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Monday, July 20, 2020 | History

5 edition of The solar tachocline found in the catalog.

The solar tachocline

The solar tachocline

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Published by Cambridge University Press in Cambridge .
Written in English

    Subjects:
  • Helioseismology.

  • Edition Notes

    Includes bibliographical references and index.

    Statementedited by David W. Hughes, Robert Rosner, Nigel O. Weiss.
    ContributionsHughes, David W., Rosner, Robert., Weiss, N. O.
    Classifications
    LC ClassificationsQB539.I5 S68 2007
    The Physical Object
    Paginationxi, 367 p. :
    Number of Pages367
    ID Numbers
    Open LibraryOL22754478M
    ISBN 100521861012
    ISBN 109780521861014

    We study the physics of the solar tachocline and related MHD instabilities. We have performed 3-D MHD simulations of the solar radiative interior to check.   The solar tachocline may consist of two parts: the inner radiative layer with a strongly stable stratification and the outer overshoot layer with a weakly stable stratification (Gilman ). The latitudinal differential rotation should be stronger in the upper tachocline and weaker in the lower one.

    It is not clear whether the solar tachocline is linearly unstable: when one applies the criterion derived by Watson [10] to an angular velocity profile of the type Ω ∝ 1 − α 1sin2λ, where λ is the latitude, linear instability requires α 1 > , which is larger than the solar value α 1 ≈ It appears, however, that a law of. The global-scale interior magnetic field B i needed to account for the Sun's observed differential rotation can be effective only if confined below the convection zone in all latitudes including, most critically, the polar caps. Axisymmetric solutions are obtained to the nonlinear magnetohydrodynamic equations showing that such polar confinement can be brought about .

      It is widely believed that the Sun's magnetic field is generated by a magnetic dynamo within the Sun. The fact that the Sun's magnetic field changes dramatically over the course of just a few years, and the fact that it changes in a cyclical manner indicates that the magnetic field continues to be generated within the Sun. A successful model for the solar . Baroclinic instability in the tachocline competing with instability of the latitude rotation gradient established in earlier studies should be important for the workings of the solar dynamo and should be expected to be found in most stars that contain an interface between radiative and convective domains.}, doi = {/X//1/


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The solar tachocline Download PDF EPUB FB2

The Solar Tachocline has been added to your Cart Add to Cart. Buy Now More Buying Choices 10 New from $ 5 Used from $ 15 used & new from $ See All Buying Options Available at a lower price from other sellers that may not offer free Prime shipping.

The Solar Tachocline is a valuable reference for researchers and graduate students in astrophysics, heliospheric physics and geophysics, and the dynamics of fluids and plasmas. Product Details About the AuthorPrice: $ It provides the only comprehensive account of the current understanding of the properties and dynamics of the tachocline, including both observational results and major theoretical issues, involving both hydrodynamic and magnetohydrodynamic behaviour.\" \"The Solar Tachocline is a reference for researchers and graduate students in astrophysics.

The Solar Tachocline is a valuable reference for researchers and graduate students in astrophysics, heliospheric physics and geophysics, and the dynamics of fluids and plasmas.

Reviews 'Many of the challenging problems discussed will probably be with us for decades, so the book will become a valuable source, both for established workers and. Containing reviews from distinguished speakers at the first meeting devoted to the tachocline, this book is the first comprehensive account of the current understanding of the subject.

It is a valuable reference for researchers and graduate students in astrophysics, heliospheric physics and geophysics, and the dynamics of fluids and plasmas.

Magnetic confinement of the solar tachocline P. Garaud; 8. Magnetic confinement and the sharp tachopause M. McIntyre; 9. ß-Plane MHD turbulence and dissipation in the solar tachocline P. Diamond, K. Itoh, S.-Cited by: We refer the reader to the book "The solar tachocline" (edited by Hughes, Rosner & Weiss, ) for a comprehensive and relatively recent review of the current research problems associated with.

1. Introduction. Helioseismic inversions inferred the existence of a thin shear-layer (Brown et al.,Goode et al., ) straddling at the base of the solar convection zone, now known to be at R ⊙.This is the layer, called the tachocline, where the purely latitudinal differential rotation of the convection zone transitions to the solid rotation of the core.

The Solar Tachocline is a valuable reference for researchers and graduate students in astrophysics, heliospheric physics and geophysics, and the dynamics of fluids ings, it was agreed that we should edit a book containing invited chapters from selected participants, each of which would be refereed by another participant.

The Solar Tachocline is a valuable reference for researchers and graduate students in astrophysics, heliospheric physics and geophysics, and the dynamics of fluids and plasmas. 我来说两句 短评. The penetration depth depends on whether or not the tachocline is turbulent.

However, even in the very unlikely case of a turbulent tachocline (left edge of Figure 2), the penetration depth is only a few thousand kilometres, that is less than 1% of the solar radius. The transport of magnetic fields into the tachocline must be weak, too. Abstract. In this paper I shall describe the dynamics of the solar tachocline.

This region at the base of the solar convection zone is believed to play a key role in the generation of the solar. Buy The Solar Tachocline from Helioseismology has enabled us to probe the internal structure and dynamics of the Sun, including how its rotation varies in the solar interior.

The unexpected discovery of an abrupt transition – the tachocline – between the differentially rotating convection zone and the uniformly rotating radiative interior has generated Price: $ The Solar Tachocline: A Self-Consistent Model of Magnetic Confinement Toby Wood Queens’ College, Cambridge A Dissertation submitted to the University of Cambridge for the degree of Doctor of Philosophy April “There is no easy way from the earth to the stars”.

the solar interior, b rough t ab out partly by Bob Dic ke’s claim that the su r- face of the Su n is s ome six times more oblate (implying a fold increase in ellipticit y) th an one would ha.

Callebaut et al. ()'s claim that Scafetta ()'s results about a correlation between year and year temperature cycles and the orbital motion of Jupiter and Saturn were not confirmed by Humlum et al.

() is erroneous and severely misleading. Also Callebaut et al. ()'s absolute claim that a planetary influences on the Sun should be ruled out as a possible cause of solar.

The lack of a tachocline in fully convective stars therefore suggests that this is not a critical ingredient in the solar dynamo and supports models in which the dynamo originates throughout the.

We also show how these results can be understood in terms of a reduced, analytical model that is asymptotically valid in the parameter regime of relevance to the solar tachocline. In Part IV we discuss how our high-latitude model can be extended to a global model of magnetic confinement within the tachocline.

The solar dynamo is a physical process that generates the Sun's magnetic is explained with a variant of the dynamo theory.A naturally occurring electric generator in the Sun's interior produces electric currents and a magnetic field, following the laws of Ampère, Faraday and Ohm, as well as the laws of fluid dynamics, which together form the laws of magnetohydrodynamics.

Abstract. Some established views of the solar magnetic cycle are discussed critically, with focus on two aspects at the core of most models: the role of convective turbulence, and the role of the “tachocline” at the base of the convection zone. tachocline definition: nounThe boundary in the solar interior between the outer convection zone and the inner radiative zone.

This boundary arises from the fact that the convection zone rotates faster near the solar equator than it does near the solar po. The Institute of Physics (IOP) is a leading scientific society promoting physics and bringing physicists together for the benefit of all.

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