Abstract:
We present observations at 610 and 235 MHz using the Giant Metrewave Radio Telescope
(GMRT) of the recurrent nova V745 Scorpii which recorded its last outburst on 2014 February 6. 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 disc. 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 along with 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.
