Organisation profile

The project started from 1996 to 1999 under the label OZR 252 'The Influence of Binaries on the number statistics and population synthesis of large groups of stars' and continued with a project OZR 188 from 1998 to 2001 'A library with evolutionary calculations of interacting binaries for a large variety of masses, mass ratio's and periods'. Both projects were joined together and are continued under the label FWOAL 157 (from 01.01.2000 tot 31.12.2003) The research unit Astrophysics develops research in the areas of: 1. Evolution of massive stars The evolution of a massive single star from main sequence-star, through WR-star ends with a Super Nova (SN), which leaves a white dwarf, neutron star (radio pulsar) or black hole as final product, i.e. a compact object (c). We study the influence of stellar wind on the evolution of these stars. The evolution of Massive Close Binaries (MCBs) is not only influenced by stellar wind but also by: mass loss through Roche Lobe Overflow, accretion and loss of mass in discs, the spiral of stars as a consequence of viscosity in the gravitational attraction field of a red giant. 2. Population Number Synthesis [PNS] In a starburst region the relative numbers of stars of different type is a function of age. These numbers have to be obtained following Single Star evolution schemes for the single stars (Maeder, Geneve) and the Binary Star evolution schemes for the binaries (Brussels). 3. Spectral Synthesis The spectra of galaxies are dominated by the radiation of the massive stars in that galaxy and the way that this radiation is transferred through the gas in the galaxy. Combining the results of the PNS, with the problem of radiative transfer in a galaxy, one can predict the intensity of a spectral feature as an indicator for the age of the galaxy. For instance, the equivalent width of the Balmer-betha emission line is a good index for the determination of the age of a galaxy. 4. Stellar dynamics. The density of stars in an starburst is enormous. The evolution of teh stars herein is influenced by the propability of collsions between them. The combination of single star evolution, binary evolution and dynamics describes the evolution of the starburst completely.

Contact information

Pleinlaan 2
1050
Brussels
Belgium
  • Fax: +32-2-6293614
  • Phone: +32-2-6293497

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