Planet-induced radio emission from the coronae of M dwarfs. (arXiv:2104.14457v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Kavanagh_R/0/1/0/all/0/1">Robert D. Kavanagh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vidotto_A/0/1/0/all/0/1">Aline A. Vidotto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Klein_B/0/1/0/all/0/1">Baptiste Klein</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jardine_M/0/1/0/all/0/1">Moira M. Jardine</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Donati_J/0/1/0/all/0/1">Jean-François Donati</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fionnagain_D/0/1/0/all/0/1">Dúalta Ó Fionnagáin</a>
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-Alfv’enic 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.
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-Alfv’enic 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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