Most stars form not in isolation but as part of a group. Many of them are initially surrounded by disks which potentially develop into planetary systems. 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 disks and planetary systems. There are two ways to use this data base:
The data base covers a wide range of periastron distances and mass ratios between the mass of the perturber and central star (see table below). When using the graphics option one can display the eccentricities, inclinations, semimajor axes, angle of periastron, or longitude of ascending node of all particles (in an initial 100 au disk) after the encounter.
Please refer to the the following papers for further details on the numerical method.
1. Breslau et. al (2017): From star-disc encounters to numerical solutions for a subset of the restricted three-body problem.
2. Bhandare et. al (2016): Effects of inclined star disk encounters on protoplanetary disk size.
3. Breslau et. al (2014): Sizes of protoplanetary discs after star-disc encounters.
Click to download the datasets.
The movie on the left shows a face-on and edge-on view of the disk during an encounter (courtesy: Manuel Steinhausen) while the one 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.
|Mass ratio (perturber mass / host mass)||0.3, 0.5, 1.0, 2.0, 5.0, 10.0, 20.0, 50.0|
|Angle of periastron (degrees)||0, 45, 90|
|Orbital inclination (degrees)||0, 10, 20, 30, 40, 50, 60, 70, 80, 90, 100, 110, 120, 130, 140, 150, 160, 170, 180|
|Periastron distance (au)||30, 50, 70, 100, 120, 150, 200, 250, 300, 500, 700, 1000|