  Luminous Blue Variables (LBVs) are massive stars caught in a post-main
sequence phase, during which they are losing a significant amount of mass. As,
on one hand, it is thought that the majority of massive stars are close
binaries that will interact during their lifetime, and on the other, the most
dramatic example of an LBV, Eta Car, is a binary, it would be useful to find
other binary LBVs. We present here interferometric observations of the LBV HR
Car done with the AMBER and PIONIER instruments attached to ESO's Very Large
Telescope Interferometer (VLTI). Our observations, spanning two years, clearly
reveal that HR Car is a binary star. It is not yet possible to constrain fully
the orbit, and the orbital period may lie between a few years and several
hundred years. We derive a radius for the primary in the system and possibly
resolve as well the companion. The luminosity ratio in the H-band between the
two components is changing with time, going from about 6 to 9. We also
tentatively detect the presence of some background flux which remained at the
2% level until January 2016, but then increased to 6% in April 2016. Our AMBER
results show that the emission line forming region of Br gamma is more extended
than the continuum emitting region as seen by PIONIER and may indicate some
wind-wind interaction. Most importantly, we constrain the total masses of both
components, with the most likely range being 33.6 and 45 solar masses. Our
results show that the LBV HR Car is possibly an Eta Car analog binary system
with smaller masses, with variable components, and further monitoring of this
object is definitively called for.
