Non-thermal emission from the interaction of magnetized exoplanets with the wind of their host star. (arXiv:1902.05165v1 [astro-ph.EP])
<a href="http://arxiv.org/find/astro-ph/1/au:+Wang_X/0/1/0/all/0/1">Xiawei Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Loeb_A/0/1/0/all/0/1">Abraham Loeb</a>

We study the non-thermal emission from the interaction between magnetized
Jupiter-like exoplanets and the wind from their host star. The supersonic
motion of planets through the wind forms a bow shock that accelerates electrons
which produces non-thermal radiation across a broad wavelength range. We
discuss three wind mass loss rates: $dot{M}_{rm w}sim10^{-14}$, $10^{-9}$,
$10^{-6},M_{odot},rm yr^{-1}$ corresponding to solar-type, T Tauri and
massive O/B type stars, respectively. We find that the expected radio
synchrotron emission from a Jupiter-like planet is detectable by the Jansky
Very Large Array and the Square Kilometer Array at ~1-10 GHz out to a distance
~ 100 pc, whereas the infrared emission is detectable by the James Webb Space
Telescope out to a similar distance. Inverse Compton scattering of the stellar
radiation results in X-ray emission detectable by Chandra X-ray Observatory out
to ~ 150 pc. Finally, we apply our model to the upper limit constraints on V380
Tau, the first star-hot Jupiter system observed in radio wavelength. Our bow
shock model provides constraints on the magnetic field, the interplanetary
medium and the non-thermal emission efficiency in V380 Tau.

We study the non-thermal emission from the interaction between magnetized
Jupiter-like exoplanets and the wind from their host star. The supersonic
motion of planets through the wind forms a bow shock that accelerates electrons
which produces non-thermal radiation across a broad wavelength range. We
discuss three wind mass loss rates: $dot{M}_{rm w}sim10^{-14}$, $10^{-9}$,
$10^{-6},M_{odot},rm yr^{-1}$ corresponding to solar-type, T Tauri and
massive O/B type stars, respectively. We find that the expected radio
synchrotron emission from a Jupiter-like planet is detectable by the Jansky
Very Large Array and the Square Kilometer Array at ~1-10 GHz out to a distance
~ 100 pc, whereas the infrared emission is detectable by the James Webb Space
Telescope out to a similar distance. Inverse Compton scattering of the stellar
radiation results in X-ray emission detectable by Chandra X-ray Observatory out
to ~ 150 pc. Finally, we apply our model to the upper limit constraints on V380
Tau, the first star-hot Jupiter system observed in radio wavelength. Our bow
shock model provides constraints on the magnetic field, the interplanetary
medium and the non-thermal emission efficiency in V380 Tau.

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