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We apply for the first time the Monte Carlo star cluster modeling method tostudy tidal tail and stellar stream formation from globular clusters, assuminga circular orbit in a smooth Galactic potential. Approximating energeticallyunbound bodies (potential escapers; PEs) as collisionless enables this fast butspherically symmetric method to capture asymmetric tidal phenomena withunprecedented detail. Beyond reproducing known stream features, includingepicyclic overdensities, we show how 'returning tidal tails' may form after thestream fully circumnavigates the Galaxy back to the cluster, enhancing thestream's velocity dispersion. While a realistically clumpy, time-dependentGalactic potential may disrupt such tails, they warrant scrutiny as potentiallyexcellent constraints on the Galactic potential's history and substructure.Re-examining the escape timescale $\Delta t$ of PEs, we find new behaviorrelated to chaotic scattering in the three-body problem; the $\Delta t$distribution features sharp plateaus corresponding to distinct locally smoothpatches of the chaotic saddle separating the phase space basins of escape. Westudy for the first time $\Delta t$ in an evolving cluster, finding that$\Delta t\sim(E_{\rm J}^{-0.1},E_{\rm J}^{-0.4})$ for PEs with (low, high)Jacobi energy $E_{\rm J}$, flatter than for a static cluster ($E_{\rmJ}^{-2}$). Accounting for cluster mass loss and internal evolution -- and(roughly) for ongoing relaxation among PEs -- lowers the median $\Delta t$ from${\sim}10\,$Gyr to ${\lesssim}100\,$Myr. We finally outline future improvementsto escape physics in the Monte Carlo method intended to enable both the firstlarge-parameter-space studies of tidal tail/stellar stream formation from fullglobular cluster simulations and detailed comparisons to stream observations.

Stellar Escape from Globular Clusters. II. Clusters May Eat Their Own Tails