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| Solar Wind (astronomy) | |
|---|---|
| Name | Solar Wind |
| Type | Stellar wind |
Solar Wind (astronomy) The solar wind is a continuous outflow of plasma from the outer atmosphere of the Sun that shapes the near-Earth environment and the heliosphere. It links phenomena on the Sun with space weather effects at Earth, other planets such as Mars, and spacecraft in interplanetary space, and it has been studied by missions including Parker Solar Probe and Voyager program.
The solar wind originates in the solar corona and extends outward to form the heliosphere that interacts with planetary magnetospheres such as Magnetosphere of Earth and with bodies like Mercury (planet), Jupiter, and Saturn. Research into the solar wind connects observatories and institutions such as National Aeronautics and Space Administration, European Space Agency, Jet Propulsion Laboratory, and facilities like Mauna Loa Observatory and SOHO. Important related events and missions include the Apollo program, Ulysses (spacecraft), and the Helios (spacecraft) missions.
The solar wind is composed primarily of electrons, protons, and alpha particles, with trace heavy ions such as oxygen and iron that reveal coronal source characteristics measured by instruments aboard ACE (spacecraft), Wind (spacecraft), and Hinode. Typical speeds range from slow (~300–500 km/s) associated with the Heliospheric current sheet to fast (~600–800 km/s) tied to open-field regions such as coronal holes identified by Solar Dynamics Observatory and Yohkoh. The plasma carries the interplanetary magnetic field, a spiral structure shaped by solar rotation first described in the Parker spiral concept; parameters such as density, temperature, and composition vary with solar cycle phases monitored by NOAA and Space Weather Prediction Center datasets.
Coronal holes and active regions on the photosphere produce different wind streams, linking features observed in Mount Wilson Observatory, Big Bear Solar Observatory, and by instruments on STEREO (spacecraft). Acceleration mechanisms invoked in models include thermal pressure gradients from coronal heating studied in the context of the coronal heating problem, wave–particle interactions such as Alfvén wave dissipation explored by researchers at Princeton University and Stanford University, and magnetic reconnection processes observed in events associated with Solar Orbiter and TRACE (spacecraft). The role of plasma turbulence, kinetic instabilities, and pickup ions informs theories developed by groups at Max Planck Institute for Solar System Research, Institut d'Astrophysique de Paris, and Harvard-Smithsonian Center for Astrophysics.
When the solar wind encounters a planetary magnetic field, it produces a bow shock, magnetosheath, and magnetotail as mapped at Earth by missions such as MMS (spacecraft) and Cluster (spacecraft), and at Jupiter by Galileo (spacecraft). At non-magnetized bodies like Mars and Venus, solar wind erosion of atmospheres has been quantified by MAVEN and Venus Express observations. Interactions drive auroral phenomena at polar regions observed by NOAA GOES satellites and ground observatories tied to institutions like University of Alaska Fairbanks. Extreme events linked to the Carrington Event alter radiation environments monitored by operators such as Federal Aviation Administration and agencies in international partnerships including International Space Station mission control centers.
The solar wind sculpts the heliosphere and modulates cosmic ray fluxes measured by the Voyager 1 and Voyager 2 spacecraft near the heliopause. Coronal mass ejections and high-speed streams produce geomagnetic storms that impact infrastructure overseen by organizations like North American Electric Reliability Corporation and services such as Global Positioning System operations. Space weather forecasting integrates data from DSCOVR (spacecraft), ACE, and ground magnetometer networks coordinated by agencies like NOAA and collaborations involving European Organisation for the Exploitation of Meteorological Satellites.
In situ plasma and field measurements come from spacecraft instruments such as ion spectrometers, magnetometers, and energetic particle detectors aboard Parker Solar Probe, Solar Orbiter, Wind, and ACE. Remote sensing of coronal sources uses extreme ultraviolet and X-ray imagers on Solar Dynamics Observatory, coronagraphs on SOHO and polarized brightness measurements from ground-based coronagraphs at Kanzelhöhe Observatory. Radio observations of shock-associated emissions are performed by facilities like LOFAR and the VLA, while laboratory experiments and numerical codes developed at institutions such as Los Alamos National Laboratory and NASA Goddard Space Flight Center support interpretation.
The solar wind concept evolved from early theoretical work by Eugene Parker and observational confirmations from the Luna (spacecraft) era to direct measurements by the Mariner 2 mission. Subsequent advances arose through coordinated missions including Ulysses, Helios, and the Voyager program, with modern high-resolution studies enabled by Parker Solar Probe and Solar Orbiter. Key scientific gatherings hosted by organizations like the American Geophysical Union and European Geosciences Union have facilitated the development of models and international collaborations.