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The Magellanic Stream is unique to sample the MW potential from ~50 kpc to300 kpc, and is also unique in constraining the LMC mass, an increasinglyimportant question for the Local Group/Milky Way modeling. Here we comparestrengths and weaknesses of the two types of models (tidal and ram-pressure) ofthe Magellanic Stream formation. I will present our modeling for the formationof the Magellanic System, including those of the most recent discoveries in theStream, in the Bridge and at the outskirts of Magellanic Clouds. This model hasbeen successful in predicting most recent observations in both properties ofstellar and gas phase. It appears that it is an over-constrained model andprovides a good path to investigate the Stream properties. In particular, thismodel requires a LMC mass significantly smaller than 110^{11} Msun

The Formation of Magellanic System and the total mass of Large Magellanic Cloud