Title: Modelling Luminous-Blue-Variable Isolation,
Abstract: Observations show that luminous blue variables (LBVs) are far more dispersed
than massive O-type stars, and Smith & Tombleson suggested that these large
separations are inconsistent with a single-star evolution model of LBVs.
Instead, they suggested that the large distances are most consistent with
binary evolution scenarios. To test these suggestions, we modelled young
stellar clusters and their passive dissolution, and we find that, indeed, the
standard single-star evolution model is mostly inconsistent with the observed
LBV environments. If LBVs are single stars, then the lifetimes inferred from
their luminosity and mass are far too short to be consistent with their extreme
isolation. This implies that there is either an inconsistency in the
luminosity- to-mass mapping or the mass-to-age mapping. In this paper, we
explore binary solutions that modify the mass-to-age mapping and are consistent
with the isolation of LBVs. For the binary scenarios, our crude models suggest
that LBVs are rejuvenated stars. They are either the result of mergers or they
are mass gainers and received a kick when the primary star exploded. In the
merger scenario, if the primary is about 19 solar masses, then the binary has
enough time to wander far afield, merge and form a rejuvenated star. In the
mass-gainer and kick scenario, we find that LBV isolation is consistent with a
wide range of kick velocities, anywhere from 0 to ~ 105 km/s. In either
scenario, binarity seems to play a major role in the isolation of LBVs.