Recent discoveries of bimodal main sequences ( MSs ) associated with young clusters ( with ages \lesssim 1 Gyr ) in the Magellanic Clouds have drawn a lot of attention .
One of the prevailing formation scenarios attributes these split MSs to a bimodal distribution in stellar rotation rates , with most stars belonging to a rapidly rotating population .
In this scenario , only a small fraction of stars populating a secondary blue sequence are slowly or non-rotating stars .
Here , we focus on the blue MS in the young cluster NGC 1850 .
We compare the cumulative number fraction of the observed blue-MS stars to that of the high-mass-ratio binary systems at different radii .
The cumulative distributions of both populations exhibit a clear anti-correlation , characterized by a highly significant Pearson coefficient of -0.97 .
Our observations are consistent with the possibility that blue-MS stars are low-mass-ratio binaries , and therefore their dynamical disruption is still ongoing .
High-mass-ratio binaries , on the other hand , are more centrally concentrated .