The old subgiant 31 Aql exhibits a strong non-cycling magnetic field and revived wind braking torque consistent with a shift to anti-solar differential rotation.
Title resolution pending
4 Pith papers cite this work. Polarity classification is still indexing.
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Pith papers citing it
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astro-ph.SR 4representative citing papers
MIST provides a new publicly available grid of solar-scaled stellar isochrones and evolutionary tracks computed self-consistently with MESA from pre-main sequence through advanced stages for masses 0.1-300 solar masses and metallicities -2 to 0.5.
Direct inclusion of CMFGEN atmosphere grids in STAREVOL evolution calculations lowers effective temperature and radius in the Wolf-Rayet phase to better match observations while leaving internal structure and chemical evolution unchanged.
A joint convective coupling index shows moderate, age-dependent correlation with rotation periods of solar-mass stars, stronger in younger objects and weaker later.
citing papers explorer
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Anti-Solar Differential Rotation May Have Revived Magnetic Braking in the Subgiant 31 Aquilae
The old subgiant 31 Aql exhibits a strong non-cycling magnetic field and revived wind braking torque consistent with a shift to anti-solar differential rotation.
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MESA Isochrones and Stellar Tracks (MIST). I: Solar-Scaled Models
MIST provides a new publicly available grid of solar-scaled stellar isochrones and evolutionary tracks computed self-consistently with MESA from pre-main sequence through advanced stages for masses 0.1-300 solar masses and metallicities -2 to 0.5.
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Wolf-Rayet stellar evolution models with improved treatment of the atmosphere
Direct inclusion of CMFGEN atmosphere grids in STAREVOL evolution calculations lowers effective temperature and radius in the Wolf-Rayet phase to better match observations while leaving internal structure and chemical evolution unchanged.
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How plasma coupling and convective-zone depth shape the rotation of solar-mass stars
A joint convective coupling index shows moderate, age-dependent correlation with rotation periods of solar-mass stars, stronger in younger objects and weaker later.