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However, strangulation cannot explain the rollover in satellite quenching times at $\mstar\lesssim10^9\msun$, because the gas-rich dwarf galaxies of the LG also have $\mgas\gtrsim\mstar$ \citep{GrcevichPutman2009} and thus contain enough cold gas to fuel star formation for a Hubble time, even absent accretion.  Thus, the rapid decline at lower $\mstar$ \emph{requires} an additional process(es) to remove gas from satellites after infall.  This likely arises from the increased efficiency of ram-pressure stripping in removing cold gas from such low-mas galaxies with shallower potential wells.  Moreover, for dwarf galaxies, the same internal stellar feedback that regulates their low star-formation efficiency and likely  heats/drives significant cold gas to large radii \citep[e.g.,][]{Muratov2015} on short timescales \citep[e.g.,][]{Muratov2015}, which  would assist any  such environmental stripping to become stripping, making it  even more efficient. Thus, the rapid environmental quenching timescales for dwarf galaxies may arise from the non-linear interplay of both internal feedback and external stripping \citep[e.g.,][]{NicholsBlandHawthorn2011, BaheMcCarthy2015}.  Overall, satellites with $\mstar\sim10^9\msun$ (similar to the Magellanic Clouds) represent the transition between these effects, and no quenching mechanism (either internal or external) appears to operate efficiently near this mass \citep[see also][]{Weisz2015}.