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Recent observations of the white dwarf (WD) populations in the Galacticglobular cluster NGC 6397 suggest that WDs receive a kick of a few km/s shortlybefore they are born. Using our Monte Carlo cluster evolution code, whichincludes accurate treatments of all relevant physical processes operating inglobular clusters, we study the effects of the kicks on their host cluster andon the WD population itself. We find that in clusters whose velocity dispersionis comparable to the kick speed, WD kicks are a significant energy source forthe cluster, prolonging the initial cluster core contraction phasesignificantly so that at late times the cluster core to half-mass radius ratiois a factor of up to ~ 10 larger than in the no-kick case. WD kicks thusrepresent a possible resolution of the large discrepancy between observed andtheoretically predicted values of this key structural parameter. Our modelingalso reproduces the observed trend for younger WDs to be more extended in theirradial distribution in the cluster than older WDs.

The Dynamical Effects of White Dwarf Birth Kicks in Globular Star Clusters