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We provide a physical interpretation and explanation of themorphology-density relation for galaxies, drawing on stellar masses, starformation rates, axis ratios and group halo masses from the Sloan Digital SkySurvey. We first re-cast the classical morphology-density relation in morequantitative terms, using low star formation rate (quiescence) as a proxy forearly-type morphology and dark matter halo mass from a group catalog as a proxyfor environmental density: for galaxies of a given stellar mass the quiescentfraction is found to increase with increasing dark matter halo mass. Our novelresult is that - at a given stellar mass - quiescent galaxies are significantlyflatter in dense environments, implying a higher fraction of disk galaxies.Supposing that the denser environments differ simply by a higher incidence ofquiescent disk galaxies that are structurally similar to star-forming diskgalaxies of similar mass, explains simultaneously and quantitatively thesequiescence -nvironment and shape-environment relations. Our findings addconsiderable weight to the slow removal of gas as the main physical driver ofthe morphology-density relation, at the expense of other explanations.

The Physical Origins of The Morphology-Density Relation: Evidence for Gas Stripping from the SDSS