Author:
Publisher:
ISBN:
Category : Sun-spots
Languages : en
Pages : 132
Book Description
Sunspot Numbers, 1610-1985
Author:
Publisher:
ISBN:
Category : Sun-spots
Languages : en
Pages : 132
Book Description
Publisher:
ISBN:
Category : Sun-spots
Languages : en
Pages : 132
Book Description
Sunspot Numbers: 1610-1985
Author: World Data Center A for Solar-Terrestrial Physics
Publisher:
ISBN:
Category :
Languages : en
Pages : 112
Book Description
Publisher:
ISBN:
Category :
Languages : en
Pages : 112
Book Description
Sunspot Numbers, 1610-1985
Author: John A. McKinnon
Publisher:
ISBN:
Category : Sunspots
Languages : en
Pages : 112
Book Description
Publisher:
ISBN:
Category : Sunspots
Languages : en
Pages : 112
Book Description
Sunspot Numbers, 1610-1985
Author: John A. McKinnon
Publisher:
ISBN:
Category : Sunspots
Languages : en
Pages : 112
Book Description
Publisher:
ISBN:
Category : Sunspots
Languages : en
Pages : 112
Book Description
Sunspot numbers : based on "The sunspot-activity in the years 1610 - 1960". [Hauptbd.]. 1610 - 1985
Author: World Data Centre for Solar Terrestrial Physics
Publisher:
ISBN:
Category :
Languages : en
Pages : 112
Book Description
Publisher:
ISBN:
Category :
Languages : en
Pages : 112
Book Description
World Data Center A for Solar-Terrestrial Physics
Author:
Publisher:
ISBN:
Category :
Languages : en
Pages :
Book Description
Publisher:
ISBN:
Category :
Languages : en
Pages :
Book Description
Energy Research Abstracts
Author:
Publisher:
ISBN:
Category : Power resources
Languages : en
Pages : 644
Book Description
Publisher:
ISBN:
Category : Power resources
Languages : en
Pages : 644
Book Description
Scientific and Technical Aerospace Reports
Author:
Publisher:
ISBN:
Category : Aeronautics
Languages : en
Pages : 964
Book Description
Publisher:
ISBN:
Category : Aeronautics
Languages : en
Pages : 964
Book Description
Report UAG.
Author:
Publisher:
ISBN:
Category : Atmosphere, Upper
Languages : en
Pages : 516
Book Description
Publisher:
ISBN:
Category : Atmosphere, Upper
Languages : en
Pages : 516
Book Description
The Origin and Dynamics of Solar Magnetism
Author: M.J. Thompson
Publisher: Springer Science & Business Media
ISBN: 1441902392
Category : Science
Languages : en
Pages : 424
Book Description
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).
Publisher: Springer Science & Business Media
ISBN: 1441902392
Category : Science
Languages : en
Pages : 424
Book Description
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).