In Milgrom-law dynamics, a simulated low-mass open star cluster develops a leading tidal tail with up to twice as many stars as the trailing tail and dissolves about 25% faster than in Newtonian gravity.
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Asymmetry of the tidal tails of open star clusters in direct N-body integrations in Milgrom-law dynamics
In Milgrom-law dynamics, a simulated low-mass open star cluster develops a leading tidal tail with up to twice as many stars as the trailing tail and dissolves about 25% faster than in Newtonian gravity.