Identify an acceptable emission model for V1723 Sco

Determine which emission model adequately describes the 887.5 MHz radio light curve of the classical nova V1723 Sco, for which the thermal, standard synchrotron, and broken-power-law modified synchrotron models all fail to provide an acceptable fit.

Background

The paper models the ASKAP VAST 887.5 MHz radio light curve of V1723 Sco using thermal free-free emission, standard synchrotron emission, and a modified synchrotron model incorporating a broken power-law density profile. Although the modified model reproduces the steep temporal evolution better than the alternatives, its reduced chi-squared remains unsatisfactory, so the observations do not establish a preferred physical emission model.

Resolving this problem would require a model capable of accounting for the rapid rise, short-lived peak, and steep decline of V1723 Sco's radio flare, potentially using multi-frequency observations, improved distance constraints, and more physically realistic shock and ejecta geometries.