Magnetically-driven protostellar jets transport sufficient angular momentum outward to prevent massive protostars from reaching critical rotation speeds, with jet strength linked to initial formation conditions producing a variety of final stellar rotation rates.
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4 Pith papers cite this work. Polarity classification is still indexing.
4
Pith papers citing it
years
2026 4verdicts
UNVERDICTED 4representative citing papers
Polarization observations reveal scale-dependent differences in magnetic field morphology between molecular clouds and clumps, a velocity-dispersion correlation, and unreliable field-strength estimates that contradict flux conservation.
Simulations indicate SKAO AA4 surveys can trace thermal and nonthermal ISM processes in high-redshift galaxy analogs beyond z=1-3, underscoring nonthermal feedback at cosmic noon.
New observations confirm hourglass magnetic fields at clump scales in G35.20-0.74, with strengths of approximately 600 μG in G35N and 850 μG in G35S, supporting magnetically regulated collapse in G35N and feedback influence in G35S.
citing papers explorer
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On the origin of the rotation of massive stars
Magnetically-driven protostellar jets transport sufficient angular momentum outward to prevent massive protostars from reaching critical rotation speeds, with jet strength linked to initial formation conditions producing a variety of final stellar rotation rates.
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Characterising magnetic fields at the onset of star cluster formation: From giant molecular clouds to infrared dark clumps
Polarization observations reveal scale-dependent differences in magnetic field morphology between molecular clouds and clumps, a velocity-dispersion correlation, and unreliable field-strength estimates that contradict flux conservation.
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Unveiling the roles of thermal and nonthermal processes in the ISM & IGM structure formation and evolution of galaxies with SKAO
Simulations indicate SKAO AA4 surveys can trace thermal and nonthermal ISM processes in high-redshift galaxy analogs beyond z=1-3, underscoring nonthermal feedback at cosmic noon.
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Investigation of Hourglass-shaped Magnetic fields in the G35.20-0.74 Star-Forming Complex
New observations confirm hourglass magnetic fields at clump scales in G35.20-0.74, with strengths of approximately 600 μG in G35N and 850 μG in G35S, supporting magnetically regulated collapse in G35N and feedback influence in G35S.