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    "next": null,
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    "results": [
        {
            "id": 11558,
            "url": "https://svs.gsfc.nasa.gov/11558/",
            "result_type": "Produced Video",
            "release_date": "2014-09-24T10:00:00-04:00",
            "title": "NASA's Many Views of a Massive CME",
            "description": "On July 23, 2012, a massive cloud of solar material erupted off the sun's right side, zooming out into space. It soon passed one of NASA's Solar Terrestrial Relations Observatory, or STEREO, spacecraft, which clocked the CME as traveling between 1,800 and 2,200 miles per second as it left the sun. This was the fastest CME ever observed by STEREO.  Two other observatories – NASA's Solar Dynamics Observatory and the joint European Space Agency/NASA Solar and Heliospheric Observatory — witnessed the eruption as well. The July 2012 CME didn't move toward Earth, but watching an unusually strong CME like this gives scientists an opportunity to observe how these events originate and travel through space.  STEREO's unique viewpoint from the sides of the sun combined with the other two observatories watching from closer to Earth helped scientists create models of the entire July 2012 event. They learned that an earlier, smaller CME helped clear the path for the larger event, thus contributing to its unusual speed. Such data helps advance our understanding of what causes CMEs and improves modeling of similar CMEs that could be Earth-directed. || ",
            "hits": 130
        },
        {
            "id": 11387,
            "url": "https://svs.gsfc.nasa.gov/11387/",
            "result_type": "Produced Video",
            "release_date": "2013-10-29T16:30:00-04:00",
            "title": "Five Days of Flares and CMEs",
            "description": "This movie shows 23 of the 26 M- and X-class flares on the sun between 18:00 UT Oct. 23 and 15:00 UT Oct. 28, 2013, as captured by NASA's Solar Dynamics Observatory. It also shows the coronal mass ejections — great clouds of solar material bursting off the sun into space — during that time as captured by the ESA/NASA Solar and Heliospheric Observatory. || ",
            "hits": 109
        },
        {
            "id": 30072,
            "url": "https://svs.gsfc.nasa.gov/30072/",
            "result_type": "Hyperwall Visual",
            "release_date": "2013-09-25T00:00:00-04:00",
            "title": "Heliophysics Fleet Captures Eruption and CME",
            "description": "On May 1, 2013, NASA's Solar Dynamics Observatory (SDO) watched as an active region (left) of the sun erupted with a huge cloud of solar material—a heated, charged gas called plasma. This eruption, called a coronal mass ejection, or CME, sent the plasma streaming out through the solar system. Viewing the sun in the extreme ultraviolet wavelength of 304 Ångström, SDO provided a beautiful view of the initial arc as it left the solar surface. In addition to the images captured by SDO the CME was also observed by the European Space Agency/NASA Solar and Heliospheric Observatory (SOHO). SOHO houses two overlapping Large Angle Spectrometric Coronagraph (LASCO) telescopes where the bright sun is blocked by a disk so it does not overpower the fainter solar atmosphere. Both LASCO telescopes, named C2 and C3, observed the CME. The LASCO C2 coronagraph shows the region out to about 2.5 million miles, while the LASCO C3 coronagraph expands even farther out to around 13.5 million miles. Both of these instruments show the CME as it expands and becomes fainter on its trip away from the sun. || ",
            "hits": 33
        },
        {
            "id": 10785,
            "url": "https://svs.gsfc.nasa.gov/10785/",
            "result_type": "Produced Video",
            "release_date": "2013-05-07T11:00:00-04:00",
            "title": "NASA's Heliophysics Fleet Captures May 1, 2013 Prominence Eruption and CME",
            "description": "On May 1, 2013, NASA's Solar Dynamics Observatory (SDO) watched as an active region just around the East limb (left edge) of the sun erupted with a huge cloud of solar material—a heated, charged gas called plasma. This eruption, called a coronal mass ejection, or CME, sent the plasma streaming out through the solar system. Viewing the sun in the extreme ultraviolet wavelength of 304 angstroms, SDO provided a beautiful view of the initial arc as it left the solar surface.  Such eruptions soon leave SDO's field of view, but other satellites in NASA's Heliophysics fleet can pick them up, tracking such space weather to determine if they are headed toward Earth or spacecraft near other planets. With advance warning, many space assets can be put into safe mode and protect themselves from the effects of such particle radiation.In addition to the images captured by SDO, the May 1, 2013 CME was also observed by the ESA/NASA Solar and Heliospheric Observatory (SOHO). SOHO houses two overlapping coronagraphs—telescopes where the bright sun is blocked by a disk so it doesn't overpower the fainter solar atmosphere—and they both saw the CME continue outward. The LASCO C2 coronagraph shows the region out to about 2.5 million miles. The LASCO C3 coronagraph expands even farther out to around 13.5 million miles. Both of these instruments show the CME as it expands and becomes fainter on its trip away from the sun.NASA's Solar Terrestrial Relations Observatory (STEREO) Ahead satellite saw the eruption from a very different angle. It, along with its twin STEREO Behind, is orbiting at a similar distance as Earth. STEREO-A orbits slightly faster than Earth and STEREO-B orbits slightly slower. Currently, STEREO-A is more than two-thirds of the way to being directly behind the sun, and has a view of the far side of the sun. From this perspective, the CME came off the right side of the sun. STEREO has an extreme ultraviolet camera similar to SDO's, but it also has coronagraphs like SOHO. As a result, using its two inner coronagraphs, it was able to track the CME from the solar surface out to 6.3 million miles.Working together, such missions provide excellent coverage of a wide variety of solar events, a wealth of scientific data—and lots of beautiful imagery.Watch this video on YouTube. || ",
            "hits": 108
        },
        {
            "id": 11246,
            "url": "https://svs.gsfc.nasa.gov/11246/",
            "result_type": "Produced Video",
            "release_date": "2013-04-11T12:00:00-04:00",
            "title": "The Sun Emits a Mid-level Flare and CME",
            "description": "The sun emitted a mid-level flare, peaking at 3:16 a.m. EDT on April 11, 2013.Solar flares are powerful bursts of radiation. Harmful radiation from a flare cannot pass through Earth's atmosphere to physically affect humans on the ground, however — when intense enough — they can disturb the atmosphere in the layer where GPS and communications signals travel. This disrupts the radio signals for as long as the flare is ongoing, anywhere from minutes to hours.This flare is classified as an M6.5 flare, some ten times less powerful than the strongest flares, which are labeled X-class flares. M-class flares are the weakest flares that can still cause some space weather effects near Earth. This flare produced a radio blackout that has since subsided. The blackout was categorized as an R2 on a scale between R1 and R5 on NOAA's space weather scales.This is the strongest flare seen so far in 2013. Increased numbers of flares are quite common at the moment, since the sun's normal 11-year activity cycle is ramping up toward solar maximum, which is expected in late 2013. Humans have tracked this solar cycle continuously since it was discovered, and it is normal for there to be many flares a day during the sun's peak activity. || ",
            "hits": 60
        },
        {
            "id": 3956,
            "url": "https://svs.gsfc.nasa.gov/3956/",
            "result_type": "Visualization",
            "release_date": "2012-09-20T00:00:00-04:00",
            "title": "Halloween Solar Storms - 2003",
            "description": "This is a 1024x1024 pixel version of solar storms providing a more complete view of the SOHO/LASCO/C3 field-of-view.Here is a view of the solar disk in 195 Å ultraviolet light (colored green in this movie) and the Sun's extended atmosphere, or corona, (blue and white in this movie). The corona is visible to the SOHO/LASCO coronagraph instruments, which block the bright disk of the Sun so the significantly fainter corona can be seen. In this movie, the inner coronagraph (designated C2) is combined with the outer coronagraph (C3). This movie covers a two week period in October and November 2003 which exhibited some of the largest solar activity events since the advent of space-based solar observing.As the movie plays, we can observe a number of features of the active Sun. Long streamers radiate outward from the Sun and wave gently due to their interaction with the solar wind. The bright white regions are visible due to their high density of free electrons which scatter the light from the photosphere towards the observer. Protons and other ionized atoms are there as well, but are not as visible since they do not interact with photons as strongly as electrons. Coronal Mass Ejections (CMEs) are occasionally observed launching from the Sun. Some of these launch particle events which can saturate the cameras with snow-like artifacts.Also visible in the coronagraphs are stars and planets. Stars are seen to drift slowly to the right, carried by the relative motion of the Sun and the Earth. The planet Mercury is visible as the bright point moving left of the Sun. The horizontal 'extension' in the image is called 'blooming' and is due to a charge leakage along the readout wires in the CCD imager in the camera. || ",
            "hits": 92
        },
        {
            "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": 35
        },
        {
            "id": 3504,
            "url": "https://svs.gsfc.nasa.gov/3504/",
            "result_type": "Visualization",
            "release_date": "2008-04-02T00:00:00-04:00",
            "title": "Halloween 2003 Solar Storms: SOHO/EIT and SOHO/LASCO",
            "description": "Here is a view of the solar disk in 195 Å ultraviolet light (colored green in this movie) and the Sun's extended atmosphere, or corona, (blue and white in this movie). The corona is visible to the SOHO/LASCO coronagraph instruments, which block the bright disk of the Sun so the significantly fainter corona can be seen. In this movie, the inner coronagraph (designated C2) is combined with the outer coronagraph (C3). This movie covers a two week period in October and November 2003 which exhibited some of the largest solar activity events since the advent of space-based solar observing.As the movie plays, we can observe a number of features of the active Sun. Long streamers radiate outward from the Sun and wave gently due to their interaction with the solar wind. The bright white regions are visible due to their high density of free electrons which scatter the light from the photosphere towards the observer. Protons and other ionized atoms are there as well, but are not as visible since they do not interact with photons as strongly as electrons. Coronal Mass Ejections (CMEs) are occasionally observed launching from the Sun. Some of these launch particle events which can saturate the cameras with snow-like artifacts.Also visible in the coronagraphs are stars and planets. Stars are seen to drift slowly to the right, carried by the relative motion of the Sun and the Earth. The planet Mercury is visible as the bright point moving left of the Sun. The horizontal 'extension' in the image is called 'blooming' and is due to a charge leakage along the readout wires in the CCD imager in the camera.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 angstromHalloween 2003 Solar Storms: SOHO/EIT Ultraviolet, 304 angstromHalloween 2003 Solar Storms: SOHO/MDI Continuum Halloween 2003 Solar Storms: SOHO/MDI Magnetograms For more information, visit the SOHO project page.. || ",
            "hits": 52
        },
        {
            "id": 3431,
            "url": "https://svs.gsfc.nasa.gov/3431/",
            "result_type": "Visualization",
            "release_date": "2007-05-29T00:00:00-04:00",
            "title": "Coronal Mass Ejections (CME): Radio Quiet Variety",
            "description": "This is a simple comparison of SOHO/LASCO/C3 difference images (left side) combined with radio data from Wind/WAVES (right side).The LASCO difference images are produced from a time series of images by subtracting the previous image from the current image. Moving material therefore appears white on the leading edge and dark behind it. The WAVES spectrograph shows the variation of radio intensity (black is low, violet is high) in frequency (vertical axis) and time(horizontal axis). A vertical white bar marks the time of the LASCO image.This CME shows no radio-loud emission between 0.2-1.0 MHz. || ",
            "hits": 22
        },
        {
            "id": 3432,
            "url": "https://svs.gsfc.nasa.gov/3432/",
            "result_type": "Visualization",
            "release_date": "2007-05-29T00:00:00-04:00",
            "title": "Coronal Mass Ejections (CME): Radio Loud Variety",
            "description": "This is a simple comparison of SOHO/LASCO/C3 difference images (left side) combined with radio data from Wind/WAVES (right side).The LASCO difference images are produced from a time series of images by subtracting the previous image from the current image.  Moving material therefore appears white on the leading edge and dark behind it.  The WAVES spectrograph shows the variation of radio intensity (black is low, violet is high) in frequency (vertical axis) and time(horizontal axis).  A vertical white bar marks the time of the LASCO image.The radio-loud emission of the CME is the yellow-orange band between 0.2-1.0 MHz. || ",
            "hits": 44
        },
        {
            "id": 3406,
            "url": "https://svs.gsfc.nasa.gov/3406/",
            "result_type": "Visualization",
            "release_date": "2007-03-01T00:00:00-05:00",
            "title": "STEREO Coronal Mass Ejection:  From the EUVI to HI-2",
            "description": "This movie collects imagery from SOHO and STEREO-A of a coronal mass ejection (CME) during January of 2007. The instruments in this view, from left to right, are STEREO/HI-1, STEREO/HI-2, SOHO/LASCO/C3, SOHO/LASCO/C2, and STEREO/EUVI. The Heliospheric Imager, HI-2, shows some of the tail of comet McNaught. The dark trapezoidal shape on the left edge of the image in HI-2 is the Earth occulter which will block out the disk of the Earth when it moves into view (since the planet will appear so bright as to saturate the detectors). Due to ongoing work with the STEREO coronagraphs, COR1 and COR2, the SOHO/LASCO coronagraphs are used for this movie. The blue Sun in the center of the coronagraphs is STEREO/EUVI ultraviolet images.There is a 22 hour gap in the data coverage for HI-2 which creates the appearance of a jump in the playback.These are not standard images but are called 'running difference' images which highlight changes in the view. White pixels correspond to increases in brightness, while dark pixels reflect a decrease in brightness, with respect to the immediately previous image.'Running differencing' generates some unusual effects. For example, the mottled background is created by the motion of the stars through the field-of-view as the spacecraft pointing direction slowly changes (the Andromeda galaxy is the oblong 'smudge' near the upper left corner). The planets Venus (right edge of HI-2) and Mercury are visible (near center of HI-1), their column of pixels saturated due to their brightness.STEREO: Solar TErrestrial RElations ObservatorySOHO: SOlar Heliospheric ObservatoryLASCO: Large Angle and Spectrometric CoronagraphEUVI: Extreme UltraViolet Imager || ",
            "hits": 32
        },
        {
            "id": 3159,
            "url": "https://svs.gsfc.nasa.gov/3159/",
            "result_type": "Visualization",
            "release_date": "2005-05-24T12:00:00-04:00",
            "title": "SOHO/LASCO View of January 2005 Solar Events",
            "description": "The January 20 flare began just before 2 a.m. ET. A storm of energetic protons impacted Earth just 15 minutes later. These views of the flare are from the Solar and Heliospheric Observatory (SOHO). The proton storm near Earth causes `snow' in the images, obscuring the Sun as radiation swamps the cameras. The structure at the 1:30 position in the SOHO/LASCO/C3 data is the occulting disk pylon. || ",
            "hits": 44
        },
        {
            "id": 2961,
            "url": "https://svs.gsfc.nasa.gov/2961/",
            "result_type": "Visualization",
            "release_date": "2004-07-08T12:00:00-04:00",
            "title": "Halloween Solar Storms from SOHO/EIT and SOHO/LASCO",
            "description": "This movie is a combination of SOHO/EIT at 195 angstroms as well as the LASCO/C2 and C3 cameras. At this scale we can see the flashes from solar flares in SOHO/EIT (green) and the subsequent coronal mass ejections in SOHO/LASCO/C2 (red) and SOHO/LASCO/C3 (blue). This movie is synchronized to play with animation IDs 2960 and 2959. For more information on how X-ray solar flares are classified (B, C, M, X), visit SpaceWeather.com. || ",
            "hits": 25
        },
        {
            "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": 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": 24
        },
        {
            "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": 15
        },
        {
            "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": 22
        }
    ]
}