Dwarf novae are a subclass of Cataclysmic variable stars, which are a type of binary system
that contain a white dwarf primary star and a main-sequence secondary star (typically a K- or
an M-type star) where the secondary star transfers matter onto the white dwarf via Roche-lobe
overflow. These binary systems often have an accretion disc. Dwarf novae have outbursts, which
are 2-6 magnitude increases in the brightness of the system that usually happen in regular intervals,
which aren’t necessarily periodic. These outbursts occur on a timescale of the order of days or
even years. Occasionally, these sources will go into superoutburst, which are much brighter and
last longer than regular outbursts. The standard model that explains this is known as the disc
instability model. This involves a thermal-viscous instability that switches the accretion disc
between the outburst (hot, ionised) and quiescent (cold, unionised) states. During these processes
the non-thermal emission is believed to be driven by magnetic reconnection. The aim of this study
is to use the optical light curves of these sources to obtain target of opportunity observations using
the MeerKAT telescope when these sources are in outburst. The aim is to see if any radio flux density can
be detected from these sources, and to model their spectra using the Van der Laan model, which
assumes that the flux density observed in the spectrum is from a superposition of multiple expanding
synchrotron emitting blobs.