The underlying mechanisms driving the quenching of dwarf-mass satellite galaxies remain poorly constrained , but recent studies suggest they are particularly inefficient for those satellites with stellar mass 10 ^ { 9 } M _ { \odot } .
We investigate the characteristic evolution of these systems with chemodynamical simulations and idealised models of their tidal/hydrodynamic interactions within the 10 ^ { 13 - 13.5 } M _ { \odot } group-mass hosts in which they are preferentially quenched .
Our fiducial simulations highlight the role played by secular star formation and stellar bars , and demonstrate a transition from a gas-rich to passive , H I -deficient state ( i.e . \Delta SFR \leq -1 , def _ { H { \sc I } } \geq 0.5 ) within 6 Gyr of first infall .
Furthermore , in the 8-10 Gyr in which these systems have typically been resident within group hosts , the bulge-to-total ratio of an initially bulgeless disc can increase to 0.3 < B/T < 0.4 , its specific angular momentum \lambda _ { R } reduce to \sim 0.5 , and strong bisymmetries formed .
Ultimately , this scenario yields satellites resembling dwarf S0s , a result that holds for a variety of infall inclinations/harassments albeit with broad scatter .
The key assumptions here lie in the rapid removal of the satellite ’ s gaseous halo upon virial infall , and the satellite ’ s local intra-group medium density being defined by the host ’ s spherically-averaged profile .
We demonstrate how quenching can be greatly enhanced if the satellite lies in an overdensity , consistent with recent cosmological-scale simulations but contrasting with observationally-inferred quenching mechanisms/timescales ; an appraisal of these results with respect to the apparent preferential formation of dS0s/S0s in groups is also given .