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Zustand: Good. This is an ex-library book and may have the usual library/used-book markings inside.This book has hardback covers. In good all round condition. No dust jacket. Please note the Image in this listing is a stock photo and may not match the covers of the actual item,450grams, ISBN:0571115500. …

Hardcover Jul 08, 2009. Zustand: gebraucht; wie neu.

Zustand: New. In English.

Zustand: New. In English.

Zustand: Sehr gut. Zustand: Sehr gut | Seiten: 436 | Sprache: Englisch | Produktart: Bücher | Starting in 1995 numerical modeling of the Earth¿s dynamo has ourished with remarkable success. Direct numerical simulation of convection-driven MHD- ow in a rotating spherical shell show magnetic elds that resemble the geomagnetic eld in many respects: they are dominated by the axial dipole of approximately the right strength, they show spatial power spectra similar to that of Earth, and the magnetic eld morphology and the temporal var- tion of the eld resembles that of the geomagnetic eld (Christensen and Wicht 2007). Some models show stochastic dipole reversals whose details agree with what has been inferred from paleomagnetic data (Glatzmaier and Roberts 1995; Kutzner and Christensen 2002; Wicht 2005). While these models represent direct numerical simulations of the fundamental MHD equations without parameterized induction effects, they do not match actual pla- tary conditions in a number of respects. Speci cally, they rotate too slowly, are much less turbulent, and use a viscosity and thermal diffusivity that is far too large in comparison to magnetic diffusivity. Because of these discrepancies, the success of geodynamo models may seem surprising. In order to better understand the extent to which the models are applicable to planetary dynamos, scaling laws that relate basic properties of the dynamo to the fundamental control parameters play an important role. In recent years rst attempts have been made to derive such scaling laws from a set of numerical simulations that span the accessible parameter space (Christensen and Tilgner 2004; Christensen and Aubert 2006).…

Paperback. Zustand: Brand New. 436 pages. 9.25x6.10x1.03 inches. In Stock.

Taschenbuch. Zustand: Neu. Helioseismology and Dynamics of the Solar Interior | M. J. Thompson (u. a.) | Taschenbuch | Space Sciences Series of ISSI | vi | Englisch | 2018 | Springer | EAN 9789402414714 | Verantwortliche Person für die EU: Springer Verlag GmbH, Tiergartenstr. 17, 69121 Heidelberg, juergen[dot]hartmann[at]springer[dot]com | Anbieter: preigu. …

Hardcover. Zustand: Brand New. 1st edition. 430 pages. 9.29x0.87x0.31 inches. In Stock.

Buch. Zustand: Neu. Druck auf Anfrage Neuware - Printed after ordering - The articles republished in this book survey and summarize recent research in helioseismology as well as studies of the interior structure, dynamics and magnetism of the solar interior that are being tested and refined using the helioseismic results.Helioseismology has in the last few decades become a highly productive technique for studying the Sun's interior from observations of the vibrations of its surface. The vibrations are manifestations of resonant modes of the Sun that are continuously excited by turbulent motions in the Sun's convection zone, and a plethora of data have been obtained from dedicated ground-based and space-based observing systems.The book will be of particular interest to researchers and graduate students in the fields of helioseismology, solar interior dynamics and the solar dynamo. It will also be of interest to researchers in solar physics, solar activity, stellar physics, astrophysical fluid dynamics and asteroseismology.Originallypublished in Space Science Reviews, Volume 196, Issue 1-4, December 2015.…

Taschenbuch. Zustand: Neu. Druck auf Anfrage Neuware - Printed after ordering - The articles republished in this book survey and summarize recent research in helioseismology as well as studies of the interior structure, dynamics and magnetism of the solar interior that are being tested and refined using the helioseismic results.Helioseismology has in the last few decades become a highly productive technique for studying the Sun's interior from observations of the vibrations of its surface. The vibrations are manifestations of resonant modes of the Sun that are continuously excited by turbulent motions in the Sun's convection zone, and a plethora of data have been obtained from dedicated ground-based and space-based observing systems.The book will be of particular interest to researchers and graduate students in the fields of helioseismology, solar interior dynamics and the solar dynamo. It will also be of interest to researchers in solar physics, solar activity, stellar physics, astrophysical fluid dynamics and asteroseismology.Originallypublished in Space Science Reviews, Volume 196, Issue 1-4, December 2015.…

Taschenbuch. Zustand: Neu. Druck auf Anfrage Neuware - Printed after ordering - Starting in 1995 numerical modeling of the Earth's dynamo has ourished with remarkable success. Direct numerical simulation of convection-driven MHD- ow in a rotating spherical shell show magnetic elds that resemble the geomagnetic eld in many respects: they are dominated by the axial dipole of approximately the right strength, they show spatial power spectra similar to that of Earth, and the magnetic eld morphology and the temporal var- tion of the eld resembles that of the geomagnetic eld (Christensen and Wicht 2007). Some models show stochastic dipole reversals whose details agree with what has been inferred from paleomagnetic data (Glatzmaier and Roberts 1995; Kutzner and Christensen 2002; Wicht 2005). While these models represent direct numerical simulations of the fundamental MHD equations without parameterized induction effects, they do not match actual pla- tary conditions in a number of respects. Speci cally, they rotate too slowly, are much less turbulent, and use a viscosity and thermal diffusivity that is far too large in comparison to magnetic diffusivity. Because of these discrepancies, the success of geodynamo models may seem surprising. In order to better understand the extent to which the models are applicable to planetary dynamos, scaling laws that relate basic properties of the dynamo to the fundamental control parameters play an important role. In recent years rst attempts have been made to derive such scaling laws from a set of numerical simulations that span the accessible parameter space (Christensen and Tilgner 2004; Christensen and Aubert 2006).…

Buch. Zustand: Neu. Druck auf Anfrage Neuware - Printed after ordering - Starting in 1995 numerical modeling of the Earth's dynamo has ourished with remarkable success. Direct numerical simulation of convection-driven MHD- ow in a rotating spherical shell show magnetic elds that resemble the geomagnetic eld in many respects: they are dominated by the axial dipole of approximately the right strength, they show spatial power spectra similar to that of Earth, and the magnetic eld morphology and the temporal var- tion of the eld resembles that of the geomagnetic eld (Christensen and Wicht 2007). Some models show stochastic dipole reversals whose details agree with what has been inferred from paleomagnetic data (Glatzmaier and Roberts 1995; Kutzner and Christensen 2002; Wicht 2005). While these models represent direct numerical simulations of the fundamental MHD equations without parameterized induction effects, they do not match actual pla- tary conditions in a number of respects. Speci cally, they rotate too slowly, are much less turbulent, and use a viscosity and thermal diffusivity that is far too large in comparison to magnetic diffusivity. Because of these discrepancies, the success of geodynamo models may seem surprising. In order to better understand the extent to which the models are applicable to planetary dynamos, scaling laws that relate basic properties of the dynamo to the fundamental control parameters play an important role. In recent years rst attempts have been made to derive such scaling laws from a set of numerical simulations that span the accessible parameter space (Christensen and Tilgner 2004; Christensen and Aubert 2006).…

Paperback. Zustand: Brand New. reprint edition. 362 pages. 9.25x6.10x0.83 inches. In Stock.

Zustand: gut. The Origin and Dynamics of Solar Magnetism (Space Sciences Series of ISSI, 32, Band 144) In englischer Sprache. pages.