Searching for star-planet interactions in GJ 486 at radio wavelengths with the uGMRT

We did not detect any quiescent radio emission in any epoch above 3 σ . Similarly, we did not detect any bursty emission in our dynamic spectra. Conclusions.

While we cannot completely rule out that the absence of a radio detection is due to time variability of the radio emission or to the maximum electron-cyclotron maser emission being below our observing range, these cases seem unlikely. We discuss two possible scenarios: an intrinsic dim radio signal and, alternatively, a situation where the anisotropic beamed emission is pointed away from the observer. If the non-detection of radio emission from the star-planet interaction in GJ 486 is due to an intrinsically dim signal, this implies that independent of whether the planet is magnetized or not, the mass-loss rate is small ( Ṁ ⋆ ≲ 0.3 Ṁ ⊙ ) and that, concomitantly, the efficiency of the conversion of the Poynting flux into radio emission must be low ( β ≲ 10 −3 ).

Free-free absorption effects are negligible, given the high value of the coronal temperature. Finally, if the anisotropic beaming pointed away from the observer, this would imply that GJ 486 has very low values of magnetic obliquity and inclination.