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Rapidly spinning, strongly magnetized proto-neutron stars ("millisecondproto-magnetars") are candidate central engines of long-duration gamma-raybursts (GRB), superluminous supernovae (SLSNe), and binary neutron starmergers. Magnetar birth may be accompanied by the fall-back of stellar debris,lasting for seconds or longer following the explosion. Accretion alters themagnetar evolution by (1) providing an additional source of rotational energy(or a potential sink, if the propeller mechanism operates); (2) enhancing thespin-down luminosity above the dipole rate by compressing the magnetosphere andexpanding the polar cap region of open magnetic field lines; (3) supplying anadditional accretion-powered neutrino luminosity that sustains the windbaryon-loading, even after the magnetar's internal neutrino luminosity hassubsided. The more complex evolution of the jet power and magnetization of anaccreting magnetar more readily accounts for the high 56Ni yields GRB SNe andirregular time evolution of some GRB light curves (e.g.~bursts with precursorsfollowed by a long quiescent interval before the main emission episode).Additional baryon-loading from accretion-powered neutrino irradiation of themagnetar polar cap lengthens the timeframe over which the jet magnetization isin the requisite range sigma ~< 1e3 for efficient gamma-ray emission, therebyaccommodating GRBs with ultra-long durations. Though accretion does notsignificantly raise the maximum energy budget from the limit of <~ few 1e52ergs for an isolated magnetar, it greatly expands the range of magnetic fieldstrengths and birth spin periods capable of powering GRB jets, reducing thedifferences between the magnetar properties normally invoked to explain GRBsversus SLSNe.

Effects of Fall-Back Accretion on Proto-Magnetar Outflows in Gamma-Ray Bursts and Superluminous Supernovae