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A protoplanetary disk typically forms a dead zone near its midplane at thedistance of a few au from the central protostar. Accretion through such amagnetically layered disk can be intrinsically unstable and has been associatedwith episodic outbursts in young stellar objects. We present the firstinvestigation into the effects of low metallicity environment on the structureof the dead zone as well as the resulting outbursting behavior of theprotoplanetary disk. We conducted global numerical hydrodynamic simulations ofprotoplanetary disk formation and evolution in the thin-disk limit. Theconsequences of metallicity were considered via its effects on the gas and dustopacity of the disk, the thickness of the magnetically active surface layer,and the temperature of the prestellar cloud core. We show that the metal poordisks accumulate much more mass in the innermost regions, as compared to thesolar metallicity counterparts. The duration of the outbursting phase alsovaries with metallicity - the low metallicity disks showed more powerfulluminosity eruptions with a shorter burst phase, which was confined mostly tothe early, embedded stages of the disk evolution. The lowest metallicity diskswith the higher cloud core temperature showed the most significant differences.The occurrence of outbursts was relatively rare in the disks around low massstars and this was especially true at lowest metallicities. We conclude thatthe metal content of the disk environment can have profound effects on both thedisk structure and evolution in terms of episodic accretion.

Eruptive Behavior of Magnetically Layered Protoplanetary Disks in Low Metallicity Environments