On the origin of the absorption and emission line components in the
  spectra of PHL 293B
  From the structure of PHL 293B and the physical properties of its ionizing
cluster and based on results of hydrodynamic models, we point at the various
events required to explain in detail the emission and absorption components
seen in its optical spectrum. We ascribe the narrow and well centered emission
lines, showing the low metallicity of the galaxy, to an HII region that spans
through the main body of the galaxy. The broad emission line components are due
to two off-centered supernova remnants evolving within the ionizing cluster
volume and the absorption line profiles are due to a stationary cluster wind
able to recombine at a close distance from the cluster surface, as originally
suggested by Silich et al. (2004). Our numerical models and analytical
estimates confirm the ionized and neutral column density values and the
inferred X-ray emission derived from the observations.
