3D SPH simulations show that localized, mildly super-Keplerian equatorial mass ejections with high viscosity reproduce the photometric, spectroscopic, and polarimetric signatures of Be star flicker events.
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Magnetic fields in Be stars reach up to 460 G, much stronger than the under-100 G values reported in earlier studies, based on new spectropolarimetric observations of seven stars.
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The birth of Be star disks III. SPH models of localised mass ejections
3D SPH simulations show that localized, mildly super-Keplerian equatorial mass ejections with high viscosity reproduce the photometric, spectroscopic, and polarimetric signatures of Be star flicker events.
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The magnetic fields in Be stars are stronger than previously suggested
Magnetic fields in Be stars reach up to 460 G, much stronger than the under-100 G values reported in earlier studies, based on new spectropolarimetric observations of seven stars.