Artist interpretation of flying by the Earth, Sun and Heliopause.
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This movie shows the particle flow around the Earth as the CME strikes.
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Exactly where the solar wind transitions from a rotational flow to a perfectly radial flow has implications for how the Sun sheds energy. NASA's Parker Solar Probe located a transition region in the solar wind's flow that point may help us better understand the lifecycle of other stars or the formation of protoplanetary disks, the dense disks of gas and dust around young stars that eventually coalesce into planets.
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Observed near Earth, the solar wind is a relatively uniform flow of plasma, with occasional turbulent tumbles. But by that point it’s traveled over ninety million miles — and the signatures of the Sun's exact mechanisms for heating and accelerating the solar wind are wiped out. Closer to the solar wind's source, NASA's Parker Solar Probe saw a much different picture: a complicated, active system.
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This animation shows energetic particles from the Sun interacting with Earth’s magnetic field, called the magnetosphere. The magnetosphere is another one of Earth’s fundamental global fields. It originates from the churning of hot, liquid metals in our planet’s core and extends thousands of miles out into space. Our magnetosphere protects us from much of the radiation we encounter in the universe, including the Sun’s energetic particles (shown here coming from the left side of the animation). When these particles run into the magnetosphere, they tend to flow around it like air deflected by the nose of a supersonic jet.
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Our magnetosphere protects us from much of the radiation we encounter in the universe, including the Sun’s energetic particles (shown here coming from the left side of the animation). When these particles run into the magnetosphere, they tend to flow around it like air deflected by the nose of a supersonic jet.Credit: NASA Goddard/CIL/Wes Buchanan, Krystofer Kim", "width": 3840, "height": 2160, "pixels": 8294400 } }, { "id": 491121, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 1158030, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a014800/a014892/14892_Endurance_SEQ3B_4K.mov", "filename": "14892_Endurance_SEQ3B_4K.mov", "media_type": "Movie", "alt_text": "Conceptual AnimationThis animation shows energetic particles from the Sun interacting with Earth’s magnetic field, called the magnetosphere. The magnetosphere is another one of Earth’s fundamental global fields. It originates from the churning of hot, liquid metals in our planet’s core and extends thousands of miles out into space. Our magnetosphere protects us from much of the radiation we encounter in the universe, including the Sun’s energetic particles (shown here coming from the left side of the animation). When these particles run into the magnetosphere, they tend to flow around it like air deflected by the nose of a supersonic jet.Credit: NASA Goddard/CIL/Wes Buchanan, Krystofer Kim", "width": 3840, "height": 2160, "pixels": 8294400 } } ], "extra_data": {} }, { "id": 378817, "url": "https://svs.gsfc.nasa.gov/14892/#media_group_378817", "widget": "Video player", "title": "", "caption": "", "description": "Conceptual Animation
This artist’s concept shows Earth’s magnetosphere immersed in the so-called “fast” solar wind, which averages between about 300 - 500 miles per second (approx. 500 - 800 kilometers per second). The fast solar wind originates from coronal holes: darker, lower density patches of the Sun’s atmosphere where the Sun’s magnetic field lines connect to interplanetary space, allowing solar material to escape out in a high-speed stream. Coronal holes are more common closer to the Sun’s poles but can occasionally appear on any area of the Sun. When a fast stream of solar wind reaches Earth, it can compress Earth’s magnetosphere like a windsock blowing in the wind.
Credit: NASA Goddard/CIL/Bailee DesRocher", "items": [ { "id": 491147, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 1158056, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a014800/a014892/14892_H_VC_Animation_fast_loop_4K_ProRes.00001_print.jpg", "filename": "14892_H_VC_Animation_fast_loop_4K_ProRes.00001_print.jpg", "media_type": "Image", "alt_text": "Conceptual AnimationThis artist’s concept shows Earth’s magnetosphere immersed in the so-called “fast” solar wind, which averages between about 300 - 500 miles per second (approx. 500 - 800 kilometers per second). The fast solar wind originates from coronal holes: darker, lower density patches of the Sun’s atmosphere where the Sun’s magnetic field lines connect to interplanetary space, allowing solar material to escape out in a high-speed stream. Coronal holes are more common closer to the Sun’s poles but can occasionally appear on any area of the Sun. When a fast stream of solar wind reaches Earth, it can compress Earth’s magnetosphere like a windsock blowing in the wind.Credit: NASA Goddard/CIL/Bailee DesRocher", "width": 1024, "height": 576, "pixels": 589824 } }, { "id": 491148, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 1158057, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a014800/a014892/14892_H_VC_Animation_fast_loop_4K_ProRes.00001_web.png", "filename": "14892_H_VC_Animation_fast_loop_4K_ProRes.00001_web.png", "media_type": "Image", "alt_text": "Conceptual AnimationThis artist’s concept shows Earth’s magnetosphere immersed in the so-called “fast” solar wind, which averages between about 300 - 500 miles per second (approx. 500 - 800 kilometers per second). The fast solar wind originates from coronal holes: darker, lower density patches of the Sun’s atmosphere where the Sun’s magnetic field lines connect to interplanetary space, allowing solar material to escape out in a high-speed stream. Coronal holes are more common closer to the Sun’s poles but can occasionally appear on any area of the Sun. When a fast stream of solar wind reaches Earth, it can compress Earth’s magnetosphere like a windsock blowing in the wind.Credit: NASA Goddard/CIL/Bailee DesRocher", "width": 320, "height": 180, "pixels": 57600 } }, { "id": 491149, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 1158058, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a014800/a014892/14892_H_VC_Animation_fast_loop_4K_ProRes.00001_thm.png", "filename": "14892_H_VC_Animation_fast_loop_4K_ProRes.00001_thm.png", "media_type": "Image", "alt_text": "Conceptual AnimationThis artist’s concept shows Earth’s magnetosphere immersed in the so-called “fast” solar wind, which averages between about 300 - 500 miles per second (approx. 500 - 800 kilometers per second). The fast solar wind originates from coronal holes: darker, lower density patches of the Sun’s atmosphere where the Sun’s magnetic field lines connect to interplanetary space, allowing solar material to escape out in a high-speed stream. Coronal holes are more common closer to the Sun’s poles but can occasionally appear on any area of the Sun. When a fast stream of solar wind reaches Earth, it can compress Earth’s magnetosphere like a windsock blowing in the wind.Credit: NASA Goddard/CIL/Bailee DesRocher", "width": 80, "height": 40, "pixels": 3200 } }, { "id": 491123, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 1158032, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a014800/a014892/14892_H_VC_Animation_fast_loop_v01_4K.mp4", "filename": "14892_H_VC_Animation_fast_loop_v01_4K.mp4", "media_type": "Movie", "alt_text": "Conceptual AnimationThis artist’s concept shows Earth’s magnetosphere immersed in the so-called “fast” solar wind, which averages between about 300 - 500 miles per second (approx. 500 - 800 kilometers per second). The fast solar wind originates from coronal holes: darker, lower density patches of the Sun’s atmosphere where the Sun’s magnetic field lines connect to interplanetary space, allowing solar material to escape out in a high-speed stream. Coronal holes are more common closer to the Sun’s poles but can occasionally appear on any area of the Sun. When a fast stream of solar wind reaches Earth, it can compress Earth’s magnetosphere like a windsock blowing in the wind.Credit: NASA Goddard/CIL/Bailee DesRocher", "width": 3840, "height": 2160, "pixels": 8294400 } }, { "id": 491158, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 1158067, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a014800/a014892/14892_H_VC_Animation_fast_loop_4K_ProRes.webm", "filename": "14892_H_VC_Animation_fast_loop_4K_ProRes.webm", "media_type": "Movie", "alt_text": "Conceptual AnimationThis artist’s concept shows Earth’s magnetosphere immersed in the so-called “fast” solar wind, which averages between about 300 - 500 miles per second (approx. 500 - 800 kilometers per second). The fast solar wind originates from coronal holes: darker, lower density patches of the Sun’s atmosphere where the Sun’s magnetic field lines connect to interplanetary space, allowing solar material to escape out in a high-speed stream. Coronal holes are more common closer to the Sun’s poles but can occasionally appear on any area of the Sun. When a fast stream of solar wind reaches Earth, it can compress Earth’s magnetosphere like a windsock blowing in the wind.Credit: NASA Goddard/CIL/Bailee DesRocher", "width": 3840, "height": 2160, "pixels": 8294400 } }, { "id": 491122, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 1158031, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a014800/a014892/14892_H_VC_Animation_fast_loop_4K_ProRes.mov", "filename": "14892_H_VC_Animation_fast_loop_4K_ProRes.mov", "media_type": "Movie", "alt_text": "Conceptual AnimationThis artist’s concept shows Earth’s magnetosphere immersed in the so-called “fast” solar wind, which averages between about 300 - 500 miles per second (approx. 500 - 800 kilometers per second). The fast solar wind originates from coronal holes: darker, lower density patches of the Sun’s atmosphere where the Sun’s magnetic field lines connect to interplanetary space, allowing solar material to escape out in a high-speed stream. Coronal holes are more common closer to the Sun’s poles but can occasionally appear on any area of the Sun. When a fast stream of solar wind reaches Earth, it can compress Earth’s magnetosphere like a windsock blowing in the wind.Credit: NASA Goddard/CIL/Bailee DesRocher", "width": 3840, "height": 2160, "pixels": 8294400 } } ], "extra_data": {} }, { "id": 378818, "url": "https://svs.gsfc.nasa.gov/14892/#media_group_378818", "widget": "Video player", "title": "", "caption": "", "description": "Conceptual Animation
This artist’s concept shows a representative state of Earth’s magnetosphere immersed in the so-called “slow” solar wind, which averages between about 180 - 300 miles per second (approx. 300 - 500 kilometers per second). The slow solar wind originates from coronal streamers and other solar features most commonly found around the Sun’s equator, which make the slow solar wind the typical state of the solar wind along the equatorial plane in which the planets orbit.
Credit: NASA Goddard/CIL/Bailee DesRocher", "items": [ { "id": 491150, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 1158059, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a014800/a014892/14892_H_VC_Animation_slow_loop_v01_4K_ProRes.00001_print.jpg", "filename": "14892_H_VC_Animation_slow_loop_v01_4K_ProRes.00001_print.jpg", "media_type": "Image", "alt_text": "Conceptual AnimationThis artist’s concept shows a representative state of Earth’s magnetosphere immersed in the so-called “slow” solar wind, which averages between about 180 - 300 miles per second (approx. 300 - 500 kilometers per second). The slow solar wind originates from coronal streamers and other solar features most commonly found around the Sun’s equator, which make the slow solar wind the typical state of the solar wind along the equatorial plane in which the planets orbit.Credit: NASA Goddard/CIL/Bailee DesRocher", "width": 1024, "height": 576, "pixels": 589824 } }, { "id": 491151, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 1158060, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a014800/a014892/14892_H_VC_Animation_slow_loop_v01_4K_ProRes.00001_web.png", "filename": "14892_H_VC_Animation_slow_loop_v01_4K_ProRes.00001_web.png", "media_type": "Image", "alt_text": "Conceptual AnimationThis artist’s concept shows a representative state of Earth’s magnetosphere immersed in the so-called “slow” solar wind, which averages between about 180 - 300 miles per second (approx. 300 - 500 kilometers per second). The slow solar wind originates from coronal streamers and other solar features most commonly found around the Sun’s equator, which make the slow solar wind the typical state of the solar wind along the equatorial plane in which the planets orbit.Credit: NASA Goddard/CIL/Bailee DesRocher", "width": 320, "height": 180, "pixels": 57600 } }, { "id": 491152, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 1158061, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a014800/a014892/14892_H_VC_Animation_slow_loop_v01_4K_ProRes.00001_thm.png", "filename": "14892_H_VC_Animation_slow_loop_v01_4K_ProRes.00001_thm.png", "media_type": "Image", "alt_text": "Conceptual AnimationThis artist’s concept shows a representative state of Earth’s magnetosphere immersed in the so-called “slow” solar wind, which averages between about 180 - 300 miles per second (approx. 300 - 500 kilometers per second). The slow solar wind originates from coronal streamers and other solar features most commonly found around the Sun’s equator, which make the slow solar wind the typical state of the solar wind along the equatorial plane in which the planets orbit.Credit: NASA Goddard/CIL/Bailee DesRocher", "width": 80, "height": 40, "pixels": 3200 } }, { "id": 491124, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 1158033, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a014800/a014892/14892_H_VC_Animation_slow_loop_v01_4K.mp4", "filename": "14892_H_VC_Animation_slow_loop_v01_4K.mp4", "media_type": "Movie", "alt_text": "Conceptual AnimationThis artist’s concept shows a representative state of Earth’s magnetosphere immersed in the so-called “slow” solar wind, which averages between about 180 - 300 miles per second (approx. 300 - 500 kilometers per second). The slow solar wind originates from coronal streamers and other solar features most commonly found around the Sun’s equator, which make the slow solar wind the typical state of the solar wind along the equatorial plane in which the planets orbit.Credit: NASA Goddard/CIL/Bailee DesRocher", "width": 3840, "height": 2160, "pixels": 8294400 } }, { "id": 491159, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 1158068, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a014800/a014892/14892_H_VC_Animation_slow_loop_v01_4K_ProRes.webm", "filename": "14892_H_VC_Animation_slow_loop_v01_4K_ProRes.webm", "media_type": "Movie", "alt_text": "Conceptual AnimationThis artist’s concept shows a representative state of Earth’s magnetosphere immersed in the so-called “slow” solar wind, which averages between about 180 - 300 miles per second (approx. 300 - 500 kilometers per second). The slow solar wind originates from coronal streamers and other solar features most commonly found around the Sun’s equator, which make the slow solar wind the typical state of the solar wind along the equatorial plane in which the planets orbit.Credit: NASA Goddard/CIL/Bailee DesRocher", "width": 3840, "height": 2160, "pixels": 8294400 } }, { "id": 491125, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 1158034, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a014800/a014892/14892_H_VC_Animation_slow_loop_v01_4K_ProRes.mov", "filename": "14892_H_VC_Animation_slow_loop_v01_4K_ProRes.mov", "media_type": "Movie", "alt_text": "Conceptual AnimationThis artist’s concept shows a representative state of Earth’s magnetosphere immersed in the so-called “slow” solar wind, which averages between about 180 - 300 miles per second (approx. 300 - 500 kilometers per second). The slow solar wind originates from coronal streamers and other solar features most commonly found around the Sun’s equator, which make the slow solar wind the typical state of the solar wind along the equatorial plane in which the planets orbit.Credit: NASA Goddard/CIL/Bailee DesRocher", "width": 3840, "height": 2160, "pixels": 8294400 } } ], "extra_data": {} }, { "id": 378819, "url": "https://svs.gsfc.nasa.gov/14892/#media_group_378819", "widget": "Video player", "title": "", "caption": "", "description": "Conceptual Animation
A conceptual animation showing solar wind interacting with Earth's magnetic field and causing atmospheric loss at the polar cusps.
Credit: NASA Goddard/CIL/Josh Masters", "items": [ { "id": 491153, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 1158062, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a014800/a014892/14892_Atmospheric_Escape_4K_ProRes.00001_print.jpg", "filename": "14892_Atmospheric_Escape_4K_ProRes.00001_print.jpg", "media_type": "Image", "alt_text": "Conceptual AnimationA conceptual animation showing solar wind interacting with Earth's magnetic field and causing atmospheric loss at the polar cusps.Credit: NASA Goddard/CIL/Josh Masters", "width": 1024, "height": 576, "pixels": 589824 } }, { "id": 491154, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 1158063, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a014800/a014892/14892_Atmospheric_Escape_4K_ProRes.00001_web.png", "filename": "14892_Atmospheric_Escape_4K_ProRes.00001_web.png", "media_type": "Image", "alt_text": "Conceptual AnimationA conceptual animation showing solar wind interacting with Earth's magnetic field and causing atmospheric loss at the polar cusps.Credit: NASA Goddard/CIL/Josh Masters", "width": 320, "height": 180, "pixels": 57600 } }, { "id": 491155, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 1158064, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a014800/a014892/14892_Atmospheric_Escape_4K_ProRes.00001_thm.png", "filename": "14892_Atmospheric_Escape_4K_ProRes.00001_thm.png", "media_type": "Image", "alt_text": "Conceptual AnimationA conceptual animation showing solar wind interacting with Earth's magnetic field and causing atmospheric loss at the polar cusps.Credit: NASA Goddard/CIL/Josh Masters", "width": 80, "height": 40, "pixels": 3200 } }, { "id": 491126, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 1158035, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a014800/a014892/14892_Atmospheric_Escape_1080.mp4", "filename": "14892_Atmospheric_Escape_1080.mp4", "media_type": "Movie", "alt_text": "Conceptual AnimationA conceptual animation showing solar wind interacting with Earth's magnetic field and causing atmospheric loss at the polar cusps.Credit: NASA Goddard/CIL/Josh Masters", "width": 1920, "height": 1080, "pixels": 2073600 } }, { "id": 491160, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 1158069, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a014800/a014892/14892_Atmospheric_Escape_4K_ProRes.webm", "filename": "14892_Atmospheric_Escape_4K_ProRes.webm", "media_type": "Movie", "alt_text": "Conceptual AnimationA conceptual animation showing solar wind interacting with Earth's magnetic field and causing atmospheric loss at the polar cusps.Credit: NASA Goddard/CIL/Josh Masters", "width": 3840, "height": 2160, "pixels": 8294400 } }, { "id": 491127, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 1158036, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a014800/a014892/14892_Atmospheric_Escape_4K.mp4", "filename": "14892_Atmospheric_Escape_4K.mp4", "media_type": "Movie", "alt_text": "Conceptual AnimationA conceptual animation showing solar wind interacting with Earth's magnetic field and causing atmospheric loss at the polar cusps.Credit: NASA Goddard/CIL/Josh Masters", "width": 3840, "height": 2160, "pixels": 8294400 } }, { "id": 491128, "type": "media", "extra_data": null, "title": null, "caption": null, "instance": { "id": 1158037, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a014800/a014892/14892_Atmospheric_Escape_4K_ProRes.mov", "filename": "14892_Atmospheric_Escape_4K_ProRes.mov", "media_type": "Movie", "alt_text": "Conceptual AnimationA conceptual animation showing solar wind interacting with Earth's magnetic field and causing atmospheric loss at the polar cusps.Credit: NASA Goddard/CIL/Josh Masters", "width": 3840, "height": 2160, "pixels": 8294400 } } ], "extra_data": {} } ], "studio": "gms", "funding_sources": [ "PAO" ], "credits": [ { "role": "Producer", "people": [ { "name": "Lacey Young", "employer": "eMITS" } ] } ], "missions": [], "series": [], "tapes": [], "papers": [], "datasets": [], "nasa_science_categories": [ "Sun" ], "keywords": [ "Corona", "Earth", "Magnetic Fields", "Magnetosphere", "Plasma", "Solar Wind", "Space Weather" ], "recommended_pages": [], "related": [ { "id": 14956, "url": "https://svs.gsfc.nasa.gov/14956/", "page_type": "Produced Video", "title": "Space Weather Effects Animations", "description": "Solar flares, coronal mass ejections, solar particle events, and the solar wind form the recipe for space weather that affects life on Earth and astronauts in space. A farmer stops their planting operations due to poor GPS signal for their autonomous tractor. A power grid manager changes the configuration of their network to ensure a blackout doesn’t occur due to voltage instability. A pilot switches to back-up communication equipment due to loss of high-frequency radio. A commercial internet company providing service to the military must change the orbit of their spacecraft to avoid a collision due to increased atmospheric drag.These are a few examples of the ways the Sun influences our everyday lives. This is what we define as space weather – the conditions of the space environment driven by the Sun and it’s impacts on objects in the solar system. Learn more about space weather: https://science.nasa.gov/space-weather-2/ || ", "release_date": "2026-01-26T16:00:00-05:00", "update_date": "2026-01-27T10:11:45-05:00", "main_image": { "id": 1196084, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a014900/a014956/14956_SatelliteImpact01_4K_ProRes.00001_print.jpg", "filename": "14956_SatelliteImpact01_4K_ProRes.00001_print.jpg", "media_type": "Image", "alt_text": "AnimationSpace weather impacting a satellite with Earth seen in the background.Credit: NASA", "width": 1024, "height": 576, "pixels": 589824 } }, { "id": 14683, "url": "https://svs.gsfc.nasa.gov/14683/", "page_type": "Produced Video", "title": "NASA, NOAA Announce That the Sun Has Reached the Solar Maximum Period", "description": "In a teleconference with reporters on Tuesday, October 15, 2024, representatives from NASA, the National Oceanic and Atmospheric Agency (NOAA), and the Solar Cycle Prediction Panel announced the Sun has reached its solar maximum period.The solar cycle is the natural cycle of the Sun as it transitions between low and high activity. Roughly every 11 years, at the height of the solar cycle, the Sun’s magnetic poles flip — on Earth, that’d be like the North and South Poles swapping places every decade — and the Sun transitions from sluggish to active and stormy.During the most active part of the cycle, known as solar maximum, the Sun can unleash immense explosions of light, energy, and solar radiation — all of which create conditions known as space weather. Space weather can affect satellites and astronauts in space, as well as communications systems — such as radio and GPS — and power grids on Earth. When the Sun is most active, space weather events become more frequent. Solar activity, such as the storm in May 2024, has led to increased aurora visibility and impacts on satellites and infrastructure in recent months.Listen to the media telecon.Read NASA's article about the news. || ", "release_date": "2024-10-15T13:30:00-04:00", "update_date": "2025-02-28T14:02:15.113776-05:00", "main_image": { "id": 1098353, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a014600/a014683/001_Sun_Comparison.00001_print.jpg", "filename": "001_Sun_Comparison.00001_print.jpg", "media_type": "Image", "alt_text": "1. VideoImages from NASA’s Solar Dynamics Observatory highlight the appearance of the Sun at solar minimum (left, Dec. 2019) versus solar maximum (right, May 2024). These images are in the 171 wavelength of extreme ultraviolet light, which reveals the active regions on the Sun that are more common during solar maximum.Credit: NASA/SDO ", "width": 1024, "height": 576, "pixels": 589824 } }, { "id": 14628, "url": "https://svs.gsfc.nasa.gov/14628/", "page_type": "Produced Video", "title": "Discovering Earth’s Third Global Energy Field", "description": "High above the Earth’s North and South Poles, a steady stream of particles escapes from our atmosphere into space. Scientists call this mysterious outflow the “polar wind,” and for almost 60 years, spacecraft have been flying through it as scientists have theorized about its cause. The leading theory was that a planet-wide electric field was drawing those particles up into space. But this so-called ambipolar electric field, if it exists, is so weak that all attempts to measure it have failed – until now.In 2022, scientists traveled to Svalbard, a small archipelago in Norway, to launch a rocket in an attempt to measure Earth’s ambipolar electric field for the first time. This was NASA’s Endurance rocketship mission, and this is its story.To learn more, visit: https://science.nasa.gov/science-research/heliophysics/nasa-discovers-long-sought-global-electric-field-on-earth/ || ", "release_date": "2024-08-28T11:30:00-04:00", "update_date": "2024-08-28T11:37:52.179001-04:00", "main_image": { "id": 1096850, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a014600/a014628/Thumbnail02.jpg", "filename": "Thumbnail02.jpg", "media_type": "Image", "alt_text": "Discovering Earth's Third Global Energy FieldWatch this video on the NASA Goddard YouTube channel.Complete transcript available.Music credit: \"Atoms in Motion\" by Phillip John Gregory [PRS], “Curious By Nature” by Eddie Saffron [PRS], “Perfect Vibes” by Thomas Gallicani [SACEM], “Natural Response” by Jonathan Elisa [ASCAP] and Sarah Trevino [ASCAP] from Universal Production MusicSound effects: Pixabay", "width": 1280, "height": 720, "pixels": 921600 } }, { "id": 20347, "url": "https://svs.gsfc.nasa.gov/20347/", "page_type": "Animation", "title": "Fast and Slow Solar Wind", "description": "These animations show how Earth’s magnetosphere responds as it encounters the slow and fast solar wind.The solar wind is a plasma made of ions and electrons that have escaped the Sun. The solar wind streams outwards in all directions, filling the spaces between the planets and carrying with it the Sun’s magnetic field. When the solar wind reaches Earth’s magnetosphere, the region of space surrounding our planet where Earth’s magnetic field is dominant, the magnetosphere can respond differently depending on the speed of the solar wind, as demonstrated here. || ", "release_date": "2021-09-28T00:00:00-04:00", "update_date": "2021-09-21T23:00:13.808436-04:00", "main_image": { "id": 376605, "url": "https://svs.gsfc.nasa.gov/vis/a020000/a020300/a020347/H_VC_Animation_slow_loop_v01.00010_print.jpg", "filename": "H_VC_Animation_slow_loop_v01.00010_print.jpg", "media_type": "Image", "alt_text": "This artist’s concept shows a representative state of Earth’s magnetosphere immersed in the so-called “slow” solar wind, which averages between about 180 - 300 miles per second (approx. 300 - 500 kilometers per second). The slow solar wind originates from coronal streamers and other solar features most commonly found around the Sun’s equator, which make the slow solar wind the typical state of the solar wind along the equatorial plane in which the planets orbit.", "width": 1024, "height": 576, "pixels": 589824 } }, { "id": 13506, "url": "https://svs.gsfc.nasa.gov/13506/", "page_type": "Produced Video", "title": "Solar Wind Interacting with Earth's Magnetic Field", "description": "A conceptual animation showing solar wind interacting with Earth's magnetic field and causing atmospheric loss at the polar cusps. || YOUTUBE_1080_13506_Atmospheric_Escape_youtube_1080.00001_print.jpg (1024x576) [77.5 KB] || YOUTUBE_1080_13506_Atmospheric_Escape_youtube_1080.00001_searchweb.png (320x180) [74.4 KB] || YOUTUBE_1080_13506_Atmospheric_Escape_youtube_1080.00001_web.png (320x180) [74.4 KB] || YOUTUBE_1080_13506_Atmospheric_Escape_youtube_1080.00001_thm.png (80x40) [6.3 KB] || YOUTUBE_1080_13506_Atmospheric_Escape_youtube_1080.mp4 (1920x1080) [43.1 MB] || FACEBOOK_720_13506_Atmospheric_Escape_facebook_720.mp4 (1280x720) [32.8 MB] || TWITTER_720_13506_Atmospheric_Escape_twitter_720.mp4 (1280x720) [5.7 MB] || FACEBOOK_720_13506_Atmospheric_Escape_facebook_720.webm (1280x720) [3.0 MB] || PRORES_B-ROLL_13506_Atmospheric_Escape_prores_b-roll.mov (1280x720) [227.8 MB] || YOUTUBE_4K_13506_Atmospheric_Escape_youtube_4k.mp4 (3840x2160) [187.6 MB] || 13506_Atmospheric_Escape_Prores.mov (3840x2160) [2.4 GB] || ", "release_date": "2019-12-20T17:00:00-05:00", "update_date": "2023-05-03T13:45:18.835555-04:00", "main_image": { "id": 388639, "url": "https://svs.gsfc.nasa.gov/vis/a010000/a013500/a013506/YOUTUBE_4K_13506_Cusp+Aurora_youtube_4k.00001_print.jpg", "filename": "YOUTUBE_4K_13506_Cusp+Aurora_youtube_4k.00001_print.jpg", "media_type": "Image", "alt_text": "A conceptual animation showing Earth's polar cusps and the cusp aurora. ", "width": 1024, "height": 576, "pixels": 589824 } }, { "id": 20299, "url": "https://svs.gsfc.nasa.gov/20299/", "page_type": "Animation", "title": "Parker Science Result animations", "description": "On Dec. 4, 2019, four new papers in the journal Nature describe what scientists working with data from NASA's Parker Solar Probe have learned from this unprecedented exploration of our star — and what they look forward to learning next. These findings reveal new information about the behavior of the material and particles that speed away from the Sun, bringing scientists closer to answering fundamental questions about the physics of our star. These animations represent five of those findings. || ", "release_date": "2019-12-04T13:00:00-05:00", "update_date": "2025-03-16T23:28:24.418035-04:00", "main_image": { "id": 392323, "url": "https://svs.gsfc.nasa.gov/vis/a020000/a020200/a020299/SwitchbackSun_4k_0000_print.jpg", "filename": "SwitchbackSun_4k_0000_print.jpg", "media_type": "Image", "alt_text": "Top-down view of Switchback Magnetic FieldsParker indicated that the solar magnetic field embedded in the solar wind flips in the direction. These reversals — dubbed \"switchbacks\" — last anywhere from a few seconds to several minutes as they flow over Parker Solar Probe. During a switchback, the magnetic field whips back on itself until it is pointed almost directly back at the Sun.Credit: NASA Goddard/CIL/Adriana Manrique Gutierrez", "width": 1024, "height": 576, "pixels": 589824 } }, { "id": 3902, "url": "https://svs.gsfc.nasa.gov/3902/", "page_type": "Visualization", "title": "A Coronal Mass Ejection strikes the Earth!", "description": "Energetic events on the Sun have impacts throughout the Solar System. This visualization, developed for the Dynamic Earth dome show, utilizes data from space weather models based on a real coronal mass ejection (CME) event from mid-December 2003. Particles are used to represent the flow of solar material from the Sun around the Earth. It is important to note that the flowing material of the CME are actually ions and electrons far too small to see. This visualization tries to represent the motions of these tiny particles in a form large enough for us to see. We open with a close-up view of the Earth, the particles representing the solar wind streaming around the Earth due to extended influence of the Earth's magnetic field. We pull out from the Earth and move so that we see the Sun in the distance. The enormous density enhancement in the solar wind is the coronal mass ejection. As the CME reaches the Earth, we see how effective the Earth's magnetic field is at diverting the solar material around the Earth. As the CME passes, we move earthward, and reveal the field lines representing the Earth's magnetic field, emanating from the magnetic poles and blown behind the Earth due to the influence of the solar wind. For simplicity, we have represented the Earth's magnetic field as unchanging, but it is actually very dynamic in its response to a CME or other change in the solar wind. || ", "release_date": "2012-01-24T00:00:00-05:00", "update_date": "2023-05-03T13:53:19.014318-04:00", "main_image": { "id": 485540, "url": "https://svs.gsfc.nasa.gov/vis/a000000/a003900/a003902/cme.00600_web.png", "filename": "cme.00600_web.png", "media_type": "Image", "alt_text": "This movie shows the particle flow around the Earth as the CME strikes.", "width": 320, "height": 180, "pixels": 57600 } } ], "sources": [], "products": [], "newer_versions": [], "older_versions": [], "alternate_versions": [] }