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Tuning in to the radio environment of HD189733b

Published online by Cambridge University Press:  24 September 2020

R. D. Kavanagh Open the ORCID record for R. D. Kavanagh [Opens in a new window] ,
A. A. Vidotto Open the ORCID record for A. A. Vidotto [Opens in a new window] ,
D. Ó Fionnagáin Open the ORCID record for D. Ó Fionnagáin [Opens in a new window] ,
V. Bourrier ,
R. Fares ,
M. Jardine Open the ORCID record for M. Jardine [Opens in a new window] ,
Ch. Helling ,
C. Moutou ,
J. Llama Open the ORCID record for J. Llama [Opens in a new window]  and
P. J. Wheatley
R. D. Kavanagh
Affiliation:
School of Physics, Trinity College Dublin, The University of Dublin, Dublin 2, Ireland email: mailto:[email protected]
A. A. Vidotto
Affiliation:
School of Physics, Trinity College Dublin, The University of Dublin, Dublin 2, Ireland email: mailto:[email protected]
D. Ó Fionnagáin
Affiliation:
School of Physics, Trinity College Dublin, The University of Dublin, Dublin 2, Ireland email: mailto:[email protected]
V. Bourrier
Affiliation:
Observatoire de l'Université de Genéve, Chemin des Maillettes 51, Versoix, CH-1290, Switzerland
R. Fares
Affiliation:
Physics Department, United Arab Emirates University, P.O. Box 15551, Al-Ain, United Arab Emirates University of Southern Queensland, Centre for Astrophysics, Toowoomba, Queensland, 4350, Australia
M. Jardine
Affiliation:
SUPA, School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews, Fife, Scotland, KY16 9SS
Ch. Helling
Affiliation:
Centre for Exoplanet Science, University of St Andrews, St Andrews KY16 9SS, UK
C. Moutou
Affiliation:
CNRS/CFHT, 65-1238 Mamalahoa Highway, Kamuela HI 96743, USA
J. Llama
Affiliation:
Lowell Observatory, 1400 W. Mars Hill Rd, Flagstaff. AZ 86001. USA
P. J. Wheatley
Affiliation:
Department of Physics, University of Warwick, Coventry CV4 7AL, UK
Rights & Permissions [Opens in a new window]

Abstract

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The hot Jupiter HD189733b is expected to be a source of strong radio emission, due to its close proximity to its magnetically active host star. Here, we model the stellar wind of its host star, based on reconstructed surface stellar magnetic field maps. We use the local stellar wind properties at the planetary orbit obtained from our models to compute the expected radio emission from the planet. Our findings show that the planet emits with a peak flux density within the detection capabilities of LOFAR. However, due to absorption by the stellar wind itself, this emission may be attenuated significantly. We show that the best time to observe the system is when the planet is near primary transit of the host star, as the attenuation from the stellar wind is lowest in this region.

Keywords

stars: individual (HD189733)stars: magnetic fieldsstars: winds, outflowsstars: planetary systems
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 15 , Symposium S354: Solar and Stellar Magnetic Fields: Origins and Manifestations , June 2019 , pp. 305 - 309
Copyright
© International Astronomical Union 2020

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