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When a star passes too close to a supermassive black hole, it gets disruptedby strong tidal forces. The stellar debris then evolves into an elongatedstream of gas that partly falls back towards the black hole. We present ananalytical model describing for the first time the full stream evolution duringsuch a tidal disruption event (TDE). Our framework consists in dividing thestream into different sections of elliptical geometry, whose properties areindependently evolved in their co-moving frame under the tidal, pressure, andself-gravity forces. Through an explicit treatment of the tidal force and theinclusion of the gas angular momentum, we can accurately follow the streamevolution near pericenter. Our model evolves the longitudinal stream stretchingand both transverse widths simultaneously. For the latter, we identify tworegimes depending on whether the dynamics is entirely dominated by the tidalforce (ballistic regime) or additionally influenced by pressure andself-gravity (hydrostatic regime). We find that the stream undergoes transversecollapses both shortly after the stellar disruption and upon its return nearthe black hole, at specific locations determined by the regime of evolutionconsidered. The stream evolution predicted by our model can be used todetermine the subsequent interactions experienced by this gas that are at theorigin of most of the electromagnetic emission from TDEs. Our results suggestthat the accretion disk may be fed at a rate that differs from the standardfallback rate, which would provide novel observational signatures dependent onblack hole spin.

From Pericenter and Back: Full Debris Stream Evolution in Tidal Disruption Events