{ "count": 34, "next": null, "previous": null, "results": [ { "id": 14685, "url": "https://svs.gsfc.nasa.gov/14685/", "result_type": "Produced Video", "release_date": "2024-10-15T15:00:00-04:00", "title": "What is Solar Maximum?", "description": "The Sun is stirring from its latest slumber. As sunspots and flares bubble from the Sun’s surface, representatives from NASA, the National Oceanic and Atmospheric Agency (NOAA), and the Solar Cycle Prediction Panel announced on Tuesday, September 24, 2024, 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. 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. || ", "hits": 359 }, { "id": 5344, "url": "https://svs.gsfc.nasa.gov/5344/", "result_type": "Visualization", "release_date": "2024-10-15T14:00:00-04:00", "title": "Solar Cycle 25 - the Solar Magnetic Field from Solar Minimum to Pole Flip", "description": "One advantage of long-lived missions like Solar Dynamics Observatory (SDO) is the ability to see slow but significant changes over long periods of time.This view from SDO's Helioseismic and Magnetic Imager (HMI) shows the evolution of sunspots on the solar disk starting from solar minimum (around December 2019) and into the maximum solar activity phase. The video ends in September 2024, however this maximum phase is expected to continue into 2025.", "hits": 790 }, { "id": 13714, "url": "https://svs.gsfc.nasa.gov/13714/", "result_type": "Produced Video", "release_date": "2020-09-15T13:00:00-04:00", "title": "Solar Cycle 25 Is Here. NASA, NOAA Scientists Explain What This Means", "description": "Solar Cycle 25 has begun. The Solar Cycle 25 Prediction Panel announced solar minimum occurred in December 2019, marking the transition into a new solar cycle. In a press event, experts from the panel, NASA, and NOAA discussed the analysis and Solar Cycle 25 prediction, and how the rise to the next solar maximum and subsequent upswing in space weather will impact our lives and technology on Earth.A new solar cycle comes roughly every 11 years. Over the course of each cycle, the star transitions from relatively calm to active and stormy, and then quiet again; at its peak, the Sun’s magnetic poles flip. Now that the star has passed solar minimum, scientists expect the Sun will grow increasingly active in the months and years to come.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 the satellites and communications signals traveling around Earth, or one day, Artemis astronauts exploring distant worlds. Scientists study the solar cycle so we can better predict solar activity.Click here for the NOAA press kit.Listen to the media telecon.Participants:• Lisa Upton, Co-chair, Solar Cycle 25 Prediction Panel; Solar Physicist, Space Systems Research Corporation• Doug Biesecker, Solar Physicist, NOAA’s Space Weather Prediction Center; Co-chair, Solar Cycle 25 Prediction Panel• Elsayed Talaat, Director, Office of Projects, Planning and Analysis; NOAA’s Satellite and Information Service • Lika Guhathakurta, Heliophysicist, Heliophysics Division, NASA Headquarters • Jake Bleacher, Chief Exploration Scientist, NASA Human Exploration and Operations Mission Directorate || ", "hits": 234 }, { "id": 13715, "url": "https://svs.gsfc.nasa.gov/13715/", "result_type": "Produced Video", "release_date": "2020-09-15T13:00:00-04:00", "title": "How To Track The Solar Cycle", "description": "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. Now that the star has passed solar minimum, scientists expect the Sun will grow increasingly active in the months and years to come.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 the satellites and communications signals traveling around Earth, or one day, Artemis astronauts exploring distant worlds. Scientists study the solar cycle so we can better predict solar activity. As of 2020, the Sun has begun to shake off the sleep of minimum, which occurred in December 2019, and Solar Cycle 25 is underway. Scientists use several indicators to track solar cycle progress. || ", "hits": 411 }, { "id": 13275, "url": "https://svs.gsfc.nasa.gov/13275/", "result_type": "Produced Video", "release_date": "2019-08-07T11:30:00-04:00", "title": "How NASA Will Protect Astronauts From Space Radiation", "description": "Today, the Apollo-era flares serve as a reminder of the threat of radiation exposure for technology and astronauts in space. Understanding and predicting solar eruptions is crucial for safe space exploration. Almost 50 years since those 1972 storms, the data, technology and resources available to NASA have improved, enabling advancements towards space weather forecasts and astronaut protection — key to NASA’s Artemis program to return astronauts to the Moon.", "hits": 419 }, { "id": 4551, "url": "https://svs.gsfc.nasa.gov/4551/", "result_type": "Visualization", "release_date": "2017-02-11T10:00:00-05:00", "title": "A Solar Cycle from Solar Dynamics Observatory", "description": "4K x 4K imagery from the SDO/HMI instrument. || SolarCycleHMI.02000_print.jpg (1024x1024) [154.4 KB] || SolarCycleHMI.02000_searchweb.png (320x180) [50.4 KB] || SolarCycleHMI.02000_thm.png (80x40) [3.7 KB] || SolarCycleHMI_1024p30.mp4 (1024x1024) [333.3 MB] || SolarCycleHMI_1024p30.webm (1024x1024) [19.2 MB] || Intensity-Frames (4096x4096) [512.0 KB] || Intensity-Time (4096x4096) [512.0 KB] || ", "hits": 57 }, { "id": 12500, "url": "https://svs.gsfc.nasa.gov/12500/", "result_type": "Produced Video", "release_date": "2017-02-11T10:00:00-05:00", "title": "SDO: Year 7", "description": "The Solar Dynamics Observatory, or SDO, has now captured nearly seven years worth of ultra-high resolution solar footage. This time lapse shows that full run from two of SDO's instruments. The large orange sun is visible light captured by the Helioseismic and Magnetic Imager, or HMI. The smaller golden sun is extreme ultraviolet light from the Atmospheric Imaging Assembly, or AIA, and reveals some of the sun's atmosphere, the corona. Both appear at one frame every 12 hours. SDO's nearly unbroken run is now long enough to watch the rise and fall of the current solar cycle. The graph of solar activity shows the sunspot number, a measurement based on the number of individual spots and the number of sunspot groups. In this case, the line represents a smoothed 26-day average to more clearly show the overall trend.Music: \"Web of Intrigue\" from Killer TracksWatch this video on the NASA Goddard YouTube channel.Complete transcript available. || SDO_Year7_Graph_Still.jpg (3840x2160) [1.2 MB] || 12500_SDO_Year_7_Good_H264_1080.m4v (1920x1080) [239.0 MB] || 12500_SDO_Year_7_1080.mov (1920x1080) [366.0 MB] || 12500_SDO_Year_7_FINAL_appletv.m4v (1280x720) [142.4 MB] || 12500_SDO_Year_7_Compatible.m4v (960x540) [98.1 MB] || 12500_SDO_Year_7_FINAL_appletv_subtitles.m4v (1280x720) [142.5 MB] || 12500_SDO_Year_7_Compatible.webm (960x540) [24.9 MB] || 12500_SDO_Year_7_ProRes_3840x2160_2997.mov (3840x2160) [12.1 GB] || 12500_SDO_Year_7_FINAL_youtube_hq.mov (3840x2160) [6.8 GB] || 12500_SDO_Year_7-Good_H264_4K.m4v (3840x2160) [1.1 GB] || 12500_SDO_Year_7_H264_4K.mov (3840x2160) [474.8 MB] || WMV_12500_SDO_Year_7_FINAL_HD.wmv (3840x2160) [2.2 GB] || 12500_SDO_Year_7_SRT_Captions.en_US.srt [1.4 KB] || 12500_SDO_Year_7_SRT_Captions.en_US.vtt [1.4 KB] || ", "hits": 75 }, { "id": 11720, "url": "https://svs.gsfc.nasa.gov/11720/", "result_type": "Produced Video", "release_date": "2014-11-20T00:00:00-05:00", "title": "Sunspot Live Shots 2014", "description": "Canned interviews for Sunspot live shot 11/20/2014 || Alex_Young_Canned_interview_youtube_hq_print.jpg (1024x576) [102.0 KB] || Alex_Young_Canned_interview_youtube_hq_web.png (320x180) [86.5 KB] || Alex_Young_Canned_interview_youtube_hq_thm.png (80x40) [6.8 KB] || Alex_Young_Canned_interview_appletv.m4v (960x540) [86.6 MB] || Alex_Young_Canned_interview_appletv.webmhd.webm (960x540) [40.6 MB] || Alex_Young_Canned_interview_appletv_subtitles.m4v (960x540) [86.7 MB] || Alex_Young_Canned_interview_1280x720.wmv (1280x720) [106.0 MB] || Alex_Young_Canned_interview_youtube_hq.mov (1280x720) [289.0 MB] || Alex_Young_Canned_interview_ipod_lg.m4v (640x360) [34.0 MB] || Alex_Young_Canned_Interview.en_US.srt [4.0 KB] || Alex_Young_Canned_Interview.en_US.vtt [4.0 KB] || Alex_Young_Canned_interview_nasaportal.mov (640x360) [86.1 MB] || Alex_Young_Canned_interview_ipod_sm.mp4 (320x240) [18.0 MB] || Alex_Young_Canned_interview_prores.mov (1280x720) [3.1 GB] || ", "hits": 38 }, { "id": 10804, "url": "https://svs.gsfc.nasa.gov/10804/", "result_type": "Produced Video", "release_date": "2011-10-27T08:00:00-04:00", "title": "The Solar Cycle", "description": "The number of sunspots increases and decreases over time in a regular, approximately 11-year cycle, called the sunspot cycle. The exact length of the cycle can vary. It has been as short as eight years and as long as fourteen, but the number of sunspots always increases over time, and then returns to low again. More sunspots mean increased solar activity, when great blooms of radiation known as solar flares or bursts of solar material known as coronal mass ejections (CMEs) shoot off the sun's surface. The highest number of sun spots in any given cycle is designated \"solar maximum,\" while the lowest number is designated \"solar minimum.\" Each cycle, varies dramatically in intensity, with some solar maxima being so low as to be almost indistinguishable from the preceding minimum. Sunspots are a magnetic phenomenon and the entire sun is magnetized with a north and a south magnetic pole just like a bar magnet. The comparison to a simple bar magnet ends there, however, as the sun's interior is constantly on the move. By tracking sound waves that course through the center of the sun, an area of research known as helioseismology, scientists can gain an understanding of what's deep inside the sun. They have found that the magnetic material inside the sun is constantly stretching, twisting, and crossing as it bubbles up to the surface. The exact pattern of movements is not conclusively mapped out, but over time they eventually lead to the poles reversing completely. The sunspot cycle happens because of this poles flip — north becomes south and south becomes north—approximately every 11 years. Some 11 years later, the poles reverse again back to where they started, making the full solar cycle actually a 22-year phenomenon. The sun behaves similarly over the course of each 11-year cycle no matter which pole is on top, however, so this shorter cycle tends to receive more attention. || ", "hits": 740 }, { "id": 3692, "url": "https://svs.gsfc.nasa.gov/3692/", "result_type": "Visualization", "release_date": "2010-04-21T14:15:00-04:00", "title": "SDO/AIA CME Event of April 8, 2010 (Multiband)", "description": "This is a close-up view of the April 8 CME in ultraviolet light which reveals a wave (darker regions) expanding outward from the flare event. This movie creates a color image by combining filters for 211 Ångstroms (red), 193 Ångstroms (green) and 171 Ångstroms (blue). || ", "hits": 33 }, { "id": 3693, "url": "https://svs.gsfc.nasa.gov/3693/", "result_type": "Visualization", "release_date": "2010-04-21T14:15:00-04:00", "title": "SDO/AIA Zoom-In on Launching Filament (Bands 304, 171, 211)", "description": "As the AIA camera was activated, one of its first views was this fliament launching from the Sun. || ", "hits": 33 }, { "id": 3695, "url": "https://svs.gsfc.nasa.gov/3695/", "result_type": "Visualization", "release_date": "2010-04-21T14:15:00-04:00", "title": "SDO/AIA CME Event of April 8, 2010 Full Disk (Multiband)", "description": "This visualization is a full-disk view of the CME launched from the Sun on April 8, 2010. This is a 3-color image produced by combining three different filters from the AIA instrument: 211 (red), 193 (green), and 171 (blue). || ", "hits": 34 }, { "id": 3696, "url": "https://svs.gsfc.nasa.gov/3696/", "result_type": "Visualization", "release_date": "2010-04-21T14:15:00-04:00", "title": "SDO/HMI Continuum Full Disk View - March 29, 2010", "description": "This early sequence of HMI images from SDO focuses on a large sunspot group of Solar Cycle 24. || ", "hits": 66 }, { "id": 3703, "url": "https://svs.gsfc.nasa.gov/3703/", "result_type": "Visualization", "release_date": "2010-04-21T14:15:00-04:00", "title": "SDO/HMI Continuum Sunspot Closeup - March 29, 2010", "description": "This is a close-up view of a large sunspot group visible as the HMI instrument turned on their imagers. || ", "hits": 38 }, { "id": 3704, "url": "https://svs.gsfc.nasa.gov/3704/", "result_type": "Visualization", "release_date": "2010-04-21T14:15:00-04:00", "title": "SDO/HMI Continuum Sunspot Zoom-in - March 29, 2010", "description": "This is a zoom-in view of a large sunspot group visible as the HMI instrument turned on their imagers. || ", "hits": 32 }, { "id": 3705, "url": "https://svs.gsfc.nasa.gov/3705/", "result_type": "Visualization", "release_date": "2010-04-21T14:15:00-04:00", "title": "SDO/HMI Magnetogram Sunspot Close-Up - March 29, 2010", "description": "This early sequence of images from the HMI imager is processed to reveal the magnetic field structure (magnetogram). White locations represent a positive magnetic field value (north polarity) while black represents a negative magnetic field value (south polarity). Grey is zero magnetic field.This version is a close-up view of a large sunspot group. || ", "hits": 49 }, { "id": 3706, "url": "https://svs.gsfc.nasa.gov/3706/", "result_type": "Visualization", "release_date": "2010-04-21T14:15:00-04:00", "title": "SDO/HMI Magnetogram Sunspot Zoom-In - March 29, 2010", "description": "This early sequence of images from the HMI imager is processed to reveal the magnetic field structure (magnetogram). White locations represent a positive magnetic field value (north polarity) while black represents a negative magnetic field value (south polarity). Grey is zero magnetic field.This movie zooms-in on a large sunspot group. || ", "hits": 20 }, { "id": 3712, "url": "https://svs.gsfc.nasa.gov/3712/", "result_type": "Visualization", "release_date": "2010-04-21T14:15:00-04:00", "title": "SDO/HMI Continuum Full Disk View - April 7, 2010", "description": "This early sequence of HMI images from SDO focuses on a large sunspot group of Solar Cycle 24. || ", "hits": 70 }, { "id": 3713, "url": "https://svs.gsfc.nasa.gov/3713/", "result_type": "Visualization", "release_date": "2010-04-21T14:15:00-04:00", "title": "SDO/HMI Magnetogram Full Disk View - April 7, 2010", "description": "This early sequence of images from the HMI imager is processed to reveal the magnetic field structure (magnetogram). White locations represent a positive magnetic field value (north polarity) while black represents a negative magnetic field value (south polarity). Gray is zero magnetic field.Notice that the surface magnetic fields reveal much more structure than the white-light images in SDO/HMI Continuum Full Disk View - April 7, 2010. || ", "hits": 38 }, { "id": 3714, "url": "https://svs.gsfc.nasa.gov/3714/", "result_type": "Visualization", "release_date": "2010-04-21T14:15:00-04:00", "title": "SDO/HMI Dopplergram Sunspot Close-Up - March 29, 2010", "description": "The dopplergram from SDO/HMI data shows the velocity of solar material on the line-of-sight. White pixels are moving away from the camera and black pixels are moving towards the camera. || ", "hits": 31 }, { "id": 3715, "url": "https://svs.gsfc.nasa.gov/3715/", "result_type": "Visualization", "release_date": "2010-04-21T14:15:00-04:00", "title": "SDO/AIA Close-up on Launching Filament (band 304)", "description": "A close-up view of the filament launch in the 304 band, which corresponds to a wavelength of about 304 Ångstroms. || ", "hits": 26 }, { "id": 3716, "url": "https://svs.gsfc.nasa.gov/3716/", "result_type": "Visualization", "release_date": "2010-04-21T14:15:00-04:00", "title": "SDO/AIA Full-Disk View of Launching Filament (Band 304)", "description": "Full disk view of a filament launch in the SDO AIA 304 band. || ", "hits": 45 }, { "id": 3717, "url": "https://svs.gsfc.nasa.gov/3717/", "result_type": "Visualization", "release_date": "2010-04-21T14:15:00-04:00", "title": "SDO/AIA Zoom-out of Launching Filament (Band 304)", "description": "This view of the filament launch loops several times before pulling out to show the full solar disk. || ", "hits": 30 }, { "id": 3683, "url": "https://svs.gsfc.nasa.gov/3683/", "result_type": "Visualization", "release_date": "2010-04-02T00:00:00-04:00", "title": "Halloween 2003 Solar Storms: GOES/SXI X-ray view", "description": "Here is a view of the full solar disk during a two-week period in October and November of 2003 which exhibited some of the largest solar activity events since the advent of space-based solar observing. The GOES-12/Solar X-Ray Imager was experiencing significant problems during this time period and was offline during part of the opening and closing portions of this movie, which is why there is a significant number of black frames. Actual data collection began on October 28, 2003 and terminated on November 5, 2003.This movie is part of a series of movies with matching cadence designed to play synchronously with each other. The other movies in this series are Halloween 2003 Solar Storms: SOHO/EIT Ultraviolet, 195 angstromsHalloween 2003 Solar Storms: SOHO/EIT Ultraviolet, 304 angstromsHalloween 2003 Solar Storms: SOHO/MDI ContinuumHalloween 2003 Solar Storms: SOHO/MDI MagnetogramsHalloween 2003 Solar Storms: SOHO/EIT and SOHO/LASCO || ", "hits": 38 }, { "id": 3691, "url": "https://svs.gsfc.nasa.gov/3691/", "result_type": "Visualization", "release_date": "2010-03-31T00:00:00-04:00", "title": "A Comparative View of the Sun: SDO/AIA 193 and SOHO/EIT 195", "description": "This movie compares the spatial and temporal resolutions of the SDO/AIA (Atmospheric Imaging Assembly) imager to the SOHO/EIT (Extreme ultraviolet Imaging Telescope) imager. SOHO/EIT's highest resolution is 1024x1024 pixels with images taken about every 12 minutes for the 195 Ångstrom band. The SDO/AIA 193 band takes images at 4096x4096 pixels every twelve seconds!In this movie we can see the difference this makes for a closeup view of Active Region 1087. EIT reveals changes in the active region, which AIA reveals many details.This visualization is a companion piece to A Comparative View of the Sun: SDO/AIA 193 and STEREO-B/EUVI 195. || ", "hits": 61 }, { "id": 3694, "url": "https://svs.gsfc.nasa.gov/3694/", "result_type": "Visualization", "release_date": "2010-03-24T00:00:00-04:00", "title": "A Comparative View of the Sun: SDO/AIA 193 and STEREO-B/EUVI 195", "description": "This movie compares the spatial and temporal resolutions of the SDO/AIA (Atmospheric Imaging Assembly) imager to the STEREO/EUVI (Extreme UltraViolet Imager) imager. STEREO-B/EUVI's highest resolution is 2048x2048 pixels with images taken about every 5 minutes for the 195 Ångstrom band. The SDO/AIA 193 band takes images at 4096x4096 pixels every twelve seconds!While STEREO's vantage point at this time is very different from SDO, we can still identify some features of the Active Region 1087 in these two views. EUVI shows the launch of the filament, while AIA reveals many finer details.This visualization is a companion piece to A Comparative View of the Sun: SDO/AIA 193 and SOHO/EIT 195. || ", "hits": 52 }, { "id": 3505, "url": "https://svs.gsfc.nasa.gov/3505/", "result_type": "Visualization", "release_date": "2009-10-01T00:00:00-04:00", "title": "Solar Cycle 23: Minimum-Maximum-Minimum Synoptic Sequence", "description": "This is a sequence of solar synoptic maps covering Solar Cycle 23.The SOHO spacecraft began collecting this data in May of 1996, near the beginning (minimum) of the sunspot cycle. The sequence is projected in cylindrical-equidistant (CED) coordinates suitable for reprojection on spheres for animation or visualization purposes. These images are not suitable for scientific analysis.The original data were collected in FITS format from the SOHO/MDI archive, one image for each Carrington Rotation, which are 27.2753 days long.Solar minimum for Cycle 23 was in May 1996 (Carrington Rotation #1909), solar maximum around March 2000 (Carrington Rotation #1960), with a return to minimum about October 2008 (Carrington Rotation #2075). There are two gaps in the sequence, totalling four rotations, at Carrington rotations #1938, 1939, 1940, 1941, and 1998. These images are missing from the sequence due to SOHO being offline. Gaps in the data coverage for individual maps (occasional day outages or poor coverage near the poles of the Sun) were filled using data accumulated from previous maps.IMPORTANT NOTE: These images are for visualization purposes only. They are not suitable for scientific analysis. || ", "hits": 86 }, { "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": 114 }, { "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": 262 }, { "id": 3503, "url": "https://svs.gsfc.nasa.gov/3503/", "result_type": "Visualization", "release_date": "2008-04-02T00:00:00-04:00", "title": "Halloween 2003 Solar Storms: SOHO/MDI Magnetograms", "description": "Here is a view of the full solar disk during a two-week period in October and November of 2003 which exhibited some of the largest solar activity events since the advent of space-based solar observing.The Michelson Doppler Interferometer (MDI) takes images of the Sun at five very narrow wavelength bands and four different polarizations in visible light. For this sequence, the images are processed in a form that reveals the magnetic field strength on the solar photosphere. Other combinations of the images act as white-light images and dopplergrams (which measure the velocity of the solar 'surface').This movie is part of a series of movies with matching cadence designed to play synchronously with each other. The other movies in this series are Halloween 2003 Solar Storms: SOHO/EIT Ultraviolet, 195 angstroms Halloween 2003 Solar Storms: SOHO/EIT Ultraviolet, 304 angstroms Halloween 2003 Solar Storms: SOHO/MDI Continuum Halloween 2003 Solar Storms: SOHO/EIT and SOHO/LASCO For more information, visit the SOHO project page.. || ", "hits": 51 }, { "id": 2921, "url": "https://svs.gsfc.nasa.gov/2921/", "result_type": "Visualization", "release_date": "2005-03-08T12:00:00-05:00", "title": "Solar Tsunamis", "description": "Push-in to a region of the Sun to witness a 'solar tsunami' after a flare event. The tsunami moves hot gas (bright) out of the region, revealing cooler regions (darker) below. || ", "hits": 28 }, { "id": 2922, "url": "https://svs.gsfc.nasa.gov/2922/", "result_type": "Visualization", "release_date": "2005-03-08T12:00:00-05:00", "title": "Solar Tsunamis - View with a Spin", "description": "Push-in to a region of the Sun to witness a 'solar tsunami' after a flare event. The tsunami moves hot gas (bright) out of the region, revealing cooler regions (darker) below. This view rotates on the push-in to keep the region of the flare event visible (to the left in the final frame). || ", "hits": 17 }, { "id": 2936, "url": "https://svs.gsfc.nasa.gov/2936/", "result_type": "Visualization", "release_date": "2004-05-23T12:00:00-04:00", "title": "The fastest CME of Cycle 23 overtakes another fast CME", "description": "On November 4, 2003, the Sun produced its fastest coronal mass ejection (CME) for cycle 23 out of the active region 0486 located near the southwest limb of the Sun. The CME was expelled with a speed of approximately 2700 km/s. At the time of the launch of this CME, there was another ejection in progress from the same region. The previous ejection started about 7 hours earlier with a speed of about 1000 km/s. The fastest CME overtook the previous one within 2 hours and produced a spectacular radio radiation detected by the Wind, Ulysses and Cassini spacecraft. The movie shows the radio emission and the two interacting CMEs as observed by the SOHO spacecraft. || ", "hits": 64 }, { "id": 2923, "url": "https://svs.gsfc.nasa.gov/2923/", "result_type": "Visualization", "release_date": "2004-03-08T12:00:00-05:00", "title": "SOHO/MDI's 'Window' Through the Sun", "description": "Using the mathematical techniques, the SOHO/MDI view of the front side of the Sun can be processed to reveal features on the far side of the Sun. || ", "hits": 32 } ] }