Solar mass black holes from neutron stars and bosonic dark matter
  Black holes with masses $\approx 1\, M_{\odot}$ cannot be produced via
stellar evolution. A popular scenario of their formation involves transmutation
of neutron stars - by accumulation of dark matter triggering gravitational
collapse in the star centers. We show that this scenario can be realized in the
models of bosonic dark matter despite the apparently contradicting requirements
on the interactions of dark matter particles: on the one hand, they should
couple to neutrons strongly enough to be captured inside the neutron stars, on
the other, their loop-induced self-interactions impede collapse. Observing that
these conflicting conditions are imposed at different scales, we demonstrate
that models with efficient accumulation of dark matter can be deformed at large
fields to make unavoidable its subsequent collapse into a black hole. Workable
examples include weakly coupled models with bended infinite valleys.
