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Keywords = solar supergranulation

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23 pages, 17262 KB  
Review
Research Progress on Solar Supergranulation: Observations, Theories, and Numerical Simulations
by Chong Huang and Rui Wang
Universe 2025, 11(3), 87; https://doi.org/10.3390/universe11030087 - 6 Mar 2025
Viewed by 1010
Abstract
Solar supergranulation is a large-scale convective structure on the solar surface, whose formation mechanism and dynamical properties are closely related to key physical processes such as solar magnetic field evolution, coronal heating, and solar wind acceleration. This paper reviews recent research progress on [...] Read more.
Solar supergranulation is a large-scale convective structure on the solar surface, whose formation mechanism and dynamical properties are closely related to key physical processes such as solar magnetic field evolution, coronal heating, and solar wind acceleration. This paper reviews recent research progress on solar supergranulation, focusing on the latest achievements in high-resolution observations, theoretical models, and numerical simulations. By analyzing the flow field structure, magnetic field distribution, and their relationship with the solar activity cycle, the crucial role of supergranulation in solar physics is revealed. Studies indicate that supergranulation is not only a crucial component of the solar convection zone but also drives coronal heating and solar wind acceleration through mechanisms such as magnetic reconnection and Alfvén wave propagation. Furthermore, the interaction between supergranulation and larger-scale convective patterns (e.g., giant cells) provides new insights into the dynamics of the solar interior. Despite significant progress in recent years, the formation mechanism and dynamical nature of supergranulation remain unresolved. Future research should combine high-resolution observations, theoretical modeling, and numerical simulations to further elucidate the complex dynamical processes and the central role of supergranulation in solar physics. Full article
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11 pages, 577 KB  
Article
Stellar Turbulent Convection: The Multiscale Nature of the Solar Magnetic Signature
by Stefano Scardigli, Francesco Berrilli, Dario Del Moro and Luca Giovannelli
Atmosphere 2021, 12(8), 938; https://doi.org/10.3390/atmos12080938 - 22 Jul 2021
Cited by 3 | Viewed by 2517
Abstract
The multiscale dynamics associated with turbulent convection present in physical systems governed by very high Rayleigh numbers still remains a vividly disputed topic in the community of astrophysicists, and in general, among physicists dealing with heat transport by convection. The Sun is a [...] Read more.
The multiscale dynamics associated with turbulent convection present in physical systems governed by very high Rayleigh numbers still remains a vividly disputed topic in the community of astrophysicists, and in general, among physicists dealing with heat transport by convection. The Sun is a very close star for which detailed observations and estimations of physical properties on the surface, connected to the processes of the underlying convection zone, are possible. This makes the Sun a unique natural laboratory in which to investigate turbulent convection in the hard turbulence regime, a regime typical of systems characterized by high values of the Rayleigh number. In particular, it is possible to study the geometry of convection using the photospheric magnetic voids (or simply voids), the quasi-polygonal quiet regions nearly devoid of magnetic elements, which cover the whole solar surface and which form the solar magnetic network. This work presents the most extensive statistics, both in the spatial scales studied (1–80 Mm) and in the temporal duration (SC 23 and SC 24), to investigate the multiscale nature of solar magnetic patterns associated with the turbulent convection of our star. We show that the size distribution of the voids, in the 1–80 Mm range, for the 317,870 voids found in the 692 analyzed magnetograms, is basically described by an exponential function. Full article
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