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Accretion Disks - New Aspects by Emmi Meyer-Hofmeister, Henk Spruit

By Emmi Meyer-Hofmeister, Henk Spruit

The main luminous compact items are powered by way of accretion of mass. Accretion disks are the only universal and primary component of those resources on broadly various scales, starting from shut stellar binaries, galactic black holes and X-ray pulsars to energetic galactic nuclei (AGN). Key new advancements in thought and observations, reviewed by means of specialists within the box, are awarded during this booklet. The contributions to the workshop hide the puzzles awarded by way of the X-UV spectra of AGN and their variability, the hot numerical simulations of magnetic fields in disks, the awesome habit of the superluminal resource 1915+105 and the "bursting pulsar" 1744-28, to say a number of the issues.

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4 below) and the stellar mass function slope. 5 Fig. 4. The metallicity distribution of Milky Way globular clusters. Also shown are the individual Gaussian fits to the two populations determined by mixture-modeling. have smaller, denser cores but at all luminosities there is considerable scatter in this relationship. Djorgovski and Meylan (1994) find a deficiency of high-luminosity, lowconcentration clusters and low-luminosity, high-concentration clusters. 5 below). The two most notable correlations, other than those depending on position within the Galaxy, involve globular cluster velocity dispersion which increases with both luminosity and central surface brightness.

Currently, there does not appear to be a consensus on whether these variations have a primordial or evolutionary origin. For the main thrust of this book and as clues to the globular cluster formation process, two issues revealed by abundance studies stand out. The first is that the chemical homogeneity of iron-peak elements in globular clusters is a unique feature of these objects not shared by other stellar systems. The second is the possibility that some global property of globular clusters may be influencing some of the elemental abundances of their constituent stars.

1996). There are several problems in using these observational results to compare the frequency of binarism in globular clusters to that in the field. The current database for globular clusters is still relatively small and is comprised of surveys adopting different strategies and probing different period ranges. Further, it appears that the binary fraction varies from one globular cluster to another (Meylan and Heggie 1996 and references therein). Thus most estimates of the binary fraction in globular clusters rely on comparisons between observations and Monte Carlo simulations.

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