A general procedure to build self-gravitational, rotating equilibrium structures with the Smoothed Particle Hydrodynamics (SPH) technique does not exist. In particular, obtaining
stable rotating configurations for white dwarf (WD) stars is
currently a major drawback of many astrophysical simulations.
Rotating WDs with low internal temperatures are connected with
both, explosive and implosive scenarios such as type Ia supernova
explosions or neutron stars formation. Simulations of these events
with SPH codes demand stable enough particle configurations as
initial models. In this work we have developed and tested a relaxation method to obtain equilibrium configurations of rotating
WDs. This method is straightforward and takes advantage of the
excellent mass and angular momentum conservation properties
of the SPH technique. Although we focus on rigid rotation and
its potential applications to several Type Ia supernova scenarios,
we also show that our proposal is also able to provide good initial
models in differential rotation, which has the potential to benefit
many other types of simulations where rotation plays a capital
role, like disk evolution and stellar formation.
