show some peculiarities relative to the solar abundance pattern, which suggests the important contributions of hypernovae and faint supernovae in the early chemical enrichment of galaxies. These constraints on supernova nucleosynthesis are taken into account in the latest yield table for chemical evolution modeling.

scholarly journals Chemical Evolution of Galaxies: Abundance Trends and Implications

1991 ◽  
Vol 145 ◽  
pp. 13-19
Author(s):  
James W. Truran
Keyword(s):  
Massive Stars ◽  
Current Knowledge ◽  
Spectroscopic Studies ◽  
Early History ◽  
Elemental Abundance ◽  
Type Ii ◽  
Halo Stars ◽  
Abundance Patterns ◽  
Abundance Trends ◽  
History Of

Recent spectroscopic studies of the elemental abundance patterns associated with extremely metal deficient field halo stars and globular cluster stars are briefly reviewed. These metal deficient stellar populations have been found to be characterized by abundance patterns which differ quite distinctly from those of solar system abundances, but are consistent with the view that they reflect primarily the nucleosynthesis products of the evolution of massive stars and associated Type II supernovae. Guided by our current knowledge of nucleosynthesis as a function of stellar mass occurring in stars and supernovae, we identify some interesting constraints upon theories of the formation and early history of our Galaxy.

scholarly journals Simulated X-Ray Emission from Starburst Driven Winds

1998 ◽  
Vol 188 ◽  
pp. 287-288
Author(s):  
D. K. Strickland ◽  
I. R. Stevens ◽  
T. J. Ponman
Keyword(s):  
Galaxy Evolution ◽  
Massive Stars ◽  
Temperature Structure ◽  
Mass Loading ◽  
X Ray ◽  
Chemical Enrichment ◽  
Hot Gas ◽  
Galactic Winds ◽  
Complex Temperature ◽  
Initial Results

Winds from massive stars and supernovae in starburst galaxies drive global outflows of hot X-ray emitting plasma, as seen in M82 and NGC 253. These galactic winds are important for understanding galaxy evolution & formation, chemical enrichment of the IGM, and the starburst phenomenon itself.X-ray observations provide the only direct probe of the hot gas in these winds. However, the limitations of current X-ray observatories and factors such as complex temperature structure, mass loading by ambient material and projection effects all make the link between the observed data and existing 1 & 2-D modeling and theory difficult to make.We have therefore begun a program of numerical simulations of galactic winds, concentrating on predicting their observable X-ray properties. We present some initial results, comparing them to the archetypal starburst wind system M82.

scholarly journals Chemical evolution of the Galaxy disk in connection with large-scale winds

2008 ◽  
Vol 4 (S254) ◽  
pp. 393-398
Author(s):  
Takuji Tsujimoto ◽  
Joss Bland-Hawthorn ◽  
Kenneth C. Freeman
Keyword(s):  
Chemical Evolution ◽  
Large Scale ◽  
Solar Neighborhood ◽  
Elemental Abundance ◽  
Abundance Gradient ◽  
Chemical Enrichment ◽  
Outer Disk ◽  
The Galaxy ◽  
Galaxy Disk ◽  
Set Up

AbstractComparison of elemental abundance features between old and young thin disk stars may reveal the action of ravaging winds from the Galactic bulge, which once enriched the whole disk, and set up the steep abundance gradient in the inner disk (RGC ≲ 10–;12 kpc) and simultaneously the metallicity floor ([Fe/H]~ −0.5) in the outer disk. After the end of a crucial influence by winds, chemical enrichment through accretion of a metal-poor material from the halo onto the disk gradually reduced the metallicity of the inner region, whereas an increase in the metallicity proceeded beyond a solar circle. This results in a flattening of abundance gradient in the inner disk, and our chemical evolution models confirm this mechanism for a flattening, which is in good agreement with the observations. Our scenario also naturally explains an observed break in the metallicity floor of the outer disk by young stars since the limit of self-enrichment in the outer disk is supposed to be [Fe/H]≲ −1 and inevitably incurs a direct influence of the dilution by a low-metal infall whose metallicity is [Fe/H]~ −1. Accordingly, we propose that the enrichment by large-scale winds is a crucial factor for chemical evolution of the disk, and claim to reconsider the models thus far for the disk including the solar neighborhood, in which the metallicity is predicted to monotonously increase with time. Furthermore, we anticipate that a flattening of abundance gradient together with a metal-rich floor in the outer disk are the hallmark of disk galaxies with significant central bulges.

scholarly journals Star Formation in Disk Galaxies

1998 ◽  
Vol 15 (1) ◽  
pp. 118-122 ◽  
Author(s):  
Rosemary F. G. Wyse ◽  
Annette M. N. Ferguson ◽  
Jay S. Gallagher ◽  
Deidre A. Hunter
Keyword(s):  
Star Formation ◽  
Interstellar Medium ◽  
Massive Stars ◽  
Broad Band ◽  
Hii Regions ◽  
Disk Galaxies ◽  
Chemical Enrichment

AbstractWe present results, some preliminary, from a major new study of the star formation properties of a sample of nearby disk galaxies (Ferguson 1997). Our emphasis is on the faint outer regions of disks. Hα images, combined with broad-band images and spectroscopy of HII regions, constrain the present and past star formation rates and chemical enrichment. These data also allow study of faint diffuse ionised gas, which traces the influence of massive stars on their environment, and the structure of the interstellar medium.

scholarly journals Iron-peak elements Sc, V, Mn, Cu, and Zn in Galactic bulge globular clusters

2018 ◽  
Vol 616 ◽  
pp. A18 ◽  
Author(s):  
H. Ernandes ◽  
B. Barbuy ◽  
A. Alves-Brito ◽  
A. Friaça ◽  
C. Siqueira-Mello ◽  
...  
Keyword(s):  
Globular Clusters ◽  
Massive Stars ◽  
Theoretical Models ◽  
Thick Disk ◽  
Galactic Bulge ◽  
Abundance Pattern ◽  
Chemical Enrichment ◽  
Very Large Telescope ◽  
Type Ia ◽  
Cu And Zn

Aims. Globular clusters are tracers of the history of star formation and chemical enrichment in the early Galaxy. Their abundance pattern can help understanding their chemical enrichment processes. In particular, the iron-peak elements have been relatively little studied so far in the Galactic bulge. Methods. The main aim of this work is to verify the strength of abundances of iron-peak elements for chemical tagging in view of identifying different stellar populations. Besides, the nucleosynthesis processes that build these elements are complex, therefore observational data can help constraining theoretical models, as well as give suggestions as to the kinds of supernovae that enriched the gas before these stars formed. Results. The abundances of iron-peak elements are derived for the sample clusters, and compared with bulge field, and thick disk stars. We derived abundances of the iron-peak elements Sc, V, Mn, Cu, and Zn in individual stars of five bulge globular clusters (NGC 6528, NGC 6553, NGC 6522, NGC 6558, HP 1), and of the reference thick disk/or inner halo cluster 47 Tucanae (NGC 104). High resolution spectra were obtained with the UVES spectrograph at the Very Large Telescope over the years. Conclusions. The sample globular clusters studied span metallicities in the range –1.2 ≲ [Fe/H] ≲ 0.0. V and Sc appear to vary in lockstep with Fe, indicating that they are produced in the same supernovae as Fe. We find that Mn is deficient in metal-poor stars, confirming that it is underproduced in massive stars; Mn-over-Fe steadily increases at the higher metallicities due to a metallicity-dependent enrichment by supernovae of type Ia. Cu behaves as a secondary element, indicating its production in a weak-s process in massive stars. Zn has an alpha-like behaviour at low metallicities, which can be explained in terms of nucleosynthesis in hypernovae. At the metal-rich end, Zn decreases with increasing metallicity, similarly to the alpha-elements.

scholarly journals The Galactic Thick Disk: An Observational Perspective

2009 ◽  
Vol 5 (S265) ◽  
pp. 289-299
Author(s):  
Bacham E. Reddy
Keyword(s):  
Galaxy Formation ◽  
Chemical Properties ◽  
Thick Disk ◽  
Elemental Abundance ◽  
Distinct Component ◽  
Chemical Enrichment ◽  
Abundance Patterns ◽  
The Galaxy ◽  
Star Formation Histories ◽  
And Chemical Properties

AbstractIn this review, we present a brief description of observational efforts to understand the Galactic thick disk and its relation to the other Galactic components. This review primarily focused on elemental abundance patterns of the thick disk population to understand the process or processes that were responsible for its existence and evolution. Kinematic and chemical properties of disk stars establish that the thick disk is a distinct component in the Milky Way, and its chemical enrichment and star formation histories hold clues to the bigger picture of understanding the Galaxy formation.

Spectroscopic Abundance Determinations in M Supergiants

1980 ◽  
Vol 4 (1) ◽  
pp. 93-95
Author(s):  
P. J. McGregor
Keyword(s):  
Mass Loss ◽  
Massive Stars ◽  
Solar Neighbourhood ◽  
Carbon Stars ◽  
Chemical Enrichment ◽  
Galaxy Type ◽  
Late Stages

The M supergiants are rare objects in the solar neighbourhood and consequently until recently their importance has been largely overlooked. It is now being realized that these stars hold the key to extragalactic distance determinations since they can be detected at large distances while the maximum luminosity they attain seems to be remarkably constant and independent of galaxy type (Sandage and Tammann 1974; Humphreys 1978, 1979a, 1979b; Humphreys and Davidson 1979). They are also important in their own right since they are massive stars in the late stages of their evolution and undoubtedly suffer from mass loss and chemical enrichment due to the mixing of processed materials to their surfaces. In this light they can be considered as precursors of the luminous carbon stars and supernovae.

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