Transition from super-alfvenic to sub-alfvenic stellar wind flow passing by an exoplanet, using the example of HD 209458b

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Abstract

Depending on the distance of the exoplanet from the central star and on the properties of this star, different regimes of stellar wind flow around it arise. If the exoplanet is at a distance up to the Alfven radius at which the wind speed is equal to the Alfven speed, or the Alfven Mach number MA = 1, then the exoplanet generates Alfven wings. If it is located beyond the Alfven radius, a comet-like magnetosphere appears, like that of the planets of the Solar System. The paper examines how the transition from one flow regime to another can be described on the base of a paraboloid model of the magnetospheric magnetic field using the example of exoplanet HD 209458b.

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About the authors

E. S. Belenkaya

Lomonosov Moscow State University, Skobeltsyn Institute of Nuclear Physics (SINP MSU)

Author for correspondence.
Email: elena@dec1.sinp.msu.ru
Russian Federation, Moscow

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Supplementary files

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2. Fig. 1. Meridional cross section of the day-night magnetosphere of exoplanet HD 209458b. The model parameters are described in the text. The interplanetary magnetic field is represented in the stellar-magnetospheric coordinate system (X, Y, Z) with components {0,0,-90} nTl corresponding to MA > 1

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3. Fig. 2. Same as Fig. 1, but for MMP: {0,0,-1389} nTl, corresponding to MA = 1

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4. Fig. 3. Same as Fig. 1, but for MMPs: {0,0,-13,890} nTl, corresponding to MA < 1

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