Projekt

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The first goal of this project is to carefully analyse how accretion processes such as tidal disruption and accretion of stars are affected by the stability of dense stellar systems around SMBH and to numerically study the validity of the (typically) linear stability analysis for real systems. The centre of our own Galaxy is an important prototype to let our models undergo a reality check in comparison with a wealth of recent observational data of the distribution of stars there. The second goal of the project is to investigate how the presence of the gas changes the stability of the central star cluster and the star accretion rates (by interaction of the stars with the gas) and how much gas from the central disk will be accreted onto the SMBH. Here the lifetime and stability of the central AD will also be investigated.

• Prof. Dr. Rainer Spurzem

  Universität Heidelberg
  Zentrum für Astronomie
  Astronomisches Rechen-Institut
  Heidelberg
  

• Prof. Dr. Andreas Just

  Universität Heidelberg
  Zentrum fuer Astronomie der Universitaet
  Astronomisches Rechen-Institut
  Heidelberg
  

• Dr. Peter Berczik

  National Academy of Sciences of Ukraine
  Main Astronomical Observatory
  Kiev
  Ukraine
  

• Dr. Evgeny Polyachenko

  Russian Academy of Sciences
  Institute of Astronomy
  Moskau
  Russland
  

• Multiarm spirals on the periphery of disc galaxies

• Bar formation in the Milky Way type galaxie

• On the bar formation mechanism in galaxies with cuspy bulges

• Radial orbit instability in systems of highly eccentric orbits: Antonov problem reviewed

• Instability of the cored barotropic disc: the linear eigenvalue formulation