Searching for star–planet interactions within the magnetosphere of HD 189733

• Published in: Monthly notices of the Royal Astronomical Society Vol. 406; no. 1; pp. 409 - 419
• Main Authors: Fares, R., Donati, J.-F., Moutou, C., Jardine, M. M., Grießmeier, J.-M., Zarka, P., Shkolnik, E. L., Bohlender, D., Catala, C., Cameron, A. C.
• Format: Journal Article
• Language: English
• Published: Oxford, UK Blackwell Publishing Ltd 21-07-2010; Wiley-Blackwell; Oxford University Press
• Subjects: Astronomy; Dwarf stars; Earth, ocean, space; Exact sciences and technology; Magnetic fields; planetary systems; stars: activity; stars: individual: HD 189733; stars: magnetic field; stars: individual: HD 189733; stars: magnetic field; planetary systems; stars: activity; Giant planet; Toroidal field; Orbits; Topology; Planetary system; Radio emission; Magnetic stars; Radio flux; Models; Stellar rotation; Angular velocity; Stellar activity; Magnetic fields; Velocity shear; Stellar coronae
• ISSN: 0035-8711; 1365-2966
• DOI: 10.1111/j.1365-2966.2010.16715.x

HD 189733 is a K2 dwarf, orbited by a giant planet at 8.8 stellar radii. In order to study magnetospheric interactions between the star and the planet, we explore the large-scale magnetic field and activity of the host star. We collected spectra using the ESPaDOnS and the NARVAL spectropolarimeters, installed at the 3.6-m Canada–France–Hawaii telescope and the 2-m Telescope Bernard Lyot at Pic du Midi, during two monitoring campaigns (2007 June and 2008 July). HD 189733 has a mainly toroidal surface magnetic field, having a strength that reaches up to 40 G. The star is differentially rotating, with latitudinal angular velocity shear of dΩ= 0.146 ± 0.049 rad d−1, corresponding to equatorial and polar periods of 11.94 ± 0.16 d and 16.53 ± 2.43 d, respectively. The study of the stellar activity shows that it is modulated mainly by the stellar rotation (rather than by the orbital period or the beat period between the stellar rotation and the orbital periods). We report no clear evidence of magnetospheric interactions between the star and the planet. We also extrapolated the field in the stellar corona and calculated the planetary radio emission expected for HD 189733b, given the reconstructed field topology. The radio flux we predict in the framework of this model is time variable and potentially detectable with LOFAR.