Surface magnetic fields predict solar cycles when poloidal flux is efficiently transported back into the dynamo or when the surface field represents the radial component of the interior poloidal field.
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Stellar magnetic cycle variability decreases with faster rotation and higher dynamo number, shown by positive correlation with rotation period and negative correlations with Ro^{-2} and cycle-to-rotation ratio in Mount Wilson data and models.
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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Understanding mechanisms underlying solar cycle predictability with a general framework
Surface magnetic fields predict solar cycles when poloidal flux is efficiently transported back into the dynamo or when the surface field represents the radial component of the interior poloidal field.
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Stellar cycle variability in Mount Wilson stars and dynamo models: Rotation rate and dynamo number dependency
Stellar magnetic cycle variability decreases with faster rotation and higher dynamo number, shown by positive correlation with rotation period and negative correlations with Ro^{-2} and cycle-to-rotation ratio in Mount Wilson data and models.
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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.