4 edition of Differential rotation and stellar convection found in the catalog.
|Series||The fluid mechanics of astrophysics and geophysics ;, v. 5|
|LC Classifications||QB523 .R93 1989|
|The Physical Object|
|Pagination||328 p. :|
|Number of Pages||328|
|LC Control Number||88039551|
It combines theory and observation in a comprehensive survey of how the rotation of stars affects the structure and evolution of the Sun, single stars, and close binaries." "This book will be of primary interest to graduate students and researchers studying solar and stellar rotation and close binary systems. springer, This volume synthesizes the results of work carried out by several international teams of the SIROCO (Seismology for Rotation and Convection) collaboration. It provides the theoretical background required to interpret the huge quantity of high-quality observational data recently provided by space experiments such as CoRoT and Kepler.
Differential rotation in the convection zone Meridional circulation in the radiative core Spin-down of the solar interior Discussion Bibliographical notes 6 The early-type stars Introduction Main-sequence models . Stellar convection theory. Differential rotation and magnetic activity of the lower main sequence stars. Pages Stellar Turbulence Book Subtitle Proceedings of Colloquium 51 of the International Astronomical Union, Held at the University of Western Ontario, London, Ontario, Canada, August 27 .
The other physical information that should in principle be discoverable from photometric light curves is a measurement of differential rotation on stellar surfaces. The Sun is a differential rotator with a period of about 25 days at the equator and 29 days at the pole (and a sine law with latitude in between).Author: Gibor Basri. Oct 30, · This book brings together for the first time recent results in solar studies and stellar studies. The result is an illuminating new view of stellar magnetic activity. Key topics include radiative transfer, convective simulations, dynamo theory, outer-atmospheric heating, stellar winds and 5/5(1).
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Differential rotation affects stellar optical absorption-line spectra through line broadening caused by lines being differently Doppler-shifted across the stellar surface. Solar differential rotation causes shear at the so-called tachocline.
This is a region where rotation changes from differential in the convection zone to nearly solid-body. Differential rotation and stellar convection: sun and solar-type stars. [G Rüdiger] Home. WorldCat Home About WorldCat Help. Search. Search for Library Items Search for Lists Search for > # Differential rotation and stellar convection: sun and solar-type stars a schema:CreativeWork, schema:Book.
Title: BOOK REVIEWS: Differential rotation and stellar convection: Authors: Dogel', V. Publication: Soviet Physics Uspekhi, Volume 33, Issue 5, pp. Anti-solar differential rotation L. KITCHATINOV1,2, standing the nature of stellar differential rotation by checking stored in the radiative core into the convection zone.
In con-vection zone proper, the ﬁeld is subject to turbulent diffus ion and advection, so that toroidal ﬁeld is produced by the diffe r. Title: Differential rotation and stellar convection. Sun and the solar stars: Authors: Ruediger, Guenther: Publication: Berlin: Akademie Verlag, Stellar rotation is the angular motion of a star about its axis.
The rate of rotation can be measured from the spectrum of the star, or by timing the movements of active features on the surface. The rotation of a star produces an equatorial bulge due to centrifugal force. As stars are not solid bodies, they can also undergo differential rotation.
The differential rotation of stars. Convection and Differential Rotation in F-Type Stars. A fast and reliable method to measure stellar differential rotation from photometric data. Apr 01, · Book Review: Gunter Rüdiger Differential Rotation and Stellar Convection.
Sun and Solar-Type StarsAuthor: A. Fridman, V. Polyachenko. Differential Rotation in Stellar Convection Zones. The increasing number of observations of solar phenomena on neighbouring stars makes this book not only indispensable for students Author: Friedrich Busse.
Summary. Theory and observations of the solar differential rotation are reviewed, concentrating on recent developments. Reynolds stresses produced by stratified rotating turbulence have recently become available as fully nonlinear functions of the angular sunshinesteaming.com by: 1.
Riidiger Differential. Rotation and Stellar Convec-tion of Sun an Solar-typed Stars. Akademie-Verlag, Berlin,pp. The autho or f th booe Gk.
Riidige isr a well-known physicist from the GDR workin ign the field of solar physics. The book is devoted to an investigation of the nature of dif.
Mar 14, · Central to this problem is the description of stellar turbulent convection and how it transports heat and energy, how it redistributes angular momentum to yield large scale flows such as differential rotation and meridional circulation, and how it generates, maintains and organizes magnetic fields (see below).
Jul 18, · The review considers the modelling process for stellar convection rather than specific astrophysical results. For achieving reasonable depth and length we deal with hydrodynamics only, omitting MHD.
A historically oriented introduction offers first glimpses on the physics of stellar convection. Examination of its basic properties shows that two very different kinds of modelling keep being Cited by: A system of equations is presented for stellar convection theory. These equations follow from the full equations of compressible fluid dynamics with the introduction of two important approximations.
The first of these is the anelastic approximation, commonly used in meteorology. Its aim is to filter. the description of stellar turbulent convection and how it transports heat and energy, how it redistributes angular momentum to yield large scale flows such as differential rotation and meridional circulation, and how it generates, maintains and organizes magnetic fields (see below).
1) General Astrophysical Context. Differential rotation in stellar convection zones. Journal Article Busse, F.H. - Astron. Astrophys., v. 28, no. 1, pp. The analysis of an earlier paper (Busse la) in which the differential rotation of the Sun was explained as the result of large scale convection in the solar convection zone is extended to include the detailed.
Stellar rotation is the angular motion of a star about its axis. The rate of rotation can be measured from the spectrum of the star, or by timing the movements of active features on the surface.
The rotation of a star produces an equatorial bulge due to centripetal force. As stars are not solid bodies, they can also undergo differential rotation. Because of the pre-stellar accretion phase, and the conservation of angular momentum, rotation is induced.
Differential rotation is caused by convection in stars. This is movement of mass, due to steep temperature gradients from the core outwards. In this book the author thoroughly examines the basic mechanical and thermal effects of rotation, their influence on mass loss by stellar winds, the effects of differential rotation and its associated instabilities, the relation with magnetic fields and the evolution of the internal and surface rotation.
Astronomy concepts/terms from Horizons book Ch. 7&8 Learn with flashcards, games, and more — for free. Search. The ____ occurs when a rapidly rotating conductor is stirred by convection to produce a magnetic field.
Helioseismology is the study of the differential rotation and magnetic field of the sun. False. The rotation of the Sun's. This gives rise to a complex nonlinear interplay between turbulent convection, differential rotation, meridional circulation, and the mean specific entropy profile.
I will describe how this drama plays out in our simulations as well as in solar and stellar convection zones.Aug 24, · Such differential rotation has been observed in many F-type stars (e.g., Reiners ).
To assess how this differential rotation may arise, we have explored here the effects of rotation rate, convective overshooting, and stellar mass on the patterns and mean properties of the global-scale convection in simulations of two F-type stars.Marianne Faurobert, in The Sun as a Guide to Stellar Physics, Relations Among Activity, Rotation, and Rossby Number.
The α–Ω dynamo mechanism depends on the combined effects of differential rotation and convection.