We calculate the steady-state properties of neutrino-driven winds from strongly magnetized , rotating proto-neutron stars ( ‘ proto-magnetars ’ ) under the assumption that the outflow geometry is set by the force-free magnetic field of an aligned dipole .
Our goal is to assess proto-magnetars as sites of r -process nucleosynthesis and gamma-ray burst engines .
One dimensional solutions calculated along flux tubes corresponding to different polar field lines are stitched together to determine the global properties of the flow at a given neutrino luminosity and rotation period .
Proto-magnetars with rotation periods of P \sim 2 - 5 ms are shown to produce outflows more favorable for the production of third-peak r -process nuclei due to their much shorter expansion times through the seed nucleus formation region , yet only moderately lower entropies , as compared to normal spherical PNS winds .
Proto-magnetars with moderately rapid birth periods P \sim 3 - 5 ms may thus represent a promising Galactic r -process site which is compatible with a variety of other observations , including the recent discovery of possible magnetar-powered supernovae in metal poor galaxies .
We also confirm previous results that the outflows from proto-magnetars with P \sim 1 - 2 ms can achieve maximum Lorentz factors \Gamma _ { max } \sim 100 - 1000 in the range necessary to power gamma-ray bursts ( GRBs ) .
The implications of GRB jets with a heavy nuclei-dominated composition as sources of ultra-high energy cosmic rays are also addressed .