  We present observations at 610 MHz and 235 MHz using the Giant Metrewave
Radio Telescope (GMRT) of the recurrent nova V745 Scorpii which recorded its
last outburst on 6 February 2014. This is the second symbiotic recurrent nova
whose light curve at low frequencies has been followed in detail, the first
being RS Ophiuchi in 2006. We fitted the 610 MHz light curve by a model of
synchrotron emission from an expanding shell being modified by radiative
transfer effects due to local absorbing gas consisting of a uniformly
distributed and a clumpy component. Using our model parameters, we find that
the emission at 235 MHz peaked around day 35 which is consistent with our GMRT
observations. The two main results of our study are: (1) The radio emission at
a given frequency is visible sooner after the outburst in successive outbursts
of both V745 Scorpii and RS Ophiuchi. The earlier detection of radio emission
is interpreted to be caused by decreasing foreground densities. (2) The clumpy
material, if exists, is close to the white dwarf and can be interpreted as
being due to the material from the hot accretion disk. The uniform density gas
is widespread and attributed to the winds blown by the white dwarf. We present
implications of these results on the evolution of both novae. Such studies
alongwith theoretical understanding have the potential of resolving several
outstanding issues such as why all recurrent novae are not detectable in
synchrotron radio and whether recurrent novae are progenitor systems of type 1a
supernova.
