{ "count": 22, "next": null, "previous": null, "results": [ { "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": 77 }, { "id": 3566, "url": "https://svs.gsfc.nasa.gov/3566/", "result_type": "Visualization", "release_date": "2008-12-18T00:00:00-05:00", "title": "Multi-Sun Composition", "description": "This movie is a composition of multiple solar datasets synchronized in time. The time frame is late October and early November of 2003, the time of some record-breaking solar activity.The background of the movie shows the view of the wide-angle coronagraphs (blue/white), or LASCO instruments, aboard SOHO. They show streams of electrons outbound from the Sun, part of the solar atmosphere. The central green image is the Sun in ultraviolet light from the EIT instrument. Note that flashes of solar flares in the ultraviolet quickly propagate out from the Sun and are visible in LASCO. These events are coronal mass ejections, or CMEs.Overlaid on the upper left is a better view of the EIT ultraviolet image at a wavelength of 195 angstroms (19.5 nanometers).On the lower left, the orange movie is the EIT ultraviolet movie at 304 angstroms (30.4 nanometers).On the upper right is a solar magnetogram, taken by the MDI instrument. The white regions correspond to positive (north) magnetic flux and the dark regions to negative (south) magnetic flux.The colors for the sequences above are not real. They are chosen by convention since the properties recorded by the cameras are not visible to the human eye.The final image on the lower right is also from MDI. It is a combination of several optical wavelengths and is the best representation from SOHO of the Sun in visible light, as we would see it through ground-based telescopes.The movies that are part of this composition are also available individually on the SVS site: Halloween Solar Storms 2003: SOHO/EIT and SOHO/LASCOHalloween Solar Storms 2003: SOHO/EIT Ultraviolet, 195 angstromsHalloween Solar Storms 2003: SOHO/EIT Ultraviolet, 304 angstromsHalloween Solar Storms 2003: SOHO/MDI ContinuumHalloween Solar Storms 2003: SOHO/MDI Magnetograms || ", "hits": 30 }, { "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": 260 }, { "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": 111 }, { "id": 3502, "url": "https://svs.gsfc.nasa.gov/3502/", "result_type": "Visualization", "release_date": "2008-04-02T00:00:00-04:00", "title": "Halloween 2003 Solar Storms: SOHO/MDI Continuum", "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) records images at several very narrow wavelength bands in the visible light. These images are often used as proxies for white-light solar images. 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 Magnetograms Halloween 2003 Solar Storms: SOHO/EIT and SOHO/LASCO For more information, visit the SOHO project page. || ", "hits": 28 }, { "id": 3386, "url": "https://svs.gsfc.nasa.gov/3386/", "result_type": "Visualization", "release_date": "2006-11-08T00:00:00-05:00", "title": "Mercury Transit from SOHO/MDI", "description": "This is a view of the planet Mercury (the tiny moving black dot) as seen by the SOHO MDI.The narrow field-of-view for this camera mode necessitates the addition of black bars at the top and bottom of the frame to match HD720 resolution.This movie was generated from telemetry which has undergone a minimum of processing (to deliver quickly for the media) so data dropouts and other quick-processing artifacts may be visible. Special thanks to Steele Hill of the SOHO project for this effort. || ", "hits": 32 }, { "id": 3336, "url": "https://svs.gsfc.nasa.gov/3336/", "result_type": "Visualization", "release_date": "2006-04-01T00:00:00-05:00", "title": "The Visible Sun Revisited", "description": "Scientists working with the SOHO/MDI instrument have continued to improve on previous results. Since the first release (SOHO/MDI's 'Window' Through the Sun), improvements in helioseismology techniques have enabled them to extract more information from the same data. In this case, sonogram-type imaging of the solar far side (the side of the Sun NOT facing the Earth) has been improved to provide a more complete view of the farside. This is important in space weather forecasting as it enables us to see large sunspots and active regions before they are visible directly from the Earth. Active regions are a source of solar flares which can send high-energy protons towards the Earth. These protons can damage satellite electronics, endangering communications and weather forecasting, and are a health threat to astronauts. || ", "hits": 45 }, { "id": 3211, "url": "https://svs.gsfc.nasa.gov/3211/", "result_type": "Visualization", "release_date": "2005-08-16T12:00:00-04:00", "title": "Space Weather Forecasting: Quiet Times Ahead", "description": "SOHO/MDI magnetograms combined with the Potential-Field Source-Surface (PFSS) model can be used to generate a model of magnetic field lines in the lower part of the solar corona. When these models are compared to the loops visible in TRACE imagery, a good match (as in this case) indicates that the region will not generate flare events over the next few days. || ", "hits": 11 }, { "id": 3212, "url": "https://svs.gsfc.nasa.gov/3212/", "result_type": "Visualization", "release_date": "2005-08-16T12:00:00-04:00", "title": "Space Weather Forecasting: Active Times Ahead", "description": "SOHO/MDI magnetograms combined with the Potential-Field Source-Surface (PFSS) model can be used to generate a model of magnetic field lines in the lower part of the solar corona. When these models are compared to the loops visible in TRACE imagery, a bad match (as in this case) indicates that the region will generate flare events over the next few days. || ", "hits": 17 }, { "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": 20 }, { "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": 14 }, { "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 }, { "id": 2766, "url": "https://svs.gsfc.nasa.gov/2766/", "result_type": "Visualization", "release_date": "2003-07-09T12:00:00-04:00", "title": "Hi-resolution Solar Views from VAULT: Quiet Region", "description": "This movie presents the VAULT imagery in the context of simultaneous multi-mission observations. We zoom-in to a subset of the image which focuses on a relatively calm solar region which still reveals a great deal of activity. || ", "hits": 22 }, { "id": 2509, "url": "https://svs.gsfc.nasa.gov/2509/", "result_type": "Visualization", "release_date": "2003-01-31T12:00:00-05:00", "title": "A Multi-Mission View of the AR9906 Solar Flare with Instrument Labels", "description": "Here's a view of the Sun, from the point of view of a fleet of Sun-observing spacecraft - SOHO, TRACE, and RHESSI. The time scales of the data samples in this visualization range from six hours to as short as 12 seconds and the display rate varies throughout the movie. The region and event of interest is the solar flare over solar active region AR9906 on April 21, 2002. In this visualization, the instrument names appear in a color roughly matching the color used for the data, and black corresponds to no (current) instrument coverage. || ", "hits": 26 }, { "id": 2511, "url": "https://svs.gsfc.nasa.gov/2511/", "result_type": "Visualization", "release_date": "2003-01-31T12:00:00-05:00", "title": "A Multi-Mission View of the AR9906 Solar Flare without Instrument Labels", "description": "Here's a view of the Sun, from the point of view of a fleet of Sun-observing spacecraft - SOHO, TRACE, and RHESSI. The time scales of the data samples in this visualization range from 6 hours to as short as 12 seconds and the display rate varies throughout the movie. The region and event of interest is the solar flare over solar active region AR9906 on April 21, 2002. In this visualization, black corresponds to no (current) instrument coverage (there used to be a LASCO C1 camera inside the ring of LASCO C2, but that instrument didn't recover after SOHO was temporarily 'lost' in 1998). || ", "hits": 17 }, { "id": 2553, "url": "https://svs.gsfc.nasa.gov/2553/", "result_type": "Visualization", "release_date": "2003-01-31T12:00:00-05:00", "title": "A Multi-Mission View of the AR9906 Solar Flare with Alternate Instrument Labels", "description": "Here's a view of the Sun, from the point of view of a fleet of Sun-observing spacecraft - SOHO, TRACE, and RHESSI. The time scales of the data samples in this visualization range from 6 hours to as short as 12 seconds and the display rate varies throughout the movie. The region and event of interest is the solar flare over solar active region AR9906 on April 21, 2002. In this visualization, black corresponds to no (current) instrument coverage (there used to be a LASCO C1 camera inside the ring of LASCO C2, but that instrument didn't recover after SOHO was temporarily 'lost' in 1998). || ", "hits": 18 }, { "id": 2287, "url": "https://svs.gsfc.nasa.gov/2287/", "result_type": "Visualization", "release_date": "2001-12-10T11:30:00-05:00", "title": "The Spinning Sunspot", "description": "Zoom-in to the sunspot group and watch it rotate || a002287.00005_print.png (720x480) [413.4 KB] || spinspot2_pre.jpg (320x240) [5.6 KB] || a002287.webmhd.webm (960x540) [4.9 MB] || a002287.dv (720x480) [60.1 MB] || spinspot2.mpg (320x240) [2.4 MB] || Full sun view with SOHO-MDI data || spinningspot0001.jpg (2560x1920) [351.5 KB] || spinningspot0001_web.jpg (320x240) [7.3 KB] || spinningspot0001.tif (2560x1920) [2.1 MB] || ", "hits": 28 }, { "id": 2243, "url": "https://svs.gsfc.nasa.gov/2243/", "result_type": "Visualization", "release_date": "2001-11-06T13:00:00-05:00", "title": "SOHO/MDI Views the Sun - 1998", "description": "This version projects the solar image on a sphere for improved perspective. || Movie of the solar disk from April 30 to June 24, 1998. || a002243.00020_print.png (720x480) [376.5 KB] || FullDisk1998_pre.jpg (320x240) [4.6 KB] || a002243.webmhd.webm (960x540) [712.6 KB] || a002243.dv (720x480) [30.9 MB] || FullDisk1998.mpg (320x240) [922.3 KB] || ", "hits": 32 }, { "id": 2244, "url": "https://svs.gsfc.nasa.gov/2244/", "result_type": "Visualization", "release_date": "2001-11-06T13:00:00-05:00", "title": "SOHO/MDI Views the Sun - 2001", "description": "This version projects the solar image on a sphere for improved perspective. || SOHO-MDI views the Sun from March 1 to May 31, 2001. || a002244.00095_print.png (720x480) [393.7 KB] || FD2001_pre.jpg (320x238) [4.6 KB] || a002244.webmhd.webm (960x540) [4.2 MB] || a002244.dv (720x480) [157.8 MB] || FD2001.mpg (352x240) [6.3 MB] || ", "hits": 38 }, { "id": 2268, "url": "https://svs.gsfc.nasa.gov/2268/", "result_type": "Visualization", "release_date": "2001-11-06T13:00:00-05:00", "title": "SOHO/MDI Views the Sun - 1998", "description": "This version projects the solar image on a flat plane. It runs at a third of the speed of the original version. || SOHO-MDI images the sun from April 30 to June 24, 1998. || a002268.00095_print.png (720x480) [363.2 KB] || a002268_pre.jpg (320x240) [4.3 KB] || a002268.webmhd.webm (960x540) [1.5 MB] || a002268.dv (720x480) [75.5 MB] || a002268.mpg (320x240) [995.0 KB] || ", "hits": 27 }, { "id": 2269, "url": "https://svs.gsfc.nasa.gov/2269/", "result_type": "Visualization", "release_date": "2001-11-06T13:00:00-05:00", "title": "SOHO/MDI Views the Sun - 2001", "description": "This version projects the solar image on a flat plane. || A view of the Sun from SOHO-MDI from March thru May 2001. || a002269.00095_print.png (720x480) [379.6 KB] || Sunspots2001_pre.jpg (320x238) [4.2 KB] || a002269.webmhd.webm (960x540) [3.6 MB] || a002269.dv (720x480) [157.8 MB] || Sunspots2001.mpg (352x240) [6.3 MB] || ", "hits": 20 } ] }