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dc.contributor.authorVidotto, Aline
dc.contributor.authorFares, Rim
dc.contributor.authorJardine, Moira Mary
dc.contributor.authorMoutou, C.
dc.contributor.authorDonati, J.-F.
dc.identifier.citationVidotto , A , Fares , R , Jardine , M M , Moutou , C & Donati , J-F 2015 , ' On the environment surrounding close-in exoplanets ' , Monthly Notices of the Royal Astronomical Society , vol. 449 , no. 4 , pp. 4117-4130 .
dc.identifier.otherBibCode: 2015MNRAS.449.4117V
dc.identifier.otherORCID: /0000-0002-1466-5236/work/57821803
dc.descriptionAAV acknowledges support from the Swiss National Science Foundation through an Ambizione Fellowship. RF acknowledges support from a STFC grant. Date of Acceptance: 17/03/2015en
dc.description.abstractExoplanets in extremely close-in orbits are immersed in a local interplanetary medium (i.e. the stellar wind) much denser than the local conditions encountered around the Solar system planets. The environment surrounding these exoplanets also differs in terms of dynamics (slower stellar winds, but higher Keplerian velocities) and ambient magnetic fields (likely higher for host stars more active than the Sun). Here, we quantitatively investigate the nature of the interplanetary media surrounding the hot Jupiters HD 46375b, HD 73256b, HD 102195b, HD 130322b and HD 179949b. We simulate the three-dimensional winds of their host stars, in which we directly incorporate their observed surface magnetic fields. With that, we derive mass-loss rates (1.9–8.0 × 10−13 M⊙ yr−1) and the wind properties at the position of the hot Jupiters’ orbits (temperature, velocity, magnetic field intensity and pressure). We show that these exoplanets’ orbits are supermagnetosonic, indicating that bow shocks are formed surrounding these planets. Assuming planetary magnetic fields similar to Jupiter's, we estimate planetary magnetospheric sizes of 4.1–5.6 planetary radii. We also derive the exoplanetary radio emission released in the dissipation of the stellar wind energy. We find radio fluxes ranging from 0.02 to 0.13 mJy, which are challenging to be observed with present-day technology, but could be detectable with future higher sensitivity arrays (e.g. Square Kilometre Array). Radio emission from systems having closer hot Jupiters, such as from τ Boo b or HD 189733b, or from nearby planetary systems orbiting young stars, are likely to have higher radio fluxes, presenting better prospects for detecting exoplanetary radio emission.
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.subjectMethods: numericalen
dc.subjectStars: magnetic fielden
dc.subjectPlanetary systemsen
dc.subjectStars: windsen
dc.subjectQC Physicsen
dc.subjectQB Astronomyen
dc.titleOn the environment surrounding close-in exoplanetsen
dc.typeJournal articleen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.description.statusPeer revieweden

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