Magnetised exoplanets are expected to emit at radio frequencies analogously to the radio auroral emission of Earth and Jupiter .
Here , we predict the radio emission from V830 Tau b , the youngest ( 2 Myr ) detected exoplanet to date .
We model the wind of its host star using three-dimensional magnetohydrodynamics simulations that take into account the reconstructed stellar surface magnetic field .
Our simulations allow us to constrain the local conditions of the environment surrounding V830 Tau b that we use to then compute its radio emission .
We estimate average radio flux densities of 6 to 24 mJy , depending on the assumption of the radius of the planet ( one or two Jupiter radii ) .
These radio fluxes are not constant along one planetary orbit , and present peaks that are up to twice the average values .
We show here that these fluxes are weakly dependent ( a factor of 1.8 ) on the assumed polar planetary magnetic field ( 10 to 100 G ) , opposed to the maximum frequency of the emission , which ranges from 18 to 240 MHz .
We also estimate the thermal radio emission from the stellar wind .
By comparing our results with the Karl G. Jansky Very Large Array and the Very Long Baseline Array observations of the system , we constrain the stellar mass-loss rate to be \lesssim 3 \times 10 ^ { -9 } ~ { } { M } _ { \odot } ~ { } { yr } ^ { -1 } , with likely values between \sim 10 ^ { -12 } and 10 ^ { -10 } ~ { } { M } _ { \odot } ~ { } { yr } ^ { -1 } .
With these values , we estimate that the frequency-dependent extension of the radio-emitting wind is around \sim 3 to 30 stellar radii ( R _ { \star } ) for frequencies in the range of 275 to 50 MHz , implying that V830 Tau b , at an orbital distance of 6.1 ~ { } R _ { \star } , could be embedded in the regions of the host star ’ s wind that are optically thick to radio wavelengths , but not deeply so .
We also note that planetary emission can only propagate in the stellar wind plasma if the frequency of the cyclotron emission exceeds the stellar wind plasma frequency .
In other words , we find that for planetary radio emission to propagate through the host star wind , planetary magnetic field strengths larger than \sim 1.3 to 13 G are required .
Since our radio emission computations are based on analogies with solar system planets , we caution that our computations should be considered as estimates .
Nevertheless , the V830 Tau system is a very interesting system for conducting radio observations from both the perspective of radio emission from the planet as well as from the host star ’ s wind .