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The Evolution of Galaxies [PDF]
Publications of the Astronomical Society of the Pacific, 1959 spiral structure is rather more open. In Sc nebulae the nucleus is very small, becoming quite inconspicuous in type Sc+. The spiral arms are very loosely wound and have a patchy structure due to the presence of supergiant stars and emission nebulae.
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Chemical Evolution of the Galaxy
Annual Review of Astronomy and Astrophysics, 1991Since the discovery of the cosmic microwave background ( 1 84), it is gen erally assumed that the universe originated from a hot big bang (78). Detailed nucleosynthesis calculations based on the hot big bang model (e.g. 4, 1 82, 221 ) showed that no element heavier than 9Be could have been synthesized primordially with an abundance exceeding 101 4 by ...
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Galaxy Formation and Evolution
Space Science Reviews, 2016In this chapter, we discuss the current status of observational and computational studies on galaxy formation and evolution. In particular, a joint analysis of star-formation rates (SFRs), stellar masses, and metallicities of galaxies throughout cosmic time can shed light on the processes by which galaxies build up their stellar mass and enrich the ...
Kentaro Nagamine +4 more
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1975
The methods by which the masses and mass-to light ratios of galaxies are determined from the velocity dispersions of stars and from dynamical studies of clusters of galaxies are outlined. It is concluded that while small clusters give no evidence for “missing mass” there is a discrepancy of about a factor of 5 in the case of large clusters.
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The methods by which the masses and mass-to light ratios of galaxies are determined from the velocity dispersions of stars and from dynamical studies of clusters of galaxies are outlined. It is concluded that while small clusters give no evidence for “missing mass” there is a discrepancy of about a factor of 5 in the case of large clusters.
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1976
Galaxies come in a wide variety of shapes and sizes. Until now, it has not really mattered for the purposes of this book just how galaxies differ from one another — we have been primarily concerned to account for their existence, and have considered them as ‘test particles’ which enable us to observe the expansion of the Universe. But if we are to find
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Galaxies come in a wide variety of shapes and sizes. Until now, it has not really mattered for the purposes of this book just how galaxies differ from one another — we have been primarily concerned to account for their existence, and have considered them as ‘test particles’ which enable us to observe the expansion of the Universe. But if we are to find
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The Evolution of Galaxies in Clusters
Annual Review of Astronomy and Astrophysics, 1984Clusters of galaxies are laboratories for the study of galaxy evolution. Predictions of the effects of tidal stripping, merging, and accretion are compared to optical observations, particularly in connection with the formation of galaxies in rich clusters.
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BARRED GALAXIES AND GALAXY EVOLUTION
2007We know from near-infrared imaging that bars are present in more than three quarters of local disk galaxies. Several studies have recently led to the con- clusion that the fraction, as well as the properties, of bars in galaxies have not changed much from a redshift of about unity to the present day.
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2002
We review recent ideas on the evolution of galaxies. Two models are competing to explain the observational features: the monolithic model in which galaxies assemble at high redshift, and evolve with little influence from the environment, and the hierarchical model in which small galaxies progressively assemble to form bigger objects.
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We review recent ideas on the evolution of galaxies. Two models are competing to explain the observational features: the monolithic model in which galaxies assemble at high redshift, and evolve with little influence from the environment, and the hierarchical model in which small galaxies progressively assemble to form bigger objects.
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