  When planet-hosting stars evolve off the main sequence and go through the
red-giant branch, the stars become orders of magnitudes more luminous and, at
the same time, lose mass at much higher rates than their main-sequence
counterparts. Accordingly, if planetary companions exist around these stars at
orbital distances of a few AU, they will be heated up to the level of canonical
hot Jupiters and also be subjected to a dense stellar wind. Given that
magnetized planets interacting with stellar winds emit radio waves, such
"Red-Giant Hot Jupiters" (RGHJs) may also be candidate radio emitters. We
estimate the spectral auroral radio intensity of RGHJs based on the empirical
relation with the stellar wind as well as a proposed scaling for planetary
magnetic fields. RGHJs might be intrinsically as bright as or brighter than
canonical hot Jupiters and about 100 times brighter than equivalent objects
around main-sequence stars. We examine the capabilities of low-frequency radio
observatories to detect this emission and find that the signal from an RGHJ may
be detectable at distances up to a few hundred parsecs with the Square
Kilometer Array.
