  Dissipative dark matter self-interactions can affect halo evolution and
change its structure. We perform a series of controlled N-body simulations to
study impacts of the dissipative interactions on halo properties. The interplay
between gravitational contraction and collisional dissipation can significantly
speed up the onset of gravothermal collapse, resulting in a steep inner density
profile. For reasonable choices of model parameters controlling the
dissipation, the collapse timescale can be a factor of 10-100 shorter than that
predicted in purely elastic self-interacting dark matter. The effect is
maximized when energy loss per collision is comparable to characteristic
kinetic energy of dark matter particles in the halo. Our simulations provide
guidance for testing the dissipative nature of dark matter with astrophysical
observations.
