Numerical simulation of the Hall effect in magnetized accretion disks with the Pluto code

Nakhaei, Mohammad; Safaei, Ghasem; Abbassi, Shahram

doi:10.1088/1674-4527/14/1/008

Cited by 1 publication

(1 citation statement)

References 28 publications

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“…Hence, we only consider the case of axisymmetric stellar winds in this work. Thanks to PLUTO modular capabilities, such dynamical processes could be studied more accurately by taking into account explicit ohmic, Hall, and eventually ambipolar dissipation (these effects are not included in the public version of PLUTO yet, for first implementations see Lesur et al 2014;Nakhaei et al 2014). These aspects are beyond the scope of the present work and will be explored in future studies.…”

Section: Numericsmentioning

confidence: 99%

Magnetic Games Between a Planet and Its Host Star: The Key Role of Topology

Strugarek

Brun

Matt

et al. 2015

ApJ

105

134

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Magnetic interactions between a star and a close-in planet are postulated to be a source of enhanced emissions and to play a role in the secular evolution of the orbital system. Close-in planets generally orbit in the sub-alfvénic region of the stellar wind, which leads to efficient transfers of energy and angular momentum between the star and the planet. We model the magnetic interactions occurring in close-in star-planet systems with three-dimensional, global, compressible magneto-hydrodynamic numerical simulations of a planet orbiting in a self-consistent stellar wind. We focus on the cases of magnetized planets and explore three representative magnetic configurations. The Poynting flux originating from the magnetic interactions is an energy source for enhanced emissions in star-planet systems. Our results suggest a simple geometrical explanation for ubiquitous on/off enhanced emissions associated with close-in planets, and confirm that the Poynting fluxes can reach powers of the order of 10 19 W. Close-in planets are also showed to migrate due to magnetic torques for sufficiently strong stellar wind magnetic fields. The topology of the interaction significantly modifies the shape of the magnetic obstacle that leads to magnetic torques. As a consequence, the torques can vary by at least an order of magnitude as the magnetic topology of the interaction varies. Subject headings: planets and satellites: dynamical evolution and stability -planet-star interactions -stars: wind, outflows -magnetohydrodynamics (MHD) strugarek@astro.umontreal.ca 1 From the database exoplanet.eu, 01/09/2015.

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Section: Numericsmentioning

confidence: 99%