3D MHD models of the centrifugal magnetosphere from a massive star with an oblique dipole field

Asif ud-Doula*, Stanley P Owocki*, Christopher Russell, Marc Gagné, Simon Daley-Yates

*Corresponding author for this work

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We present results from new self-consistent 3D MHD simulations of the magnetospheres from massive stars with a dipole magnetic axis that has a non-zero obliquity angle (β) to the star’s rotation axis. As an initial direct application, we compare the global structure of co-rotating disks for nearly aligned (β = 5o) versus half-oblique (β = 45o) models, both with moderately rapid rotation (∼ 0.5 critical). We find that accumulation surfaces broadly resemble the forms predicted by the analytic Rigidly Rotating Magnetosphere (RRM) model, but the mass buildup to near the critical level for centrifugal breakout against magnetic confinement distorts the field from the imposed initial dipole. This leads to an associated warping of the accumulation surface toward the rotational equator, with the highest density concentrated in wings centered on the intersection between the magnetic and rotational equators. These MHD models can be used to synthesize rotational modulation of photometric absorption and H α emission for a direct comparison with observations.
Original languageEnglish
Pages (from-to)3947–3954
Number of pages8
JournalMonthly Notices of the Royal Astronomical Society
Issue number3
Early online date1 Feb 2023
Publication statusPublished - 1 Apr 2023


  • (Magnetohydrodynamics) MHD
  • Stars: winds
  • Outflows
  • Stars: magnetic fields
  • Stars: massive
  • Stars: mass-loss


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