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This study confirms MLS110213:022733+130617 as a new eclipsing polar. Weperformed optical spectroscopic, polarimetric and photometric follow-up of thisvariable source identified by the Catalina Real Time Transient Survey. Usingthe mid-eclipse times, we estimated an orbital period of 3.787 h, which isabove the orbital period gap of the cataclysmic variables. There are nine otherknown polars with longer orbital periods, and only four of them are eclipsing.We identified high and low-brightness states and high polarization modulatedwith the orbital period. The spectra are typical of polars, with strong highionization emission lines and inverted Balmer decrement. The HeII4686 A line isas strong as Hbeta. We modelled the photometric and polarimetric bright-statelight curves using the CYCLOPS code. Our modelling suggests an extendedemitting region on the WD surface, with a mean temperature of 9 keV and B inthe range 18 -- 33 MG, although the possibility that it could be a two-poleaccretor cannot yet be ruled out. The WD mass estimated from the shocktemperature is 0.67 Msol. The derived parameters are consistent with theeclipse profile. The distance was estimated as 406+- 54 pc using thePeriod-Luminosity-Colours method. MLS110213 populates a rare sub-group ofpolars, near the upper limit of the period distribution, important tounderstand the evolution of mCVs.

MLS110213:022733+130617: A new eclipsing polar above the period gap