scholarly journals Pulsations of rapidly rotating stars

2015 ◽  
Vol 579 ◽  
pp. A116 ◽  
Author(s):  
R.-M. Ouazzani ◽  
I. W. Roxburgh ◽  
M.-A. Dupret
Keyword(s):  
Rotating Stars ◽  
Rapidly Rotating Stars

scholarly journals Rossby Waves in Astrophysics

2021 ◽  
Vol 217 (1) ◽  
Author(s):  
T. V. Zaqarashvili ◽  
M. Albekioni ◽  
J. L. Ballester ◽  
Y. Bekki ◽  
L. Biancofiore ◽  
...  
Keyword(s):  
Large Scale ◽  
Rossby Waves ◽  
Magnetic Activity ◽  
Future Research ◽  
Rotating Stars ◽  
Spatial And Temporal Scales ◽  
Physical Role ◽  
Astrophysical Objects ◽  
Exoplanetary Atmospheres ◽  
Rapidly Rotating Stars

AbstractRossby waves are a pervasive feature of the large-scale motions of the Earth’s atmosphere and oceans. These waves (also known as planetary waves and r-modes) also play an important role in the large-scale dynamics of different astrophysical objects such as the solar atmosphere and interior, astrophysical discs, rapidly rotating stars, planetary and exoplanetary atmospheres. This paper provides a review of theoretical and observational aspects of Rossby waves on different spatial and temporal scales in various astrophysical settings. The physical role played by Rossby-type waves and associated instabilities is discussed in the context of solar and stellar magnetic activity, angular momentum transport in astrophysical discs, planet formation, and other astrophysical processes. Possible directions of future research in theoretical and observational aspects of astrophysical Rossby waves are outlined.

scholarly journals Learning about Stellar Dynamos from Long–term Photometry of Starspots

1991 ◽  
Vol 130 ◽  
pp. 353-369 ◽  
Author(s):  
Douglas S. Hall
Keyword(s):  
Differential Rotation ◽  
Rotation Period ◽  
Turnover Time ◽  
Rotating Stars ◽  
Photometric Variability ◽  
Solar Type ◽  
Magnetic Cycles ◽  
The Many ◽  
Rapidly Rotating Stars

AbstractSpottedness, as evidenced by photometric variability in 277 late-type binary and single stars, is found to occur when the Rossby number is less than about 2/3. This holds true when the convective turnover time versus B–V relation of Gilliland is used for dwarfs and also for subgiants and giants if their turnover times are twice and four times longer, respectively, than for dwarfs. Differential rotation is found correlated with rotation period (rapidly rotating stars approaching solid-body rotation) and also with lobe-filling factor (the differential rotation coefficient k is 2.5 times larger for F = 0 than F = 1). Also reviewed are latitude extent of spottedness, latitude drift during a solar-type cycle, sector structure and preferential longitudes, starspot lifetimes, and the many observational manifestations of magnetic cycles.

scholarly journals P-modes in rapidly rotating stars: Looking for regular patterns in synthetic asymptotic spectra

2010 ◽  
Vol 331 (9-10) ◽  
pp. 1053-1056 ◽  
Author(s):  
F. Lignières ◽  
B. Georgeot ◽  
J. Ballot
Keyword(s):  
Rotating Stars ◽  
Rapidly Rotating Stars ◽  
Regular Patterns

The Lack of Blue Supergiants in NGC 7419, a Red Supergiant-rich Galactic Open Cluster with Rapidly Rotating Stars

2003 ◽  
Vol 126 (3) ◽  
pp. 1415-1422 ◽  
Author(s):  
Genevive Caron ◽  
Anthony F. J. Moffat ◽  
Nicole St-Louis ◽  
Gregg A. Wade ◽  
John B. Lester
Keyword(s):  
Open Cluster ◽  
Rotating Stars ◽  
Rapidly Rotating Stars

Oscillations of Fast Rotating Stars: p-Modes in Centrifugally Flattened Polytropes

2004 ◽  
Vol 215 ◽  
pp. 414-415 ◽  
Author(s):  
F. Lignières ◽  
M. Rieutord
Keyword(s):  
Numerical Method ◽  
Centrifugal Force ◽  
Perturbation Methods ◽  
Mathematical Formalism ◽  
Rotating Stars ◽  
Oscillation Modes ◽  
Rapidly Rotating Stars ◽  
Fast Rotating

Oscillation modes of rapidly rotating stars have not yet been calculated with precision, rotational effects being generally approximated by perturbation methods. We developed a mathematical formalism and a numerical method which fully account for the deformation of the star by the centrifugal force. The method has been first tested in the case of Maclaurin spheroids and then applied to uniformly rotating polytropic stars.

scholarly journals Spectroscopy of LMC cluster stars

2019 ◽  
Vol 14 (S351) ◽  
pp. 97-100
Author(s):  
A. K. Dupree ◽  
C. I. Johnson ◽  
M. Mateo ◽  
A. P. Milone
Keyword(s):  
High Resolution ◽  
Globular Cluster ◽  
Narrow Band ◽  
Rotating Stars ◽  
Photometric Measurements ◽  
Rapidly Rotating Stars

AbstractHigh resolution spectra of stars in the ≈200 Myr LMC globular cluster, NGC 1866, reveal rapidly rotating stars with variable H α emission and absorption, and signatures of outflowing material. The variable H α line can substantially affect photometric measurements obtained with HST/WFC3 narrow-band filters.

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