  Pulsar spindown forms a reliable yet enigmatic prototype for the energy loss
processes in many astrophysical objects including accretion disks and back
holes. In this paper we review the physics of pulsar magnetospheres,
concentrating on recent developments in force-free modeling of the
magnetospheric structure. In particular, we discuss a new method for solving
the equations of time-dependent force-free relativistic MHD in application to
pulsars. This method allows to dynamically study the formation of the
magnetosphere and its response to perturbations, opening a qualitatively new
window on pulsar phenomena. Applications of the method to other magnetized
rotators, such as magnetars and accretion disks, are also discussed.
