Journal ArticleDOI
Rossby vortices as sources of global magnetic structures on the Sun
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In this paper, a numerical simulation of the process of generation of the magnetic field by Rossby vortices, whose horizontal scale is comparable to the solar radius, has been carried out.Abstract:
A numerical simulation of the process of generation of the magnetic field by Rossby vortices, whose horizontal scale is comparable to the solar radius, has been carried out. Long-lived vortices form global magnetic structures that drift together with vortices. Differential rotation in latitude leads to a longer lifetime of cyclones and corresponding magnetic structures. The cyclone and the magnetic structure travel in longitude with the velocity close to a corresponding differential rotation velocity and drift slowly poleward. The interaction of cyclones located in close latitudes makes one of them move to higher latitudes and the poloidal component of the magnetic field to intensify during the interaction. The formation of large-scale vortices was simulated, when the initial condition was specified by a grid of small-scale vortices with a random amplitude distribution. Merging of vortices of the same sign leads to the formation of large-scale vortices whose size is determined by the geometry of the problem and by the differential rotation profile.read more
Citations
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Influence of the Solar Global Magnetic Field Structure Evolution on CMEs
TL;DR: In this article, the influence of the solar global magnetic field structure (GMFS) cycle evolution on the occurrence rate and parameters of coronal mass ejections (CMEs) in cycles 23-24 was considered.
Journal ArticleDOI
Influence of the Solar Global Magnetic-Field Structure Evolution on CMEs
TL;DR: In this article, the influence of the solar global magnetic field structure (GMFS) cycle evolution on the occurrence rate and parameters of coronal mass ejections (CMEs) in Solar Cycles was considered.
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Large-Scale Transport of Magnetic Flux on the sun
TL;DR: In this article, the large-scale horizontal transport velocity field of the magnetic flux patterns was inferred over the whole solar photosphere in the course of two solar activity cycles from year 1976 to 1999.
Journal ArticleDOI
Forcing of Differential Rotation and Rossby Waves at the Interface between the Convectively Stable and Unstable Layers
TL;DR: In this paper, a model for the high-latitude region near the interface between the solar convection and radiative zones is suggested, where the deformation of the interface is due to the influence of large-scale flows on this region's conditions.
Journal ArticleDOI
Short‐scale convection and long‐scale deformationally unstable Rossby wave in a rotating fluid layer heated from below
TL;DR: In this article, a rotating fluid layer, heated from below, with a deformable upper and nondeformable lower stress free surfaces is considered in the Boussinesq approximation.
References
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Journal ArticleDOI
Planetary Circulations: 1. Barotropic Representation of Jovian and Terrestrial Turbulence
TL;DR: In this article, the formative processes of the planetary circulations of Jupiter and Saturn were studied and it was shown that a strong affinity exists between the Jovian and terrestrial circulations.
Journal ArticleDOI
Surface magnetic fields during the solar activity cycle
Robert Howard,Barry J. Labonte +1 more
Abstract: We examine magnetic field measurements from Mount Wilson that cover the solar surface over a 13 1/2 year interval, from 1967 to mid-1980. Seen in long-term averages, the sunspot latitudes are characterized by fields of preceding polarity, while the polar fields are built up by a few discrete flows of following polarity fields. These drift speeds average about 10 m s-1 in latitude - slower early in the cycle and faster later in the cycle - and result from a large-scale poleward displacement of field lines, not diffusion. Weak field plots show essentially the same pattern as the stronger fields, and both data indicate that the large-scale field patterns result only from fields emerging at active region latitudes. The total magnetic flux over the solar surface varies only by a factor of about 3 from minimum to a very strong maximum (1979). Magnetic flux is highly concentrated toward the solar equator; only about 1% of the flux is at the poles. Magnetic flux appears at the solar surface at a rate which is sufficient to create all the flux that is seen at the solar surface within a period of only 10 days. Flux can spread relatively rapidly over the solar surface from outbreaks of activity. This is presumably caused by diffusion. In general, magnetic field lines at the photospheric level are nearly radial.
Journal ArticleDOI
Nonlinear Convection of a Compressible Fluid in a Rotating Spherical Shell
Peter A. Gilman,J. Miller +1 more
Journal ArticleDOI
Solar Activity and Recurrences in Magnetic-Field Distribution
TL;DR: A study of the Mount Wilson magnetic field synoptic chart material divided into latitude zones for the interval 1959-67, and a comparison of the data with sunspot groups have provided a better understanding of the structure of the background-field pattern and its relation to activity as mentioned in this paper.
Journal ArticleDOI
Rotation of the Photospheric Magnetic Fields: A North-South Asymmetry
TL;DR: In this paper, a Fourier analysis of photospheric synoptic charts obtained at the Wilcox Solar Observatory from 1976 to 1986 and confirmed in higher resolution maps from the National Solar Observatory was performed.
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