Speaker
Description
Using multiple theoretical emission models, the flux density of dwarf novae can be modelled. These sources can emit light from radio frequencies up to x-ray frequencies. Using various theoretical models, we can gain insight on the parameters of these sources. For this study, RU Pegasi, IP Pegasi, and V426 Ophiuchi were selected as they were detected by the MeerKAT telescope during outburst. Following on the work presented at the previous HEASA conference (HEASA2025), the radio fluxes of these sources were modelled using the Van der Laan model, estimating the magnetic field strength, electron energies, number density of the electrons, and the sizes of expanding relativistic blobs. The models show parameters within a reasonable range for the detected radio fluxes. Theoretical models allow us to estimate key details about the source, such as the temperature of the source, the size and temperature of the emitting regions, as well as the magnetic fields contained in these sources. The optical and x-ray emission of Ru Pegasi and V426 Ophiuchi showed good fits for the black body and bremsstrahlung, whereas RU Pegasi only has a decent blackbody fit.