ﻻ يوجد ملخص باللغة العربية
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, in this paper we present Alfven wave-driven stellar wind models of the two active planet-hosting M dwarfs Prox Cen and AU Mic. Our models incorporate large-scale photospheric magnetic field maps reconstructed using the Zeeman-Doppler Imaging method. We obtain a mass-loss rate of $0.25~dot{M}_{odot}$ for the wind of Prox Cen. For the young dwarf AU Mic, we explore two cases: a low and high mass-loss rate. Depending on the properties of the Alfven waves which heat the corona in our wind models, we obtain mass-loss rates of $27$ and $590~dot{M}_{odot}$ for AU Mic. We use our stellar wind models to assess the generation of electron cyclotron maser instability emission in both systems, through a mechanism analogous to the sub-Alfvenic Jupiter-Io interaction. For Prox Cen we do not find any feasible scenario where the planet can induce radio emission in the stars corona, as the planet orbits too far from the star in the super-Alfvenic regime. However, in the case that AU Mic has a stellar wind mass-loss rate of $27~dot{M}_{odot}$, we find that both planets b and c in the system can induce radio emission from $sim10$ MHz to 3 GHz in the corona of the host star for the majority of their orbits, with peak flux densities of $sim10$ mJy. 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
AU Mic is a young, very active M dwarf star with a debris disk and at least one transiting Neptune-size planet. Here we present detailed analysis of the magnetic field of AU Mic based on previously unpublished high-resolution optical and near-infrare
We consider the magnetic interaction of exoplanets orbiting M-dwarfs, calculating the expected Poynting flux carried upstream along Alfv{e}n wings to the central star. A region of emission analogous to the Io footprint observed in Jupiters aurora is
We present imaging observations at 1.3 millimeters of the debris disk surrounding the nearby M-type flare star AU Mic with beam size 3 arcsec (30 AU) from the Submillimeter Array. These data reveal a belt of thermal dust emission surrounding the star
M dwarf stars are excellent candidates around which to search for exoplanets, including temperate, Earth-sized planets. To evaluate the photochemistry of the planetary atmosphere, it is essential to characterize the UV spectral energy distribution of