PIMMS extends ZDI by adding a pulsation velocity map to reconstruct surface brightness, magnetic field, and velocity from spectropolarimetric data, with numerical tests showing accurate recovery on simulated pulsating hot stars.
F., Semel, M., Carter, B
2 Pith papers cite this work. Polarity classification is still indexing.
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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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PIMMS: Pulsation-Informed Magnetic Mapping of Stars with Zeeman-Doppler Imaging I. Formalism and numerical tests
PIMMS extends ZDI by adding a pulsation velocity map to reconstruct surface brightness, magnetic field, and velocity from spectropolarimetric data, with numerical tests showing accurate recovery on simulated pulsating hot stars.
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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.