  AE Aqr was until recently the only known magnetic cataclysmic variable (MCV)
containing a rapidly spinning (33.08 s) white dwarf (WD). Its radio emission is
believed to be a superposition of synchrotron emitting plasmoids, because it
has a positive spectral index spanning three orders of magnitude (~2-2000 GHz)
and is unpolarized. Both characteristics are unusual for MCVs. Recently,
Thorstensen has suggested that the cataclysmic variable LAMOST
J024048.51+195226.9 (henceforth, J0240+19) is a twin of AE Aqr based on its
optical spectra. Optical photometry shows the star to be a high-inclination,
eclipsing binary with a spin period of 24.93 s, making it the fastest spinning
WD. This paper presents three hours of Very Large Array radio observations of
J0240+19. These observations show that the persistent radio emission from
J0240+19 is dissimilar to that of AE Aqr in that it shows high circular
polarization and a negative spectral index. The emission is most similar to the
nova-like CV V603 Aql. We argue that the radio emission is caused by a
superposition of plasmoids emitting plasma radiation or electron cyclotron
maser emission from the lower corona of the donor star and not from the
magnetosphere near the WD, because the latter site is expected to be modulated
at the orbital period of the binary and to show eclipses of which there is no
evidence. The radio source J0240+19, although weak (<1 mJy), is a persistent
source in a high-inclination eclipsing binary, making it a good laboratory for
studying radio emission from CVs.

Solar and Stellar Astrophysics;High Energy Astrophysical Phenomena