{ "count": 17, "next": null, "previous": null, "results": [ { "id": 40548, "url": "https://svs.gsfc.nasa.gov/gallery/solarand-heliospheric-observatory-soho/", "result_type": "Gallery", "release_date": "2026-03-03T00:00:00-05:00", "title": "SOHO – Solar and Heliospheric Observatory", "description": "Launched in December 1995, the Solar and Heliospheric Observatory (SOHO) is a joint mission between NASA and ESA (European Space Agency) designed to study the Sun inside out. Though its mission was originally scheduled to last until 1998, SOHO continues to collect observations about the Sun’s interior, the solar atmosphere, and the constant stream of solar particles known as the solar wind, adding to scientists' understanding of our closest star and making many new discoveries, including finding more than 5,000 comets.\n\nLearn more: https://science.nasa.gov/mission/soho/", "hits": 496 }, { "id": 40520, "url": "https://svs.gsfc.nasa.gov/gallery/solar-cycle25/", "result_type": "Gallery", "release_date": "2024-06-28T00:00:00-04:00", "title": "Solar Cycle 25", "description": "The Solar Cycle 25 Prediction Panel, an international group of experts co-sponsored by NASA and the National Oceanic and Atmospheric Administration (NOAA), announced that solar minimum occurred in December 2019, marking the start of Solar Cycle 25. Since then, the Sun’s activity has been steadily increasing as it approaches solar maximum — the peak of Solar Cycle 25.A new solar cycle comes roughly every 11 years. Over the course of each cycle, the Sun transitions from relatively calm to active and stormy, and then quiet again. At its peak, the Sun’s magnetic poles flip.Understanding the Sun’s behavior is an important part of life in our solar system. The Sun’s outbursts, including eruptions known as solar flares and coronal mass ejections, can disturb satellites and communication signals traveling around Earth. Scientists study the solar cycle so we can better understand and predict solar activity.", "hits": 569 }, { "id": 14164, "url": "https://svs.gsfc.nasa.gov/14164/", "result_type": "Produced Video", "release_date": "2022-06-07T19:00:00-04:00", "title": "Australia Sounding Rocket Campaign Press Kit", "description": "NASA will launch three suborbital sounding rockets in June and July 2022 from the Arnhem Space Center in Australia’s Northern Territory to conduct astrophysics studies that can only be done from the Southern Hemisphere. The three missions will focus on α Centauri A and B, two of the three-star α Centauri system that are the closest stars to our Sun, and X-rays emanating from the interstellar medium, clouds of gases and particles between stars.The three sounding rocket night-time missions will be launched between June 26 and July 12 on two-stage Black Brant IX sounding rockets, from the Arnhem Space Center, which is owned and operated by Equatorial Launch Australia or ELA. The Arnhem Space Center is a commercial space launch facility, located on the Dhupuma Plateau near Nhulunbuy. The NASA missions will be the first launches from Arnhem.Learn more: Australia Sounding Rocket Fact SheetWatch more: Sounding Rockets: Cutting Edge Science, 15 Minutes at a TimeWhat Is a Sounding Rocket?Riding Along with a NASA Sounding Rocket || ", "hits": 67 }, { "id": 4917, "url": "https://svs.gsfc.nasa.gov/4917/", "result_type": "Visualization", "release_date": "2021-11-29T11:00:00-05:00", "title": "ICON Snaps a Peek at the Ionospheric Dynamo", "description": "Visualization of ICON in Earth orbit, camera ahead of the spacecraft looking back on spacecraft and limb of Earth. Magenta curves are lines of Earth's geomagnetic field. Field-of-view (FOV) of MIGHTI imagers (green frustums) and the longitudinal wind vectors (green arrows) it measures are shown. MIGHTI imagers FOV eventually fades out. Vertical plasma speed (red arrows) is measured at the spacecraft. Magnetic field lines turn yellow as measurements of winds by MIGHT provide a connection to influence the plasma velocity measured at the spacecraft, redirecting the plasma flow from upward to downward. || ICONDataView.ICONSyncView+x_.clockSlate_CRTT.HD1080i.000750_print.jpg (1024x576) [135.0 KB] || ICONDataView.ICONSyncView+x_.clockSlate_CRTT.HD1080i.000750_searchweb.png (320x180) [79.4 KB] || ICONDataView.ICONSyncView+x_.clockSlate_CRTT.HD1080i.000750_thm.png (80x40) [5.7 KB] || ICONSyncView+x (1920x1080) [0 Item(s)] || ICONDataView.ICONSyncView+x.HD1080i_p30.mp4 (1920x1080) [36.4 MB] || ICONDataView.ICONSyncView+x.HD1080i_p30.webm (1920x1080) [5.1 MB] || ICONSyncView+x (3840x2160) [0 Item(s)] || ICONDataView.ICONSyncView+x.2160p30.mp4 (3840x2160) [114.3 MB] || ICONDataView.ICONSyncView+x.HD1080i_p30.mp4.hwshow || ", "hits": 64 }, { "id": 14025, "url": "https://svs.gsfc.nasa.gov/14025/", "result_type": "Produced Video", "release_date": "2021-11-29T11:00:00-05:00", "title": "Strong Winds Power Electric Fields in the Upper Atmosphere", "description": "Using observations from NASA’s ICON mission, scientists presented the first direct measurements of Earth’s long-theorized dynamo on the edge of space: a wind-driven electrical generator that spans the globe 60-plus miles above our heads. The dynamo churns in the ionosphere, the electrically charged boundary between Earth and space. It’s powered by tidal winds in the upper atmosphere that are faster than most hurricanes and rise from the lower atmosphere, creating an electrical environment that can affect satellites and technology on Earth. The new work, published today in Nature Geoscience, improves our understanding of the ionosphere, which helps scientists better predict space weather and protect our technology from its effects.More information: https://www.nasa.gov/feature/goddard/2021/strong-winds-power-electric-fields-in-upper-atmosphere-icon/ || ", "hits": 96 }, { "id": 13776, "url": "https://svs.gsfc.nasa.gov/13776/", "result_type": "Produced Video", "release_date": "2020-12-15T21:00:00-05:00", "title": "2020 AGU Roundtable: What will we learn from Solar Cycle 25?", "description": "Solar Cycle 25 is here, ushering in the next season of space weather from the Sun. As our star’s activity ramps up—a natural part of its roughly 11-year cycle—scientists are eager to test their predictions. In this AGU 2020 media roundtable, scientists will discuss outstanding questions in solar cycle science, what opportunities this new cycle provides researchers, and how we track progress in predictions. || ", "hits": 111 }, { "id": 13007, "url": "https://svs.gsfc.nasa.gov/13007/", "result_type": "Animation", "release_date": "2018-04-11T00:00:00-04:00", "title": "Jupiter Magnetic Tour", "description": "Take a tour of Jupiter's dynamo, the source of its giant magnetic field, in this new global map from the Juno mission. Watch this video on the NASA.gov Video YouTube channel. || JupiterMagneticTourSmall.mp4 (1920x1080) [71.9 MB] || JupiterMagneticTourPreview.jpg (3840x2160) [1.2 MB] || JupiterMagneticTourPreview_searchweb.png (320x180) [57.0 KB] || JupiterMagneticTourPreview_thm.png (80x40) [3.5 KB] || JupiterMagneticTourProRes.webm (960x540) [28.4 MB] || JupiterMagneticTour1080.mp4 (1920x1080) [193.9 MB] || Foreground_Jupiter_Frames (3840x2160) [0 Item(s)] || Background_Star_Frames (3840x2160) [0 Item(s)] || JupiterMagneticTour4k.mp4 (3840x2160) [492.1 MB] || JupiterMagneticTourProRes.mov (3840x2160) [4.1 GB] || ", "hits": 265 }, { "id": 40335, "url": "https://svs.gsfc.nasa.gov/gallery/interfaceto-space/", "result_type": "Gallery", "release_date": "2017-06-23T00:00:00-04:00", "title": "Interface to Space", "description": "The ionosphere is layer of the upper atmosphere (60-1000 km up) where the neutral atoms and molecules of the lower atmosphere transition to the plasma of space.", "hits": 94 }, { "id": 12296, "url": "https://svs.gsfc.nasa.gov/12296/", "result_type": "Produced Video", "release_date": "2016-06-29T09:00:00-04:00", "title": "Exploring Jupiter's Magnetic Field", "description": "NASA is sending the Juno spacecraft to peer beneath the cloudy surface of Jupiter. Juno's twin magnetometers, built at Goddard Space Flight Center, will give scientists their first look at the dynamo that drives Jupiter's vast magnetic field. Watch this video on the NASA Goddard YouTube channel.Complete transcript available. || JupiterMagnetometerPreview.jpg (1920x1080) [591.9 KB] || JupiterMagnetometerPreview_searchweb.png (320x180) [118.7 KB] || JupiterMagnetometerPreview_thm.png (80x40) [8.0 KB] || 12296_Juno_Magnetometer_appletv.m4v (1280x720) [159.8 MB] || WEBM_12296_Juno_Magnetometer_APR.webm (960x540) [124.4 MB] || 12296_Juno_Magnetometer_appletv_subtitles.m4v (1280x720) [159.9 MB] || LARGE_MP4_12296_Juno_Magnetometer_APR_large.mp4 (1920x1080) [311.4 MB] || 12296_Juno_Magnetometer_APR_Output.en_US.srt [6.2 KB] || 12296_Juno_Magnetometer_APR_Output.en_US.vtt [6.2 KB] || 12296_Juno_Magnetometer_ipod_sm.mp4 (320x240) [53.1 MB] || 12296_Juno_Magnetometer_APR.mov (1920x1080) [4.1 GB] || ", "hits": 209 }, { "id": 40223, "url": "https://svs.gsfc.nasa.gov/gallery/heliophysics-education-resources/", "result_type": "Gallery", "release_date": "2015-01-16T00:00:00-05:00", "title": "Heliophysics Education Resources", "description": "Visualizations useful for illustrating key concepts.", "hits": 144 }, { "id": 40051, "url": "https://svs.gsfc.nasa.gov/gallery/solar-cycle/", "result_type": "Gallery", "release_date": "2010-03-08T00:00:00-05:00", "title": "Solar Cycle", "description": "No description available.", "hits": 19 }, { "id": 40062, "url": "https://svs.gsfc.nasa.gov/gallery/computer-modeling/", "result_type": "Gallery", "release_date": "2010-03-08T00:00:00-05:00", "title": "Computer Modeling", "description": "No description available.", "hits": 26 }, { "id": 40052, "url": "https://svs.gsfc.nasa.gov/gallery/sunspots/", "result_type": "Gallery", "release_date": "2010-03-04T00:00:00-05:00", "title": "Sunspots", "description": "Large cooler regions on the solar photosphere where magnetic flux is concentrated.", "hits": 138 }, { "id": 3496, "url": "https://svs.gsfc.nasa.gov/3496/", "result_type": "Visualization", "release_date": "2008-08-19T00:00:00-04:00", "title": "The Solar Dynamo: Plasma Flows", "description": "In this visualization, we illustrate the fluid flows in the Sun which drive the solar magnetic dynamo. The flows can be considered as a combination of two components, a toroidal component and a meridional component. The toroidal flow corresponds to the rotational motion of the Sun. In the cut-away view, this motion is represented by the streaking flow vectors. The color code of the cross-section on the right-hand side illustrates the rotational period of this flow. Here we see that flow near the equator (in violet) takes about 24.5 days to make it all the way around the Sun. As we move to higher latitudes, we see that the flow gets steadily slower, increasing the time it takes to go around the Sun to as much as 34 days (in red) near the poles. A non-uniform fluid flow such as this is known as differential rotation. This motion in the interior can be measured at the solar surface through techniques of helioseismology.Deeper into the Sun, we see the different colors of the outer layers transition to a solid color (olive green). This transition point is called the tachocline. It is the boundary between the outer zone of the Sun where thermal energy is transferred by convection (the convective zone), and the inner region of the Sun where thermal energy is transferred by radiation (the radiative zone). The radiative zone is believed to rotate as a solid body with a period of about 28 days in this model.The yellow and white center in this model represents the solar radiative zone.In the cross-section on the left-side, we represent the other component of the flow, called the meridional flow, which moves plasma between the equator and the polar regions.These flows of solar plasma are used as input data for dynamo modeling (see The Solar Dynamo: Toroidal and Poloidal Fields and The Solar Dynamo: Toroidal and Radial Fields.) || ", "hits": 107 }, { "id": 3521, "url": "https://svs.gsfc.nasa.gov/3521/", "result_type": "Visualization", "release_date": "2008-08-19T00:00:00-04:00", "title": "The Solar Dynamo: Toroidal and Poloidal Magnetic Fields", "description": "Using the solar plasma flows as input (see The Solar Dynamo: Plasma Flows), the equations of magnetohydrodynamics, and 'seeding' the calculations with an initial small magnetic field, one can compute how a magnetic field can grow and be maintained. This is the dynamo process, the net result being that part of the Sun's outflowing thermal convective energy from nuclear processes is used to create the magnetic field.In this view of the solar dynamo mechanism, we examine the evolution of the toroidal magnetic field, the field intensity represented by colors on the right-hand cross-section, and the poloidal magnetic potential field, represented by colors on the left-hand cross-section. The poloidal magnetic potential is a scalar quantity that contains information about the radial and latitudinal magnetic field vectors. To see the radial magnetic field, see The Solar Dynamo: Toroidal and Radial Magnetic Fields.In this visualization, the magnetic field lines (represented by the 'copper wire' structures) are 'snapshots' of the field structure constructed at each time step of the model. These field lines should not be considered as 'moving' or 'stretching' as the model evolves in time. Even this simplified model reproduces a number of characteristics observed in the actual solar magnetic field. Cyclic behavior with oscillations in the magnetic field amplitude.Magnetic regions at the surface migrate from high latitudes towards the equator as the solar cycle progresses. This reproduces the \"Butterfly Diagram\" pattern.Surface magnetic polarities reverse with each cycleBecause this model is axisymmetric, it cannot simulate non-axisymmetric features such as active longitudes. || ", "hits": 219 }, { "id": 3583, "url": "https://svs.gsfc.nasa.gov/3583/", "result_type": "Visualization", "release_date": "2008-08-19T00:00:00-04:00", "title": "The Solar Dynamo: Toroidal and Radial Magnetic Fields", "description": "Using the solar plasma flows as input (see The Solar Dynamo: Plasma Flows), the equations of magnetohydrodynamics, and 'seeding' the calculations with an initial small magnetic field, one can compute how a magnetic field can grow and be maintained. This is the dynamo process, the net result being that part of the Sun's outflowing thermal convective energy from nuclear processes is used to create the magnetic field.In this view of the solar dynamo mechanism, we examine the evolution of the toroidal magnetic field, intensities represented by color on the right-hand cross-section, and the radial magnetic field, represented on the left-hand cross-section. To see the poloidal magnetic vector potential, see The Solar Dynamo: Toroidal and Poloidal Magnetic Fields.In this visualization, the magnetic field lines (represented by the 'copper wire' structures) are 'snapshots' of the field structure constructed at each time step of the model. These field lines should not be considered as 'moving' or 'stretching' as the model evolves in time.Even this simplified model reproduces a number of characteristics observed in the actual solar magnetic field.Cyclic behavior with oscillations in the magnetic field amplitude.Magnetic regions at the surface migrate from high latitudes towards the equator. This reproduces the \"Butterfly Diagram\" pattern.Surface magnetic polarities reverse with each cycleBecause this model is axisymmetric, it cannot simulate non-axisymmetric features such as active longitudes. || ", "hits": 96 }, { "id": 550, "url": "https://svs.gsfc.nasa.gov/550/", "result_type": "Visualization", "release_date": "1999-01-21T12:00:00-05:00", "title": "Solar Dynamo", "description": "A dynamo is a mechanism for a star or planet to create magnetic field. One type of solar dynamo is turbulent convection, which researchers have simulated on a supercomputer. Like soup boiling on a stove, gas at the Sun's surface is heated from the bottom and cooled at the top. Since the gas conducts electricity, these motions produce magnetic fields. || ", "hits": 30 } ] }