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Observations show a large spread in the luminosities of young protostars,which are frequently explained in the context of episodic accretion. We heretest this scenario using numerical simulations following the collapse of asolar mass molecular cloud using the GRADSPH code, varying the strength of theinitial perturbations and the temperature of the cores. A specific emphasis ofthis paper is to investigate the role of binaries and multiple systems in thecontext of episodic accretion, and to compare their evolution to the evolutionin isolated fragments. Our models form a variety of low mass protostellarobjects including single, binary and triple systems with binaries more activein exhibiting episodic accretion than isolated protostars. We also find ageneral decreasing trend for the average mass accretion rate over time,suggesting that the majority of the protostellar mass is accreted within thefirst 10^5 years. This result can potentially help to explain the surprisinglylow average luminosities in the majority of the protostellar population.

Episodic accretion in binary protostars emerging from self-gravitating solar mass cores