Misaligned protostellar cores produce a spiral flow outflow in addition to the disk wind, with the spiral flow becoming dominant and more massive at misalignment angles of 60 degrees or greater.
Frontiers 45 Teyssier & Commerc ¸ on Numerical Methods in Star Formation Vaytet N, Commerc ¸on B, Masson J, Gonz´alez M, Chabrier G
4 Pith papers cite this work, alongside 187 external citations. Polarity classification is still indexing.
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MHD collapse simulations define an Envelope-Disk Transition Zone (ENDTRANZ) where a jump in the j-r profile occurs due to positive gravitational torques, with a corresponding jump detected in ALMA observations of L1527 IRS.
Dedner's mixed divergence cleaning produces substantial artifacts for strongly localized magnetic fields or sudden timestep changes; constrained transport is more accurate, and some prior early-Universe amplification claims may be affected.
Review of MHD numerical methods for star formation, covering discretization techniques, divergence-free constraints, sink particles, and non-ideal effects like diffusion and the Hall effect.
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Multiple protostellar outflows from a single protostar with a misaligned disk
Misaligned protostellar cores produce a spiral flow outflow in addition to the disk wind, with the spiral flow becoming dominant and more massive at misalignment angles of 60 degrees or greater.
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Modelling the Break in the Specific Angular Momentum within the Envelope-Disk Transition Zone
MHD collapse simulations define an Envelope-Disk Transition Zone (ENDTRANZ) where a jump in the j-r profile occurs due to positive gravitational torques, with a corresponding jump detected in ALMA observations of L1527 IRS.
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Systematic Comparison between Constrained Transport and Mixed Divergence Cleaning Methods for Astrophysical Magnetohydrodynamic Simulations
Dedner's mixed divergence cleaning produces substantial artifacts for strongly localized magnetic fields or sudden timestep changes; constrained transport is more accurate, and some prior early-Universe amplification claims may be affected.
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Numerical Methods for Simulating Star Formation
Review of MHD numerical methods for star formation, covering discretization techniques, divergence-free constraints, sink particles, and non-ideal effects like diffusion and the Hall effect.