Theorists now say that expanded ionospheres of hot Jupiters might self-absorb this emission down to undetectable levels.
...but no significant effect at higher frequencies - where our most sensitive telescopes operate.
The Next-Generation Very Karge Array (ngVLA) is a similar-scale project under consideration in the USA.
The first radio images of the Sun revealed that emission is dominated by active regions (sunspots)
Using 17 GHz maps of the Sun Selhorst et al predicted deep transits across active regions as seen by ALMA.
How well might we do with the SKA?
Using SKA design specifications, we calculate the sensitivity of the SKA to transits around solar-like stars (using VLA fluxes of ε Eridani and the MWA SED of the Sun) and M dwarfs (scaled from LHS 3003), we predict the sensitivity of the SKA to transits.
... and broadband strong lensing from refraction through its mean density profile.
As we can see, it is very challenging to detect solar-like stars at more than a few parsecs, let alone their transits.
Transits across active M dwarfs, on the other hand, can be seen at SKA-Mid frequencies out to tens of parsecs! Gaia indicates there are many hundreds out to this distance, most undetected so far in radio.
I argue that modulation of the amplitude of this variability on an optically-determined exoplanet ephemeris will nevertheless be a strong signal.
Low frequency emission is at present poorly constrained - LOFAR will test for SKA-Low..
LOFAR will probe the M dwarf population at low frequencies - how bright are they?
Can we predict their light curves better?
What else might the SKA do for exoplanets?