SUPERNOVA FALLBACK ONTO MAGNETARS AND PROPELLER-POWERED SUPERNOVAE

Abstract

We explore fallback accretion onto newly born magnetars during the supernova of massive stars. Strong magnetic fields (~10^{15} G) and short spin periods (~1-10 ms) have an important influence on how the magnetar interacts with the infalling material. At long spin periods, weak magnetic fields, and high accretion rates, sufficient material is accreted to form a black hole, as is commonly found for massive progenitor stars. When B<5*10^{14} G, accretion causes the magnetar to spin sufficiently rapidly to deform triaxially and produce gravitational waves, but only for ~50-200 s until it collapses to a black hole. Conversely, at short spin periods, strong magnetic fields, and low accretion rates, the magnetar is in the "propeller regime" and avoids becoming a black hole by expelling incoming material. This process spins down the magnetar, so that gravitational waves are only expected if the initial protoneutron star is spinning rapidly. Even when the magnetar survives, it accretes at least ~0.3 solar masses, so we expect magnetars born within these types of environments to be more massive than the 1.4 solar masses typically associated with neutron stars. The propeller mechanism converts the ~10^{52} ergs of spin energy in the magnetar into the kinetic energy of an outflow, which shock heats the outgoing supernova ejecta during the first ~10-30 s. For a small ~5 solar mass hydrogen-poor envelope, this energy creates a brighter, faster evolving supernova with high ejecta velocities ~(1-3)*10^4 km/s and may appear as a broad-lined Type Ib/c supernova. For a large >10 solar mass hydrogen-rich envelope, the result is a bright Type IIP supernova with a plateau luminosity of ~10^{43} ergs/s lasting for a timescale of ~60-80 days.