  LBVs are massive evolved stars that suffer sporadic and violent mass-loss
events. They have been proposed as the progenitors of some core-collapse SNe,
but this idea is still debated due to the lack of direct evidence. Since SNRs
can carry in their morphology the fingerprints of the progenitor stars as well
as of the inhomogeneous CSM sculpted by the progenitors, the study of SNRs from
LBVs could help to place core-collapse SNe in context with the evolution of
massive stars. We investigate the physical, chemical and morphological
properties of the remnants of SNe originating from LBVs, in order to search for
signatures, revealing the nature of the progenitors, in the ejecta distribution
and morphology of the remnants. As a template of LBVs, we considered the actual
LBV candidate Gal 026.47+0.02. We selected a grid of models, which describe the
evolution of a massive star with properties consistent with those of Gal
026.47+0.02 and its final fate as core-collapse SN. We developed a 3D HD model
that follows the post-explosion evolution of the ejecta from the breakout of
the shock wave at the stellar surface to the interaction of the SNR with a CSM
characterized by two dense nested toroidal shells, parametrized in agreement
with multi-wavelength observations of Gal 026.47+0.02. Our models show a strong
interaction of the blast wave with the CSM which determines an important
slowdown of the expansion of the ejecta in the equatorial plane where the two
shells lay, determining a high degree of asymmetry in the remnant. After 10000
years of evolution the ejecta show an elongated shape forming a broad jet-like
structure caused by the interaction with the shells and oriented along the axis
of the toroidal shells.
