The origin and dynamics of solar magnetism /

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Bibliographic Details
Imprint:[New York, NY] : Springer, c2009.
Description:1 online resource (428 p.) : ill. (some col.)
Language:English
Series:Space sciences series of ISSI
Space sciences series of ISSI.
Subject:
Format: E-Resource Book
URL for this record:http://pi.lib.uchicago.edu/1001/cat/bib/8889416
Hidden Bibliographic Details
Other uniform titles:Space science reviews.
Other authors / contributors:Thompson, M. J., 1946-
ISBN:9781441902399
1441902392
9781441902382
Notes:"Previously published in Space Science Reviews, Volume 144, Issues 1-4, 2009."
Includes bibliographical references.
Description based on print version record.
Summary:Treats various aspects of solar magnetism, from its origin in the solar dynamo to its evolution and dynamics that create the variability of solar phenomena, from its well-known 11-year activity cycle to the ever-changing pattern of sunspots and active regions on the Sun.
Other form:Print version: Origin and dynamics of solar magnetism. New York : Springer, c2009 9781441902382
Description
Summary: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).
Item Description:"Previously published in Space Science Reviews, Volume 144, Issues 1-4, 2009."
Physical Description:1 online resource (428 p.) : ill. (some col.)
Bibliography:Includes bibliographical references.
ISBN:9781441902399
1441902392
9781441902382