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Supermassive black holes dominate the gravitational potential in galacticnuclei. In these dense environments, stars follow nearly Keplerian orbits andsee their orbital planes relax through the potential fluctuations generated bythe stellar cluster itself. For typical astrophysical galactic nuclei, the mostlikely outcome of this vector resonant relaxation (VRR) is that the orbitalplanes of the most massive stars spontaneously self-align within a narrow disc.We present a maximum entropy method to systematically determine this long-termdistribution of orientations and use it for a wide range of stellar orbitalparameters and initial conditions. The heaviest stellar objects are found tolive within a thin equatorial disk. The thickness of this disk depends on thestars' initial mass function, and on the geometry of the initial cluster. Thiswork highlights a possible (indirect) novel method to constrain thedistribution of intermediate mass black holes in galactic nuclei.

Orbital alignment and mass segregation in galactic nuclei via vector resonant relaxation