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Resistive MHD simulations of stellar wind–magnetosphere coupling in TRAPPIST-1e.

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Τίτλος: Resistive MHD simulations of stellar wind–magnetosphere coupling in TRAPPIST-1e.
Συγγραφείς: González-Avilés, J J1 (AUTHOR), Pérez-Negrón, N Baltazar1 (AUTHOR), Segura, A2 (AUTHOR)
Πηγή: Monthly Notices of the Royal Astronomical Society. Jun2026, Vol. 549 Issue 1, p1-11. 11p.
Θεματικοί όροι: *TRAPPIST-1, *Magnetosphere, *Stellar winds, *Magnetohydrodynamics, *Geomagnetism, *Magnetic permeability
Περίληψη: Close-in terrestrial exoplanets around M dwarfs reside in dense, magnetized winds, where non-ideal plasma coupling can strongly affect how electromagnetic energy is redistributed within the dayside interaction region. We present three-dimensional resistive magnetohydrodynamic simulations of the TRAPPIST-1 wind interacting with a dipolar TRAPPIST-1e magnetosphere for three stellar-wind forcing cases and four prescribed magnetic diffusivities, η = (0 , 538.018 , 5.380 18 × 10 8 , 5.380 18 × 10 12) cm2 s−1. Energy transport is diagnosed using maps of the total energy density, the magnitude of the total Poynting flux, and the divergence of the total Poynting flux. We further estimate a radio-power proxy from the volume integral of ∇ ⋅ S t o t a l over the dayside bow-shock and magnetopause layers. Across all cases, increasing prescribed η broadens the coupling layer and shifts the dominant energy-conversion regions from thin, patchy boundary arcs to thicker, more spatially extended structures, with an increasing relative contribution from the magnetopause. The inferred radio-power proxy increases by several orders of magnitude across the explored scan. However, because the estimated numerical magnetic diffusivity in the strongest gradient regions is η n u m ∼ 10 15 – 10 16 cm 2 s − 1 ⁠ , the present η scan is best interpreted as a controlled sensitivity study rather than as a direct constraint on the physical diffusivity of the TRAPPIST-1e environment. For the adopted planetary fields (⁠ B e q = 0.32 –1.28 G), the maximum cyclotron frequencies are ν c , max ≈ 1.8 –7.2 MHz, below the ground-based window, implying that meaningful radio constraints on TRAPPIST-1e magnetism will require space-based observations below 10 MHz or substantially stronger planetary fields than those assumed here. [ABSTRACT FROM AUTHOR]
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  Data: Resistive MHD simulations of stellar wind–magnetosphere coupling in TRAPPIST-1e.
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  Data: <searchLink fieldCode="JN" term="%22Monthly+Notices+of+the+Royal+Astronomical+Society%22">Monthly Notices of the Royal Astronomical Society</searchLink>. Jun2026, Vol. 549 Issue 1, p1-11. 11p.
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– Name: Abstract
  Label: Abstract
  Group: Ab
  Data: Close-in terrestrial exoplanets around M dwarfs reside in dense, magnetized winds, where non-ideal plasma coupling can strongly affect how electromagnetic energy is redistributed within the dayside interaction region. We present three-dimensional resistive magnetohydrodynamic simulations of the TRAPPIST-1 wind interacting with a dipolar TRAPPIST-1e magnetosphere for three stellar-wind forcing cases and four prescribed magnetic diffusivities, η = (0 , 538.018 , 5.380 18 × 10 8 , 5.380 18 × 10 12) cm2 s−1. Energy transport is diagnosed using maps of the total energy density, the magnitude of the total Poynting flux, and the divergence of the total Poynting flux. We further estimate a radio-power proxy from the volume integral of ∇ ⋅ S t o t a l over the dayside bow-shock and magnetopause layers. Across all cases, increasing prescribed η broadens the coupling layer and shifts the dominant energy-conversion regions from thin, patchy boundary arcs to thicker, more spatially extended structures, with an increasing relative contribution from the magnetopause. The inferred radio-power proxy increases by several orders of magnitude across the explored scan. However, because the estimated numerical magnetic diffusivity in the strongest gradient regions is η n u m ∼ 10 15 – 10 16 cm 2 s − 1 ⁠ , the present η scan is best interpreted as a controlled sensitivity study rather than as a direct constraint on the physical diffusivity of the TRAPPIST-1e environment. For the adopted planetary fields (⁠ B e q = 0.32 –1.28 G), the maximum cyclotron frequencies are ν c , max ≈ 1.8 –7.2 MHz, below the ground-based window, implying that meaningful radio constraints on TRAPPIST-1e magnetism will require space-based observations below 10 MHz or substantially stronger planetary fields than those assumed here. [ABSTRACT FROM AUTHOR]
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RecordInfo BibRecord:
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        Value: 10.1093/mnras/stag638
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      – Code: eng
        Text: English
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        PageCount: 11
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      – SubjectFull: TRAPPIST-1
        Type: general
      – SubjectFull: Magnetosphere
        Type: general
      – SubjectFull: Stellar winds
        Type: general
      – SubjectFull: Magnetohydrodynamics
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      – SubjectFull: Geomagnetism
        Type: general
      – SubjectFull: Magnetic permeability
        Type: general
    Titles:
      – TitleFull: Resistive MHD simulations of stellar wind–magnetosphere coupling in TRAPPIST-1e.
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              M: 06
              Text: Jun2026
              Type: published
              Y: 2026
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