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The particle and magnetic environments surrounding close-in exoplanets

Published online by Cambridge University Press:  09 September 2016

A. A. Vidotto ,
R. Fares ,
M. Jardine ,
C. Moutou  and
J.-F. Donati
A. A. Vidotto
Affiliation:
Université de Genève, Chemin des Maillettes 51, Versoix, CH-1290, Switzerland email: Aline.Vidotto@unige.ch
R. Fares
Affiliation:
INAF, Osservatorio Astrofisico di Catania, Via Santa Sofia, 78, 95123 Catania, Italy
M. Jardine
Affiliation:
SUPA, University of St Andrews, North Haugh, St Andrews, KY16 9SS, UK
C. Moutou
Affiliation:
CFHT, CNRS, 65-1238 Mamalahoa Hwy, Kamuela HI 96743, USA Aix Marseille Université, CNRS, LAM UMR 7326, 13388, Marseille, France
J.-F. Donati
Affiliation:
Université de Toulouse, UPS-OMP, IRAP, 14 avenue E. Belin, Toulouse, F-31400, France CNRS, IRAP / UMR 5277, Toulouse, 14 avenue E. Belin, F-31400, France
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Abstract

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The proper characterisation of stellar winds is essential for the study of propagation of eruptive events (flares, coronal mass ejections) and the study of space weather events on exoplanets. Here, we quantitatively investigate the nature of the stellar winds surrounding the hot Jupiters HD46375b, HD73256b, HD102195b, HD130322b, HD179949b. We simulate the three-dimensional winds of their host stars, in which we directly incorporate their observed surface magnetic fields. With that, we derive the wind properties at the position of the hot-Jupiters’ orbits (temperature, velocity, magnetic field intensity and pressure). We show that the exoplanets studied here are immersed in a local stellar wind that is much denser than the local conditions encountered around the solar system planets (e.g., 5 orders of magnitude denser than the conditions experienced by the Earth). The environment surrounding these exoplanets also differs in terms of dynamics (slower stellar winds, but higher Keplerian velocities) and ambient magnetic fields (2 to 3 orders of magnitude larger than the interplanetary medium surrounding the Earth). The characterisation of the host star's wind is also crucial for the study of how the wind interacts with exoplanets. For example, we compute the exoplanetary radio emission that is released in the wind-exoplanet interaction. For the hot-Jupiters studied here, we find radio fluxes ranging from 0.02 to 0.13 mJy. These fluxes could become orders of magnitude higher when stellar eruptions impact exoplanets, increasing the potential of detecting exoplanetary radio emission.

Keywords

stars: low-massbrown dwarfsstars: magnetic fieldsstars: windsoutflowsinterplanetary mediumplanets and satellites: general
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , Symposium S320: Solar and Stellar Flares and their Effects on Planets , August 2015 , pp. 397 - 402
Copyright
Copyright © International Astronomical Union 2016 

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