The 20th (and a half) Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun
Published April 29, 2021 | Version v1
Conference paper Open

Planet-induced radio emission from the coronae of M dwarfs

Authors/Creators

  • 1. Trinity College Dublin
  • 2. University of Oxford
  • 3. University of St Andrews
  • 4. Université de Toulouse
  • 5. National University of Ireland, Galway

Contributors

Editor:

Description

There have recently been detections of radio emission from low-mass stars, some of which are indicative of star-planet interactions. Motivated by these exciting new results, here we present stellar wind models for the active planet-hosting M dwarf AU Mic. Our models incorporate the large-scale photospheric magnetic field map of the star, reconstructed using the Zeeman-Doppler Imaging method. We use our models to assess if planet-induced radio emission could be generated in the corona of AU Mic, through a mechanism analogous to the sub-Alfvénic Jupiter-Io interaction. In the case that AU Mic has a mass-loss rate of 27 times that of the Sun, we find that both planets b and c in the system can induce radio emission from 10 MHz to 3 GHz in the corona of the host star for the majority of their orbits, with peak flux densities of 10 mJy. Our predicted emission bears a striking similarity to that recently reported from GJ 1151 by Vedantham et al. (2020), which is indicative of being induced by a planet. Detection of such radio emission would allow us to place an upper limit on the mass-loss rate of the star.

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Identifiers

arXiv
arXiv:2104.14457

References

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