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|Title:||Stellar wind-magnetosphere interaction at exoplanets: Computations of auroral radio powers|
|Authors:||Nichols, J. D.|
Milan, S. E.
|Publisher:||Oxford University Press (OUP), Royal Astronomical Society|
|Citation:||Monthly Notices of the Royal Astronomical Society, 461, 2353–2366 (2016)|
|Abstract:||We present calculations of the auroral radio powers expected from exoplanets with magnetospheresdriven by an Earth-like magnetospheric interaction with the solar wind. Specifically,we compute the twin cell-vortical ionospheric flows, currents, and resulting radio powers resultingfrom a Dungey cycle process driven by dayside and nightside magnetic reconnection,as a function of planetary orbital distance and magnetic field strength.We include saturation ofthe magnetospheric convection, as observed at the terrestrial magnetosphere, and we presentpower-law approximations for the convection potentials, radio powers and spectral flux densities.We specifically consider a solar-age system and a young (1 Gyr) system. We showthat the radio power increases with magnetic field strength for magnetospheres with saturatedconvection potential, and broadly decreases with increasing orbital distance.We show that themagnetospheric convection at hot Jupiters will be saturated, and thus unable to dissipate thefull available incident Poynting flux, such that the magnetic Radiometric Bode's Law (RBL)presents a substantial overestimation of the radio powers for hot Jupiters. Our radio powersfor hot Jupiters are ∼5-1300 TW for hot Jupiters with field strengths of 0.1-10 BJ orbitinga Sun-like star, while we find that competing effects yield essentially identical powers forhot Jupiters orbiting a young Sun-like star. However, in particular, for planets with weakermagnetic fields, our powers are higher at larger orbital distances than given by the RBL, andthere are many configurations of planet that are expected to be detectable using SKA.|
|Rights:||© The Authors 2016. Published by Oxford University Press on behalf of The Royal Astronomical Society. This is an Open Access article distributed under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited.|
|Appears in Collections:||Published Articles, Dept. of Physics and Astronomy|
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