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Orbit Dynamics, Stability and Chaos in Planetary Systems
Let us start with a problem of dynamical biology, which was posed about 800 years ago by Fibonacci1
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Planet Formation
Motivating the study of planet formation is not difficult for any curious audience. One of the fundamental human questions is that of origins: “where...
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Applications of the Correlation Length
The correlation length is the system–dependent parameter, which defines the structure of the dominant current–carrying (electric or fluid) paths....
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Pressure Saturation Curves and the Critical Volume Fraction for Percolation
The pressure-saturation curves of porous media give fundamental information about the pore space. In equilibrium, ignoring effects due to hysteresis,...
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Effects of Multi-Scale Heterogeneity
It is generally agreed that problems with multi-scale heterogeneity present the biggest challenge to computation and understanding. A few such...
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Clusters of Galaxies at High Redshift
For a long time, the small number of clusters at z > 0.3 in the Abell survey catalogue and simulations of the standard CDM formation of large scale...
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Velocity Dispersion Analysis of CNOC Clusters
I present results of the analysis of the internal velocity dispersions,...
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The Metal Enrichment History of Clusters of Galaxies
The ratio of the total iron mass in the ICM to the total optical luminosity of the cluster (the iron mass-to-light-ratio) is the same for all...
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Supernovae at High Redshift
Distant supernovae provide a convenient tool for cosmology. As bright beacons with small variation in their peak luminosity Type Ia Supernovae can be...
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The Galactic Bulge: Prospects for the VLT
The central bulge of the Galaxy is 100 times closer than the nearest extragalactic bulge, that of M31. Until the era of 100m telescopes arrives, the...
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The Old Population of the Magellanic Clouds
The brightest old stars in the LMC are as faint as V=16 (V=16.5 in the SMC). The VLT with UVES or GIRAFFE will provide, for the first time, high...
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The Stellar Mass Function
Considerable progress has been made recently in more accurately determining the frequency distribution of stellar masses in the critical 0.1 to 1 m...
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Synergy Between the VLT and the NGST
Three major astronomical facilities will address the distant universe and processes of star formation in the next decade: the Next Generation Space...
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The Cluster Population in a Complete Sample of Optically Identified RASS X-Ray Sources
Using the 2.1-m telescope of the Guillermo Haro Observatory (Cananea, Mexico) the optical counterparts of a count-rate and area limited complete...
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Massive Stars and Their Role in Spectra and Abundances of High Redshift Galaxies
There are great changes in our understanding of massive star evolution. Although it is a known fact that the populations of massive stars (O-stars,...
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Planetary Microlensing: Present Status and Long-Term Goals
Massive gravitational microlensing programs were begun about a decade ago as a means to search for compact baryonic dark matter in the Galaxy [1],...
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Extrasolar Planets Transits: Detection and Follow-Up
The detection of transits has a rich potential of information about extrasolar planets. This contribution gives an overview and new perspectives on...
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Solar Nebulae and Replenished Dust Disks with Planets
Having studied the primordial, protoplanetary gas disks, and older, dusty “remnant” disks in infrared-emitting (Vega-type) circumstellar systems, we...
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The Darwin Space Interferometer
Darwin is a mid-IR(5-30 micron) interferometry observatory with baselines greater than 50 metres. As a long-duration general purpose observatory, ESA...
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Surveys of the Distant Solar System
The rapid development in the 1990’s of surveys for distant Centaurs and Trans-Neptunian Objects (TNOs) is reviewed. With 94 TNOs and 9 Centaurs found...