Evaporating the Milky Way halo and its satellites with inelastic
  self-interacting dark matter
  Self-interacting dark matter provides a promising alternative for the cold
dark matter paradigm to solve potential small-scale galaxy formation problems.
Nearly all self-interacting dark matter simulations so far have considered only
elastic collisions. Here we present simulations of a galactic halo within a
generic inelastic model using a novel numerical implementation in the Arepo
code to study arbitrary multi-state inelastic dark matter scenarios. For this
model we find that inelastic self-interactions can: (i) create larger subhalo
density cores compared to elastic models for the same cross section
normalisation; (ii) lower the abundance of satellites without the need for a
power spectrum cutoff; (iii) reduce the total halo mass by about 10%; (iv)
inject the energy equivalent of O(100) million Type II supernovae in galactic
haloes through level de-excitation; (v) avoid the gravothermal catastrophe due
to removal of particles from halo centers. We conclude that a ~5 times larger
elastic cross section is required to achieve the same central density reduction
as the inelastic model. This implies that well-established constraints on
self-interacting cross sections have to be revised if inelastic collisions are
the dominant mode. In this case significantly smaller cross sections can
achieve the same core density reduction thereby increasing the parameter space
of allowed models considerably.
