# On the Structure and Properties of Differentially Rotating, Main-Sequence Stars in the 1-2 M☉ Range

@article{Macgregor2007OnTS,
title={On the Structure and Properties of Differentially Rotating, Main-Sequence Stars in the 1-2 M☉ Range},
author={Keith B. Macgregor and Stephen Jackson and Andrew Skumanich and Travis S. Metcalfe},
journal={The Astrophysical Journal},
year={2007},
volume={663},
pages={560-572}
}
• Published 10 April 2007
• Physics
• The Astrophysical Journal
We present models for chemically homogeneous, differentially rotating, main-sequence stars with masses in the range 1-2 M☉. The models were constructed using a code based on a reformulation of the self-consistent field method of computing the equilibrium stellar structure for a specified conservative internal rotation law. Relative to nonrotating stars of the same mass, these models all have reduced luminosities and effective temperatures, and flattened photospheric shapes (i.e., decreased…

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## References

SHOWING 1-10 OF 45 REFERENCES
2-dimensional models of rapidly rotating stars I. Uniformly rotating zero age main sequence stars
We present results for 2-dimensional models of rapidly rotating main sequence stars for the case where the an- gular velocity Ω is constant throughout the star. The algorithm used solves for the
On the Use of the Self-consistent-Field Method in the Construction of Models for Rapidly Rotating Main-Sequence Stars
• Physics
• 2005
A new formulation of the self-consistent-field (SCF) method for computing models of rapidly, differentially rotating stars is described. The angular velocity is assumed to depend only on the distance
THE ANGULAR MOMENTUM OF MAIN SEQUENCE STARS AND ITS RELATION TO STELLAR ACTIVITY
• Physics
• 1997
Rotational velocities are reported for intermediate-mass main sequence stars it the field. The measurements are based on new, high S/N CCD spectra from the Coude Feed Telescope of the Kitt Peak
The structure of rotating stars:the J2 method and results for uniform rotation
• Physics
• 1973
S>The J/sup 2/ method for solving the structure of uniformly and nonuniformly rotating stars is briefly described and compared with other methods. The method is restricted to rotation laws of the
Rotation in solar-type stars. I. Evolutionary models for the spin-down of the sun
• Physics
• 1981
We have calculated models of rotating 1 M/sub sun/ stars through the pre-main-sequence and main-sequence stages. The calculations start on the Hayashi track with rapid, rigid-body rotation. As the
Star clusters and stellar evolution. I. Improved synthetic color-magnitude diagrams for the oldest clusters.
New stellar evolutionary sequences extending from the main sequence to the base of the red giant branch have been computed assuming two values of the helium abundance, Y = 0.2, for each of the
The Internal Rotation of the Sun
• Physics
• 2003
▪ Abstract Helioseismology has transformed our knowledge of the Sun's rotation. Earlier studies revealed the Sun's surface rotation, but now a detailed observational picture has been built up of the
Evolutionary models of the rotating sun
• Physics
• 1989
This paper reviews current work on the evolution of a differentially rotating solar model. Although we discuss global features of the evolution with rotation in general terms, the specific models
On the equilibrium and secular instability of rapidly rotating stars.
Rotating main-sequence models in the mass range 1.5--30 M/sub sun/ have been computed with a two-dimensional relaxation technique. An analysis which incorporates a new criterion for marginal secular
Stellar evolution with rotation and magnetic fields - IV. The solar rotation profile
• Physics
• 2005
We examine the generation of a magnetic field in a solar-like star and its effects on the internal distribution of the angular velocity. We suggest that the evolution of a rotating star with magnetic