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The evolution of many close binary and multiple star systems is defined byphases of mass exchange and interaction. As these systems evolve into contact,tidal dissipation is not always sufficient to bring them into circular,synchronous orbits. In these cases, encounters of increasing strength occurwhile the orbit remains eccentric. This paper focuses on the outcomes of closetidal passages in eccentric orbits. Close eccentric passages excite dynamicaloscillations about the stars' equilibrium configurations. These tidaloscillations arise from the transfer of orbital energy into oscillation modeenergy. When these oscillations reach sufficient amplitude, they break near thestellar surface. The surface wave-breaking layer forms a shock-heatedatmosphere that surrounds the object. The continuing oscillations in the star'sinterior launch shocks that dissipate into the this atmosphere, damping thetidal oscillations. We show that the rapid, nonlinear dissipation associatedwith the wave breaking of fundamental oscillation modes therefore comes withcoupled mass loss to the wave breaking atmosphere. The mass ratio is animportant characteristic that defines the relative importance of mass loss andenergy dissipation and therefore determines the fate of systems evolving underthe influence of nonlinear dissipation. The outcome can be rapid tidalcircularization ($q\ll1$) or runaway mass exchange ($q\gg1$).

Tidal Wave Breaking in the Eccentric Lead-In to Mass Transfer and Common Envelope Phases