ScienceDaily<\/a> article published on November 12, 2026.<\/em><\/p>\n","protected":false},"excerpt":{"rendered":"Chaotic motion of plasma and magnetic fields flowing from the Sun into interplanetary space.<\/p>\n","protected":false},"author":4,"featured_media":0,"menu_order":0,"comment_status":"open","ping_status":"closed","template":"","meta":{"_acf_changed":false,"_yoast_wpseo_metadesc":"Chaotic motion of plasma and magnetic fields flowing from the Sun into interplanetary space.","glosarix_cat":"astronomia","footnotes":""},"glossary-categories":[13716],"glossary-tags":[],"glossary-languages":[],"class_list":["post-341769","glossary","type-glossary","status-publish","hentry","glossary-categories-astronomy"],"post_title":"Solar Wind Turbulence","post_content":"
Description<\/h2>\r\n
Solar wind turbulence is the irregular, multiscale fluctuation of the velocity, density, and magnetic fields of the plasma that the Sun expels into space. These variations arise because the plasma, composed of charged particles, interacts strongly with electromagnetic fields, generating waves and vortices that overlap without an evident deterministic pattern. On large scales the flow behaves like a fluid with current\u2011like and eddy\u2011like structures, while on small scales the dynamics is dominated by interactions of individual particles, where turbulence energy dissipates and heats the plasma. Solar turbulence is characterized by a wide range of eddy sizes, an energy distribution that follows power\u2011law laws, and a high anisotropy with respect to the mean magnetic field.<\/p>\r\n
History<\/h2>\r\n
The first hints of turbulence in the solar wind were detected by space probes in the 1960s, which showed random fluctuations in plasma velocity. Starting in the 1990s, magnetohydrodynamic turbulence theory was adapted to space plasma, allowing description of energy transfer across scales. The Parker Solar Probe, launched in 2018, has provided high\u2011resolution measurements that revealed previously unknown phenomena, such as sudden reversals in the direction of the magnetic field known as \"switchbacks\".<\/p>\r\n
Uses<\/h2>\r\n
In space weather forecasting, understanding solar wind turbulence helps predict the intensity and timing of geomagnetic storms that can affect satellites and power grids. Models that incorporate turbulent dynamics improve estimates of coronal mass ejection propagation and its interaction with Earth\u2019s magnetosphere. In plasma physics, studying this turbulence serves as a natural laboratory for testing theories of energy transfer and dissipation in highly conductive media. Moreover, characterizing turbulence is essential for designing space missions, as it influences radiation levels and the stability of onboard instruments.<\/p>\r\n
Examples<\/h2>\r\n
A probe venturing into the solar wind several million kilometers from the Sun records rapid variations in plasma speed, alternating between fast and slow bursts; this behavior indicates turbulence that redistributes the flow\u2019s energy. In another case, operators of a communications satellite constellation observe radio\u2011signal fluctuations that coincide with increased solar\u2011wind turbulence, forcing them to adjust frequencies to maintain link quality.<\/p>\r\n
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