Titlebook: Dynamics and Interactions of Galaxies; Proceedings of the I Roland Wielen Conference proceedings 1990 Springer-Verlag Berlin Heidelberg 199

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書目名稱Dynamics and Interactions of Galaxies影響因子(影響力)




書目名稱Dynamics and Interactions of Galaxies影響因子(影響力)學(xué)科排名




書目名稱Dynamics and Interactions of Galaxies網(wǎng)絡(luò)公開度




書目名稱Dynamics and Interactions of Galaxies網(wǎng)絡(luò)公開度學(xué)科排名




書目名稱Dynamics and Interactions of Galaxies被引頻次




書目名稱Dynamics and Interactions of Galaxies被引頻次學(xué)科排名




書目名稱Dynamics and Interactions of Galaxies年度引用




書目名稱Dynamics and Interactions of Galaxies年度引用學(xué)科排名




書目名稱Dynamics and Interactions of Galaxies讀者反饋




書目名稱Dynamics and Interactions of Galaxies讀者反饋學(xué)科排名

Pert敏捷

Are High Redshift Galaxies Interacting?rtunately, as far as mergers at high redshifts is concerned, I cannot bring myself to do this. Instead, I propose to present you with evidence that peculiar phenomena are occurring in the most distant galaxies we can study. According to your degree of faith in the “Book of Mergers”, you can decide w

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DEFT

Interactions in “Butcher-Oemler” Clusters of galaxies at redshifts near 0.4 contained a much larger population of “blue” galaxies than expected. This suggested rapid color evolution of galaxies in 1/3 of a Hubble time. In order to put this on a more quantitative level, Butcher and Oemler (1984a) undertook a photometric study of 33 clusters

Fantasy

Are Our Globular Clusters Coeval?axy formed. A basic goal is to determine the time interval over which the Galactic halo and disk were formed, since a short time interval (< 1 Gyr) would be consistent with the picture of rapid, ordered collapse proposed by Eggen, Lynden-Bell, and Sandage (1962), whereas a much longer time interval

令人悲傷

Stellar Populations and Mergerseach population being but a different stage in the process? Or have at least some of them nothing to do with the origins and evolution of the others, as expected from mergers? In the context of this meeting, we will look particularly at the latter possibility, and will discuss briefly the data suppo

令人悲傷

A New Model of the Magellanic Stream of the Magellanic Stream. In contrast Zaritsky et al. (1989), using the statistical procedure developed by Little and Tremaine (1987), have found this mass to be 3.6 × 10. M. from the orbits of satellites of the Galaxy.

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animated

Status of Shell Galaxiesatalogue (Arp, 1966). But only recently has special attention has been drawn to them. The improvement of photographic emulsions, and the application of new photographic techniques such as “unsharp masking” and “contrast enhancement” by Malin (1977, 1981) has led to the discovery of shells and other

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