Texture of average solar photospheric flows and the donut-like pattern
arXiv:2301.07988 · doi:10.1051/0004-6361/202244603
Abstract
Detailed knowledge of surface dynamics is one of the key points in understanding magnetic solar activity. The motions of the solar surface, to which we have direct access via the observations, tell us about the interaction between the emerging magnetic field and the turbulent fields. The flows computed with the coherent structure tracking (CST) technique on the whole surface of the Sun allow for the texture of the velocity modulus to be analyzed and for one to locate the largest horizontal flows and determine their organization. The velocity modulus maps show structures more or less circular and closedwhich are visible at all latitudes; here they are referred to as donuts. They reflect the most active convective cells associated with supergranulation. These annular flows are not necessarily joined as would seem to indicate the divergence maps. The donuts have identical properties (amplitude, shape, inclination, etc.) regardless of their position on the Sun. The kinematic simulation of the donuts' outflow applied to passive scalar (corks) indicates the preponderant action of the selected donuts which are, from our analysis, one of the major actors for the magnetic field diffusion on the quiet Sun. The absence of donuts in the magnetized areas (plages) indicates the action of the magnetic field on the strongest supergranular flows and thus modifies the diffusion of the magnetic field in that location. The detection of the donuts is a way to locate in the quiet Sun the vortex and the link with the jet, blinkers, coronal bright points (campfires), or other physical structures. Likewise, the study of the influence of donuts on the evolution of active events, such as the destruction of sunspots, filament eruptions, and their influences on upper layers via spicules and jets, could be done more efficiently via the detection of that structures.
arXiv comment14 pages, 17 figures
References in corpus (27)
- The Solar Internetwork. I. Contribution to the Network Magnetic Flux
- Evidence of photospheric vortex flows at supergranular junctions observed by FG/SOT (Hinode)
- Spatially resolved vertical vorticity in solar supergranulation using helioseismology and local correlation tracking
- The Solar Internetwork. II. Magnetic Flux Appearance and Disappearance Rates
- Solar supergranulation revealed by granule tracking
- Quasi full-disk maps of solar horizontal velocities using SDO/HMI data
- Diffusion of magnetic elements in a supergranular cell
- Persistent magnetic vortex flow at a supergranular vertex
- Supergranulation and multiscale flows in the solar photosphere: Global observations vs. a theory of anisotropic turbulent convection
- Relation between trees of fragmenting granules and supergranulation evolution
- Pair separation of magnetic elements in the quiet Sun
- Comparison of solar surface flows inferred from time--distance helioseismology and coherent structure tracking using HMI/SDO observations
- The Intensity Profile of the Solar Supergranulation
- Comparison of solar horizontal velocity fields from SDO/HMI and Hinode data
- Mesoscale dynamics on the Sun's surface from HINODE observations
- Large-scale photospheric motions determined from granule tracking and helioseismology from SDO/HMI data
- Evolution and wave-like properties of the average solar supergranule
- Horizontal photospheric flows trigger a filament eruption
- Relationship between supergranulation flows, magnetic cancellation and network flares
- Anisotropy of the solar network magnetic field around the average supergranule
- Magnetic pattern at supergranulation scale: the Void Size Distribution
- Occurrence and persistence of magnetic elements in the quiet Sun
- Evolution of exploding granules from coordinated observations by THEMIS, IRIS, SDO/HMI, and HINODE, and a simulation
- Synchronization of Small-scale Magnetic Features, Blinkers, and Coronal Bright Points
- Intensity contrast of the average supergranule
- Photospheric downflows observed with SDO/HMI, HINODE, and an MHD simulation
- Evolution of photospheric flows under an erupting filament in the quiet-Sun region