The Mass-Dependence of Angular Momentum Evolution in Sun-Like Stars

Matt, Sean P.; Brun, Allan Sacha; Baraffe, I.; Bouvier, J.; Chabrier, G.

doi:10.1088/2041-8205/799/2/l23

Cited by 310 publications

(496 citation statements)

References 50 publications

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“…Of these stars, 90.7% are younger than 4 Gyr, in good agreement with Matt et al (2015) estimating ∼95% comparing the sample from McQuillan et al (2014) to model predictions. Less than 0.62% of the derived ages are greater than 10 Gyr, and less than 2.2% of the B07 stars lie in the critical calibration region younger than 100 Myr, providing some confidence in the derived age distribution.…”

Section: Stellar Ages 431 Gyrochronologysupporting

confidence: 68%

Rotation, differential rotation, and gyrochronology of activeKeplerstars

Reinhold

Gizon

2015

A&A

182

170

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Context. In addition to the discovery of hundreds of exoplanets, the high-precision photometry from the CoRoT and Kepler satellites has led to measurements of surface rotation periods for tens of thousands of stars, which can potentially be used to infer stellar ages via gyrochronology. Aims. Our main goal is to derive ages of thousands of field stars using consistent rotation period measurements derived by different methods. Multiple rotation periods are interpreted as surface differential rotation (DR). We study the dependence of DR with rotation period and effective temperature. Methods. We reanalyze a previously studied sample of 24 124 Kepler stars using different approaches based on the Lomb-Scargle periodogram. Each quarter (Q1-Q14) is treated individually using a prewhitening approach. Additionally, the full time series and their different segments are analyzed. Results. For more than 18 500 stars our results are consistent with the rotation periods from McQuillan et al. (2014, ApJS, 211, 24). Of these, more than 12 300 stars show multiple significant peaks, which we interpret as DR. Dependencies of the DR with rotation period and effective temperature could be confirmed, e.g., the relative DR increases with rotation period. Gyrochronology ages between 100 Myr and 10 Gyr were derived for more than 17 000 stars using different gyrochronology relations, most of them with uncertainties dominated by period variations. We find a bimodal age distribution for T eff between 3200-4700 K. The derived ages reveal an empirical activity-age relation using photometric variability as stellar activity proxy. Additionally, we found 1079 stars with extremely stable (mostly short) periods. Half of these periods may be associated with rotation stabilized by non-eclipsing companions, the other half might be due to pulsations. Conclusions. The derived gyrochronology ages are well constrained since more than ∼93.0% of the stars seem to be younger than the Sun where calibration is most reliable. Explaining the bimodality in the age distribution is challenging, and limits accurate stellar age predictions. The relation between activity and age is interesting, and requires further investigation. The existence of cool stars with almost constant rotation period over more than three years of observation might be explained by synchronization with stellar companions, or a dynamo mechanism keeping the spot configurations extremely stable.

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Section: Stellar Ages 431 Gyrochronologysupporting

confidence: 68%

Rotation, differential rotation, and gyrochronology of activeKeplerstars

Reinhold

Gizon

2015

A&A

182

170

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“…These models account for the spin-up of stars due to PMS contraction and AM conservation, the loss of AM at the surface due to winds, and the transport of AM in the stellar interiors. In Figure 6, we show the resulting forward models for solid-body (black) and core-envelope recoupling (blue) models with the Kawaler (1988) and Matt et al (2012Matt et al ( , 2015 wind laws. These are compared as histograms to the Pleiades cluster data (red) in three different mass bins.…”

Section: Forward Modelingmentioning

confidence: 99%

“…In each panel of the first three columns, the red histogram reflects the Pleiades rotation distribution, the black histogram is a solid-body forward model, and the blue histogram is a core-envelope recoupling forward model (see Section 2.3). Each row uses a different wind law: Kawaler (1988) on the top, Matt et al (2012) in the middle, and Matt et al (2015) on the bottom. The agreement between the peak and spread of the forward models is good, in general, suggesting the wind laws are successfully predicting early Mdwarf rotational evolution.…”

Section: Forward Modelingmentioning

confidence: 99%

M Dwarf Rotation from the K2 Young Clusters to the Field. I. A Mass–Rotation Correlation at 10 Myr

Somers

Stauffer

Rebull

et al. 2017

ApJ

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Recent observations of the low-mass (0.1-0.6 M  ) rotation distributions of the Pleiades and Praesepe clusters have revealed a ubiquitous correlation between mass and rotation, such that late Mdwarfs rotate an order-of-magnitude faster than early Mdwarfs. In this paper, we demonstrate that this mass-rotation correlation is present in the 10Myr Upper Scorpius association, as revealed by new K2 rotation measurements. Using rotational evolution models, we show that the low-mass rotation distribution of the 125Myr Pleiades cluster can only be produced if it hosted an equally strong mass-rotation correlation at 10Myr. This suggests that physical processes important in the early pre-main sequence (PMS; star formation, accretion, disk-locking) are primarily responsible for the Mdwarf rotation morphology, and not quirks of later angular momentum (AM) evolution. Such early mass trends must be taken into account when constructing initial conditions for future studies of stellar rotation. Finally, we show that the average Mstar loses ∼25%-40% of its AM between 10 and 125Myr, a figure accurately and generically predicted by modern solar-calibrated wind models. Their success rules out a lossless PMS and validates the extrapolation of magnetic wind laws designed for solar-type stars to the low-mass regime at early times.

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“…Kim & Demarque 1996;Matt et al 2015). It can be defined in a variety of nearly equivalent ways (e.g.…”

Section: Convective Turnover Timementioning

confidence: 99%

Spherical-shell boundaries for two-dimensional compressible convection in a star

Pratt

Baraffe

Goffrey

et al. 2016

A&A

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Context. Studies of stellar convection typically use a spherical shell geometry. The radial extent of the shell and the boundary conditions applied are based on the model of the star investigated. We study the impact of different two-dimensional spherical shells on compressible convection. Realistic profiles for density and temperature from an established one-dimensional stellar evolution code are used to produce a model of a large stellar convection zone representative of a young low-mass star, such as our sun at 10 6 years of age. Aims. We analyze how the radial extent of the spherical shell changes the convective dynamics that result in the deep interior of the young sun model, far from the surface. In the near-surface layers, simple smaller-scale convection develops from the profiles of temperature and density. A central radiative zone below the convection zone provides a lower boundary on the convection zone. The inclusion of either of these physically distinct layers in the spherical shell can potentially affect the characteristics of deep convection. Methods. We perform hydrodynamic implicit large-eddy simulations of compressible convection using the MUltidimensional Stellar Implicit Code (MUSIC). Because MUSIC has been designed to use realistic stellar models produced from one-dimensional stellar evolution calculations, MUSIC simulations are capable of seamlessly modeling a whole star. Simulations in two-dimensional spherical shells that have different radial extents are performed over tens or even hundreds of convective turnover times, permitting the collection of well-converged statistics. Results. To measure the impact of the spherical shell geometry and our treatment of boundaries, we evaluate basic statistics of the convective turnover time, the convective velocity, and the overshooting layer. These quantities are selected for their relevance to one-dimensional stellar evolution calculations, so that our results are focused toward studies exploiting the so-called 321D link. We find that the inclusion in the spherical shell of the boundary between the radiative and convection zones decreases the amplitude of convective velocities in the convection zone. The inclusion of near-surface layers in the spherical shell can increase the amplitude of convective velocities, although the radial structure of the velocity profile established by deep convection is unchanged. The impact from including the near-surface layers depends on the speed and structure of small-scale convection in the near-surface layers. Larger convective velocities in the convection zone result in a commensurate increase in the overshooting layer width and decrease in the convective turnover time. These results provide support for non-local aspects of convection.

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The Mass-Dependence of Angular Momentum Evolution in Sun-Like Stars

Cited by 310 publications

References 50 publications

Rotation, differential rotation, and gyrochronology of activeKeplerstars

Rotation, differential rotation, and gyrochronology of activeKeplerstars

M Dwarf Rotation from the K2 Young Clusters to the Field. I. A Mass–Rotation Correlation at 10 Myr

Spherical-shell boundaries for two-dimensional compressible convection in a star

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