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Numerical Simulations Of The Interaction Between The Stellar Magnetic Field And A Planet

Numerical Simulations Of The Interaction Between The Stellar Magnetic Field And A Planet

Exoplanetology: Exoplanets & Exomoons

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astro-ph.EP

April 15, 2025

Numerical Simulations Of The Interaction Between The Stellar Magnetic Field And A Planet — Current density (J⃗ = ∇ × B/ ⃗ (4π)) streamlines for an initial magnetic field B0 = 0.1 (the magnetic field streamlines corresponding to the same simulation are shown in the upper panel of Figure 2). The computational box is rotated as shown in the coordinate axes on the left. The color scale corresponds to the intensity of the current density, from blue (lower) to red (larger current density). As the magnetic field is nearly vertical, the current density is nearly zero on the left of the computational box (with respect to the x axis). Downstream (with respect to the planet position), the current density streamlines form a complex structure, with cavities (with low current density) which start from the position of the planet and extend towards larger values of y and z (see upper right panel). The projection of the current density along the x − y plane forms a structure which resembles the one obtained in analytical models (Figure 4). — astro-ph.EP

Kepler and TESS observations led to the discovery of many close-in super Earths, including some with ultra-short orbital periods (≲1 day).

During and shortly after their multi-Myr formation epoch, their GKM host stars generally have kilogauss magnetic fields which can exert torques on the orbits of nearby super- Earths.

In this work, we examine one aspect of this interaction: the magnetic torque resulting from Alfvén-wing drag on non-corotating, non-magnetized planets engulfed by the host stars’ stellar wind.

We compute the magnitude of this torque for a range of stellar magnetic field strengths, and planetary orbital velocities.

We also model the planets’ orbital evolution, taking into account for stellar spin down and magnetic field decay, and derive the boundaries within which ultra-short-period super-Earths can survive.

Fabio De Colle, Douglas N.C. Lin, Chen Chen, Gongjie Li

Comments: 15 pages, 11 figures, submitted to MNRAS
Subjects: Earth and Planetary Astrophysics (astro-ph.EP); Solar and Stellar Astrophysics (astro-ph.SR)
Cite as: arXiv:2504.09390 [astro-ph.EP] (or arXiv:2504.09390v1 [astro-ph.EP] for this version)
https://doi.org/10.48550/arXiv.2504.09390
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Submission history
From: Fabio De Colle
[v1] Sun, 13 Apr 2025 00:53:19 UTC (1,733 KB)
https://arxiv.org/abs/2504.09390

Astrobiology,

Explorers Club Fellow, ex-NASA Space Station Payload manager/space biologist, Away Teams, Journalist, Lapsed climber, Synaesthete, Na’Vi-Jedi-Freman-Buddhist-mix, ASL, Devon Island and Everest Base Camp veteran, (he/him) 🖖🏻

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