*** Captions for animations ***

Model X002a (Fig. 2):

Animation of a circumstellar disc modelled with 250,000 SPH particles,
around a Sun-type star being perturbed by a close star-star encounter
(model X002). The time stamp in each frame refers to the time of the encounter.
The coordinate system is fixed on the central star. This can result in a slight
wobbling of the image if the star is perturbed by close-in satellites.


Model X002b (Fig. 3):

Close-up of a forming binary around about 8000 years
after the fly-by in model X002 (see also model X002).
The components of the remaining VLMS pair have masses of 0.08 M_sun and
0.09 M_sun, subsequently accreting another 0.01 M_sun each. The escaping
third body has 0.05 M_sun and is eventually ejected.
The coordinate system is fixed on the central star. This can result in a slight
wobbling of the image if the star is perturbed by close-in satellites.


Model E003 (Fig. 4):

Animation of another model with a forming binary around about 12000 years
after the encounter. The components of the remaining VLMS-BD pair have very
unequal masses of 0.09 M_sun and 0.013 M_sun (with a mass ratio q=0.14).
In contrast to the binary formed in X002, these bodies became bound due to a
frictional encounter of their accretion envelopes.
The coordinate system is fixed on the central star. This can result in a slight
wobbling of the image if the star is perturbed by close-in satellites.