Interacting Fields and Flows: Magnetic Hot Jupiters
arXiv:1711.11282 · doi:10.1002/asna.201713395
Abstract
We present Magnetohydrodynamic (MHD) simulations of the magnetic interactions between a solar type star and short period hot Jupiter exoplanets, using the publicly available MHD code PLUTO. It has been predicted that emission due to magnetic interactions such as the electron cyclotron maser instability (ECMI) will be observable. In our simulations, a planetary outflow, due to UV evaporation of the exoplanets atmosphere, results in the build-up of circumplanetary material. We predict the ECMI emission and determine that the emission is prevented from escaping from the system. This is due to the evaporated material leading to a high plasma frequency in the vicinity of the planet, which inhibits the ECMI process.
Conference proceedings: "14th Potsdam Thinkshop: Stellar Magnetism: Challenges, Connections, and Prospects", Potsdam 2017
References in corpus (19)
- PLUTO: a Numerical Code for Computational Astrophysics
- The PLUTO Code for Adaptive Mesh Computations in Astrophysical Fluid Dynamics
- WASP-12b: The hottest transiting planet yet discovered
- 3D model of hydrogen atmospheric escape from HD209458b and HD189733b: radiative blow-out and stellar wind interactions
- Simulating the escaping atmospheres of hot gas planets in the solar neighborhood
- An evaporating planet in the wind: stellar wind interactions with the radiatively braked exosphere of GJ436 b
- Classification of magnetized star--planet interactions: bow shocks, tails, and inspiraling flows
- Magnetically controlled mass loss from extrasolar planets in close orbits
- A hot Uranus transiting the nearby M dwarf GJ3470. Detected with HARPS velocimetry. Captured in transit with TRAPPIST photometry
- On the environment surrounding close-in exoplanets
- Magnetic games between a planet and its host star: the key role of topology
- Magnetospheric Radio Emission from Extrasolar Giant Planets: The Role of the Host Stars
- Atmosphere Expansion and Mass Loss of Close-Orbit Giant Exoplanets heated by Stellar XUV. II. Effects of Planetary Magnetic Field, Structuring of inner Magnetosphere
- On the diversity of magnetic interactions in close-in star-planet systems
- Stellar wind-magnetosphere interaction at exoplanets: computations of auroral radio powers
- FUV variability of HD 189733. Is the star accreting material from its hot Jupiter?
- How Expanded Ionospheres of Hot Jupiters Can Prevent Escape of Radio Emission Generated by the Cyclotron Maser Instability
- Simulating the Environment Around Planet-Hosting Stars - I. Coronal Structure
- Magnetospheres of hot Jupiters: hydrodynamic models & ultraviolet absorption
Cited by in corpus (7)
- Atmospheric Escape and the Evolution of Close-in Exoplanets
- Stellar Winds Drive Strong Variations in Exoplanet Evaporative Outflows and Transit Absorption Signatures
- Hot Jupiter accretion: 3D MHD simulations of star-planet wind interaction
- Supermassive Hot Jupiters Provide More Favourable Conditions for the Generation of Radio Emission via the Cyclotron Maser Instability - A Case Study Based on Tau Bootis b
- In search of radio emission from exoplanets: GMRT observations of the binary system HD~41004
- Large-scale structures in the stellar wind of fast-rotating stars spawned by the presence of Earth-like planets
- Corotating Interaction Regions (CIRs): evolution over a solar lifetime