Most stars form not in isolation but as part of a stellar group. Many of them are initially surrounded by disks, which can eventually harbor planet(s). Both the disk as well as planetary systems may be affected by the cluster environment due to close fly-bys. The here presented database can be used to determine the effect of such fly-bys on non-viscous disks and planetary systems.


There are two ways to use this database:

Fly-by scenarios

The movie on the left shows a face-on and edge-on view of the disk during an encounter (courtesy: Manuel Steinhausen). The movie on the right shows a face-on view of the disk, where the particles marked in blue are those that remain bound to the host star and the particles in red become unbound due to the encounter.


Please refer to the the following papers for further details on the numerical method.

  1. Bhandare et. al (2019): DESTINY: Database for the Effects of STellar encounters on dIsks and plaNetary sYstems
  2. Breslau et. al (2017): From star-disc encounters to numerical solutions for a subset of the restricted three-body problem
  3. Bhandare et. al (2016): Effects of inclined star disk encounters on protoplanetary disk size
  4. Breslau et. al (2014): Sizes of protoplanetary discs after star-disc encounters


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