3D Alfvén-wave wind simulations of the Sun and four fast rotators yield a self-consistent mass loss that scales as X-ray flux^0.67 and a braking lever arm that scales as magnetization^0.35.
Angular momentum evolution of young low-mass stars and brown dwarfs: observations and theory
6 Pith papers cite this work. Polarity classification is still indexing.
6
Pith papers citing it
abstract
This chapter aims at providing the most complete review of both the emerging concepts and the latest observational results regarding the angular momentum evolution of young low-mass stars and brown dwarfs. In the time since Protostars & Planets V, there have been major developments in the availability of rotation period measurements at multiple ages and in different star-forming environments that are essential for testing theory. In parallel, substantial theoretical developments have been carried out in the last few years, including the physics of the star-disk interaction, numerical simulations of stellar winds, and the investigation of angular momentum transport processes in stellar interiors. This chapter reviews both the recent observational and theoretical advances that prompted the development of renewed angular momentum evolution models for cool stars and brown dwarfs. While the main observational trends of the rotational history of low mass objects seem to be accounted for by these new models, a number of critical open issues remain that are outlined in this review.
representative citing papers
After bias correction, fast-rotating YSOs have exponentially distributed cold-spot coverages while slow rotators lack small long-lived spots, implying rotation-dependent spot lifetimes.
Simulations show that von Zeipel-Lidov-Kozai migration from inclined companions produces misaligned short-period hot Jupiters while coplanar high-eccentricity migration preserves alignment at longer periods.
Red main-sequence stars in the young LMC clusters NGC 1866 and NGC 1856 rotate at mean equatorial velocities near 300 km/s, about 70-80% of critical, linking rotation to the split main sequences and high Be star fractions.
A spin-spin resonance in binaries can pump the secondary's obliquity to high values as the primary's magnetic braking sweeps the precession frequencies through commensurability.
Retrievals on six isolated brown dwarfs yield near-solar C/O (0.51-0.63), metallicities, and 12C/13C ratios (91-155) supporting molecular cloud fragmentation origin.
citing papers explorer
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High-Resolution Modelling of Coronae and Winds in Solar-type Stars with Varying Rotation Rates II. Stellar Winds
3D Alfvén-wave wind simulations of the Sun and four fast rotators yield a self-consistent mass loss that scales as X-ray flux^0.67 and a braking lever arm that scales as magnetization^0.35.
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A survey for variable young stars with small telescopes - XI. Spot Lifetimes and Coverage Distributions
After bias correction, fast-rotating YSOs have exponentially distributed cold-spot coverages while slow rotators lack small long-lived spots, implying rotation-dependent spot lifetimes.
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Planet-Planet Secular Migration Predicts a Stellar Obliquity-Period Anti-Correlation
Simulations show that von Zeipel-Lidov-Kozai migration from inclined companions produces misaligned short-period hot Jupiters while coplanar high-eccentricity migration preserves alignment at longer periods.
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Tracing stellar rotation in young massive LMC clusters
Red main-sequence stars in the young LMC clusters NGC 1866 and NGC 1856 rotate at mean equatorial velocities near 300 km/s, about 70-80% of critical, linking rotation to the split main sequences and high Be star fractions.
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Spin-spin coupling in stellar binaries
A spin-spin resonance in binaries can pump the secondary's obliquity to high values as the primary's magnetic braking sweeps the precession frequencies through commensurability.
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The ESO SupJup Survey XI. Atmospheric properties of six isolated M- and L-type dwarfs with CRIRES+
Retrievals on six isolated brown dwarfs yield near-solar C/O (0.51-0.63), metallicities, and 12C/13C ratios (91-155) supporting molecular cloud fragmentation origin.