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        {
            "id": 4663,
            "url": "https://svs.gsfc.nasa.gov/4663/",
            "result_type": "Visualization",
            "release_date": "2018-07-27T00:00:00-04:00",
            "title": "Earth's Magnetosphere",
            "description": "A simple visualization of Earth's magnetosphere near the time of the equinox. || Earth_Equinox_Dayside.slate_BaseRig.HD1080i.1000_print.jpg (1024x576) [139.2 KB] || Earth_Equinox_Dayside.slate_BaseRig.HD1080i.1000_searchweb.png (320x180) [91.9 KB] || Earth_Equinox_Dayside.slate_BaseRig.HD1080i.1000_thm.png (80x40) [6.1 KB] || Equinox_Dayside-noglyph (1920x1080) [0 Item(s)] || Earth_Equinox_Dayside.HD1080i_p30.webm (1920x1080) [13.0 MB] || Earth_Equinox_Dayside.HD1080i_p30.mp4 (1920x1080) [240.4 MB] || Equinox_Dayside-noglyph (3840x2160) [0 Item(s)] || Earth_Equinox_Dayside_2160p30.mp4 (3840x2160) [642.0 MB] || Earth_Equinox_Dayside.HD1080i_p30.mp4.hwshow [199 bytes] || ",
            "hits": 149
        },
        {
            "id": 4664,
            "url": "https://svs.gsfc.nasa.gov/4664/",
            "result_type": "Visualization",
            "release_date": "2018-07-27T00:00:00-04:00",
            "title": "Jupiter's Magnetosphere",
            "description": "Jupiter's magnetosphere - a basic view. || Jupiter_JupiterBasic_Dayside.slate_BaseRig.HD1080i.1000_print.jpg (1024x576) [245.3 KB] || Jupiter_JupiterBasic_Dayside.slate_BaseRig.HD1080i.1000_searchweb.png (320x180) [132.5 KB] || Jupiter_JupiterBasic_Dayside.slate_BaseRig.HD1080i.1000_thm.png (80x40) [8.3 KB] || JupiterBasic-noglyph (1920x1080) [0 Item(s)] || Jupiter_JupiterBasic_Dayside.HD1080i_p30.webm (1920x1080) [32.8 MB] || Jupiter_JupiterBasic_Dayside.HD1080i_p30.mp4 (1920x1080) [406.6 MB] || JupiterBasic-noglyph (3840x2160) [0 Item(s)] || Jupiter_JupiterBasic_Dayside_2160p30.mp4 (3840x2160) [984.8 MB] || Jupiter_JupiterBasic_Dayside.HD1080i_p30.mp4.hwshow [206 bytes] || ",
            "hits": 195
        },
        {
            "id": 4665,
            "url": "https://svs.gsfc.nasa.gov/4665/",
            "result_type": "Visualization",
            "release_date": "2018-07-27T00:00:00-04:00",
            "title": "Saturn's Magnetosphere",
            "description": "A basic view of Saturn's magnetosphere. || Saturn_SaturnBasic_Dayside.slate_BaseRig.HD1080i.1500_print.jpg (1024x576) [186.2 KB] || Saturn_SaturnBasic_Dayside.slate_BaseRig.HD1080i.1500_searchweb.png (320x180) [107.8 KB] || Saturn_SaturnBasic_Dayside.slate_BaseRig.HD1080i.1500_thm.png (80x40) [7.1 KB] || SaturnBasic-noglyph (1920x1080) [0 Item(s)] || Saturn_SaturnBasic_Dayside.HD1080i_p30.webm (1920x1080) [22.1 MB] || Saturn_SaturnBasic_Dayside.HD1080i_p30.mp4 (1920x1080) [365.5 MB] || SaturnBasic-noglyph (3840x2160) [0 Item(s)] || Saturn_SaturnBasic_Dayside_2160p30.mp4 (3840x2160) [938.9 MB] || Saturn_SaturnBasic_Dayside.HD1080i_p30.mp4.hwshow || ",
            "hits": 122
        },
        {
            "id": 4666,
            "url": "https://svs.gsfc.nasa.gov/4666/",
            "result_type": "Visualization",
            "release_date": "2018-07-27T00:00:00-04:00",
            "title": "Uranus' Magnetosphere",
            "description": "A basic view of the Uranian magnetosphere when the rotation axis is perpendicular to the Uranus-Sun line and days and nights are of equal duration. || Uranus_UranusEquinox_Dayside.slate_BaseRig.HD1080i.1500_print.jpg (1024x576) [197.1 KB] || Uranus_UranusEquinox_Dayside.slate_BaseRig.HD1080i.1500_searchweb.png (320x180) [107.3 KB] || Uranus_UranusEquinox_Dayside.slate_BaseRig.HD1080i.1500_thm.png (80x40) [6.8 KB] || UranusEquinox-noglyph (1920x1080) [0 Item(s)] || Uranus_UranusEquinox_Dayside.HD1080i_p30.webm (1920x1080) [20.9 MB] || Uranus_UranusEquinox_Dayside.HD1080i_p30.mp4 (1920x1080) [308.1 MB] || UranusEquinox-noglyph (3840x2160) [0 Item(s)] || Uranus_UranusEquinox_Dayside_2160p30.mp4 (3840x2160) [758.5 MB] || Uranus_UranusEquinox_Dayside.HD1080i_p30.mp4.hwshow [206 bytes] || ",
            "hits": 106
        },
        {
            "id": 4667,
            "url": "https://svs.gsfc.nasa.gov/4667/",
            "result_type": "Visualization",
            "release_date": "2018-07-27T00:00:00-04:00",
            "title": "Neptune's Magnetosphere",
            "description": "A basic view of the Neptunian magnetosphere when the southern side of the rotation axis is directed sunward (southern summer) || Neptune_NeptuneSouthSummer_Dayside.slate_BaseRig.HD1080i.1500_print.jpg (1024x576) [195.5 KB] || Neptune_NeptuneSouthSummer_Dayside.slate_BaseRig.HD1080i.1500_searchweb.png (320x180) [108.2 KB] || Neptune_NeptuneSouthSummer_Dayside.slate_BaseRig.HD1080i.1500_thm.png (80x40) [6.8 KB] || NeptuneSouthSummer-noglyph (1920x1080) [0 Item(s)] || Neptune_NeptuneSouthSummer_Dayside.HD1080i_p30.webm (1920x1080) [21.4 MB] || Neptune_NeptuneSouthSummer_Dayside.HD1080i_p30.mp4 (1920x1080) [328.8 MB] || NeptuneSouthSummer-noglyph (3840x2160) [0 Item(s)] || Neptune_NeptuneSouthSummer_Dayside_2160p30.mp4 (3840x2160) [820.2 MB] || Neptune_NeptuneSouthSummer_Dayside.HD1080i_p30.mp4.hwshow [212 bytes] || ",
            "hits": 206
        },
        {
            "id": 4143,
            "url": "https://svs.gsfc.nasa.gov/4143/",
            "result_type": "Visualization",
            "release_date": "2017-07-12T10:01:00-04:00",
            "title": "Saturn's Magnetosphere",
            "description": "Earth's magnetic field creates a 'bubble' around Earth that helps protect our planet from some of the more harmful effects of energetic particles streaming out from the sun in the solar wind.  Some of the earliest hints of this interaction go back to the 1850s with the work of Richard Carrington, and in the early 1900s with the work of Kristian Birkeland and Carl Stormer.  That this field might form a type of 'bubble' around Earth was hypothesized by Sidney Chapman and Vincent Ferraro in the 1930s.  The term 'magnetosphere' was applied to magnetic bubble by Thomas Gold in 1959.  But it wasn't until the Space Age, when we sent the first probes to other planets, that we found clear evidence of their magnetic fields (though there were hints of a magnetic field for Jupiter in the 1950s, due to observations from radio telescopes).  The Voyager program , two spacecraft launched in 1977, and successors to the Pioneer 10 and 11 missions, completed flybys of the giant outer planets.  They became the implementation of the 'Grand Tour' of the outer planets originally proposed in the late 1960s.  The Voyagers provided some of the first detailed measurments of the strength, extent and diversity of the magnetospheres of the outer planets.In these visualizations, we present simplified models of these planetary magnetospheres, designed to illustrate their scale, and basic features of their structure and impacts of the magnetic axes offset from the planetary rotation axes. For these visualizations, the magnetic field structure is represented by gold/copper lines.  Some additional glyphs are provided to indicate some key directions in the field model.The Yellow arrow points towards the sun.  The magnetotail is pointed in the opposite direction.The Cyan arrow represents the magnetic axis, usually tilted relative to the rotation axis.  The arrow indicates the NORTH magnetic pole (convention has field lines moving north to south as the north pole of bar magnet (and compass pointer) points to the south magnetic pole).The Blue arrow represents the north rotation axis.  It is part of the 3-D axis glyph (red, green, and blue arrows) included to make the planetary rotation more apparent.The semi-transparent grey mesh in the distance represents the boundary of the magnetosphere.Major satellites of the planetary system are also included.  When appropriate for the time window of the visualization, the Voyager flyby trajectories are indicated.The models are constructed by combining the fields of a simple magnetic dipole, a current sheet (whose intensity is tuned match the scale of the magnetotail), and occasionally a ring current.  This is a variation of the simple Luhmann-Friesen magnetosphere model.  They are meant to be representative of the basic characteristics of the planetary magnetic fields.  Some features NOT included are longitudes of magnetic poles to a standard planetary coordinate system and offsets of the dipole center from the planetary center.  ReferencesT. Gold, Motions in the Magnetosphere of the EarthLuhmann & Friesen, A simple model of the magnetosphereLASP: Polarity of planetary magnetic fieldsWikipedia: The Solar Storm of 1859Wikipedia: Kristian BirkelandWikipedia: Carl StørmerSpecial thanks to Arik Posner (NASA/HQ) and Gina DiBraccio (UMBC/GSFC) for helpful pointers on orientation of planetary rotation and magnetic axes. || ",
            "hits": 64
        },
        {
            "id": 4141,
            "url": "https://svs.gsfc.nasa.gov/4141/",
            "result_type": "Visualization",
            "release_date": "2017-07-12T10:00:00-04:00",
            "title": "Earth's Magnetosphere",
            "description": "Earth's magnetic field creates a 'bubble' around Earth that helps protect our planet from some of the more harmful effects of energetic particles streaming out from the sun in the solar wind.  Some of the earliest hints of this interaction go back to the 1850s with the work of Richard Carrington, and in the early 1900s with the work of Kristian Birkeland and Carl Stormer.  That this field might form a type of 'bubble' around Earth was hypothesized by Sidney Chapman and Vincent Ferraro in the 1930s.  The term 'magnetosphere' was applied to magnetic bubble by Thomas Gold in 1959.  But it wasn't until the Space Age, when we sent the first probes to other planets, that we found clear evidence of their magnetic fields (though there were hints of a magnetic field for Jupiter in the 1950s, due to observations from radio telescopes).  The Voyager program , two spacecraft launched in 1977, and successors to the Pioneer 10 and 11 missions, completed flybys of the giant outer planets.  They became the implementation of the 'Grand Tour' of the outer planets originally proposed in the late 1960s.  The Voyagers provided some of the first detailed measurments of the strength, extent and diversity of the magnetospheres of the outer planets.In these visualizations, we present simplified models of these planetary magnetospheres, designed to illustrate their scale, and basic features of their structure and impacts of the magnetic axes offset from the planetary rotation axes. For this Earth visualization, note that the north magnetic pole points out of the southern hemisphere.For these visualizations, the magnetic field structure is represented by gold/copper lines.  Some additional glyphs are provided to indicate some key directions in the field model.The Yellow arrow points towards the sun.  The magnetotail is pointed in the opposite direction.The Cyan arrow represents the magnetic axis, usually tilted relative to the rotation axis.  The arrow indicates the NORTH magnetic pole (convention has field lines moving north to south as the north pole of bar magnet (and compass pointer) points to the south magnetic pole).The Blue arrow represents the north rotation axis.  It is part of the 3-D axis glyph (red, green, and blue arrows) included to make the planetary rotation more apparent.The semi-transparent grey mesh in the distance represents the boundary of the magnetosphere.Major satellites of the planetary system are also included.  When appropriate for the time window of the visualization, the Voyager flyby trajectories are indicated.The models are constructed by combining the fields of a simple magnetic dipole, a current sheet (whose intensity is tuned match the scale of the magnetotail), and occasionally a ring current.  This is a variation of the simple Luhmann-Friesen magnetosphere model.  They are meant to be representative of the basic characteristics of the planetary magnetic fields.  Some features NOT included are longitudes of magnetic poles to a standard planetary coordinate system and offsets of the dipole center from the planetary center.  ReferencesT. Gold, Motions in the Magnetosphere of the EarthLuhmann and Friesen, A simple model of the magnetosphereLASP: Polarity of planetary magnetic fieldsWikipedia: The Solar Storm of 1859Wikipedia: Kristian BirkelandWikipedia: Carl StørmerSpecial thanks to Arik Posner (NASA/HQ) and Gina DiBraccio (UMBC/GSFC) for helpful pointers on orientation of planetary rotation and magnetic axes. || ",
            "hits": 162
        },
        {
            "id": 4142,
            "url": "https://svs.gsfc.nasa.gov/4142/",
            "result_type": "Visualization",
            "release_date": "2017-07-12T10:00:00-04:00",
            "title": "Jupiter's Magnetosphere",
            "description": "Earth's magnetic field creates a 'bubble' around Earth that helps protect our planet from some of the more harmful effects of energetic particles streaming out from the sun in the solar wind.  Some of the earliest hints of this interaction go back to the 1850s with the work of Richard Carrington, and in the early 1900s with the work of Kristian Birkeland and Carl Stormer.  That this field might form a type of 'bubble' around Earth was hypothesized by Sidney Chapman and Vincent Ferraro in the 1930s.  The term 'magnetosphere' was applied to magnetic bubble by Thomas Gold in 1959.  But it wasn't until the Space Age, when we sent the first probes to other planets, that we found clear evidence of their magnetic fields (though there were hints of a magnetic field for Jupiter in the 1950s, due to observations from radio telescopes).  The Voyager program , two spacecraft launched in 1977, and successors to the Pioneer 10 and 11 missions, completed flybys of the giant outer planets.  They became the implementation of the 'Grand Tour' of the outer planets originally proposed in the late 1960s.  The Voyagers provided some of the first detailed measurments of the strength, extent and diversity of the magnetospheres of the outer planets.In these visualizations, we present simplified models of these planetary magnetospheres, designed to illustrate their scale, and basic features of their structure and impacts of the magnetic axes offset from the planetary rotation axes. The volcanic activity on Jupiter's moon Io launches a large amount of sulfur-based compounds along its orbit, which is subsequently ionized by solar ultraviolet radiation.  This is represented in the visualization by the yellowish structure along the orbit of Io.  This creates a plasma torus and ring current around Jupiter, which alters the planet's magnetic field, forming some of the perturbations in Jupiter's magnetic field along the orbit of Io.For these visualizations, the magnetic field structure is represented by gold/copper lines.  Some additional glyphs are provided to indicate some key directions in the field model.The Yellow arrow points towards the sun.  The magnetotail is pointed in the opposite direction.The Cyan arrow represents the magnetic axis, usually tilted relative to the rotation axis.  The arrow indicates the NORTH magnetic pole (convention has field lines moving north to south as the north pole of bar magnet (and compass pointer) points to the south magnetic pole).The Blue arrow represents the north rotation axis.  It is part of the 3-D axis glyph (red, green, and blue arrows) included to make the planetary rotation more apparent.The semi-transparent grey mesh in the distance represents the boundary of the magnetosphere.Major satellites of the planetary system are also included.  When appropriate for the time window of the visualization, the Voyager flyby trajectories are indicated.The models are constructed by combining the fields of a simple magnetic dipole, a current sheet (whose intensity is tuned match the scale of the magnetotail), and occasionally a ring current.  This is a variation of the simple Luhmann-Friesen magnetosphere model.  They are meant to be representative of the basic characteristics of the planetary magnetic fields.  Some features NOT included are longitudes of magnetic poles to a standard planetary coordinate system and offsets of the dipole center from the planetary center.  ReferencesT. Gold, Motions in the Magnetosphere of the EarthLuhmann and Friesen, A simple model of the magnetosphereLASP: Polarity of planetary magnetic fieldsWikipedia: The Solar Storm of 1859Wikipedia: Kristian BirkelandWikipedia: Carl StørmerSpecial thanks to Arik Posner (NASA/HQ) and Gina DiBraccio (UMBC/GSFC) for helpful pointers on orientation of planetary rotation and magnetic axes. || ",
            "hits": 250
        },
        {
            "id": 4144,
            "url": "https://svs.gsfc.nasa.gov/4144/",
            "result_type": "Visualization",
            "release_date": "2017-07-12T10:00:00-04:00",
            "title": "Uranus' Magnetosphere",
            "description": "Earth's magnetic field creates a 'bubble' around Earth that helps protect our planet from some of the more harmful effects of energetic particles streaming out from the sun in the solar wind.  Some of the earliest hints of this interaction go back to the 1850s with the work of Richard Carrington, and in the early 1900s with the work of Kristian Birkeland and Carl Stormer.  That this field might form a type of 'bubble' around Earth was hypothesized by Sidney Chapman and Vincent Ferraro in the 1930s.  The term 'magnetosphere' was applied to magnetic bubble by Thomas Gold in 1959.  But it wasn't until the Space Age, when we sent the first probes to other planets, that we found clear evidence of their magnetic fields (though there were hints of a magnetic field for Jupiter in the 1950s, due to observations from radio telescopes).  The Voyager program , two spacecraft launched in 1977, and successors to the Pioneer 10 and 11 missions, completed flybys of the giant outer planets.  They became the implementation of the 'Grand Tour' of the outer planets originally proposed in the late 1960s.  The Voyagers provided some of the first detailed measurments of the strength, extent and diversity of the magnetospheres of the outer planets.In these visualizations, we present simplified models of these planetary magnetospheres, designed to illustrate their scale, and basic features of their structure and impacts of the magnetic axes offset from the planetary rotation axes. The rotation axis of Uranus is tilted over ninety degrees relative to the revolution axis of the solar system, placing it roughly in the plane of the solar system.  In addition, the magnetic axis has a large tilt relative to the rotation axis.  These effects combine to not only give Uranus a more a more variable magnetosphere, but suggest the planet's magnetic field may be generated by a different mechanism  than that of Earth, Jupiter and Saturn.For these visualizations, the magnetic field structure is represented by gold/copper lines.  Some additional glyphs are provided to indicate some key directions in the field model.The Yellow arrow points towards the sun.  The magnetotail is pointed in the opposite direction.The Cyan arrow represents the magnetic axis, usually tilted relative to the rotation axis.  The arrow indicates the NORTH magnetic pole (convention has field lines moving north to south as the north pole of bar magnet (and compass pointer) points to the south magnetic pole).The Blue arrow represents the north rotation axis.  It is part of the 3-D axis glyph (red, green, and blue arrows) included to make the planetary rotation more apparent.The semi-transparent grey mesh in the distance represents the boundary of the magnetosphere.Major satellites of the planetary system are also included.  When appropriate for the time window of the visualization, the Voyager flyby trajectories are indicated.The models are constructed by combining the fields of a simple magnetic dipole, a current sheet (whose intensity is tuned match the scale of the magnetotail), and occasionally a ring current.  This is a variation of the simple Luhmann-Friesen magnetosphere model.  They are meant to be representative of the basic characteristics of the planetary magnetic fields.  Some features NOT included are longitudes of magnetic poles to a standard planetary coordinate system and offsets of the dipole center from the planetary center.  ReferencesT. Gold, Motions in the Magnetosphere of the EarthLuhmann & Friesen, A simple model of the magnetosphereMagnetic reconnection at Uranus' magnetopauseLASP: Polarity of planetary magnetic fieldsWikipedia: The Solar Storm of 1859Wikipedia: Kristian BirkelandWikipedia: Carl StørmerSpecial thanks to Arik Posner (NASA/HQ) and Gina DiBraccio (UMBC/GSFC) for helpful pointers on orientation of planetary rotation and magnetic axes. || ",
            "hits": 356
        },
        {
            "id": 4145,
            "url": "https://svs.gsfc.nasa.gov/4145/",
            "result_type": "Visualization",
            "release_date": "2017-07-12T10:00:00-04:00",
            "title": "Neptune's Magnetosphere",
            "description": "Earth's magnetic field creates a 'bubble' around Earth that helps protect our planet from some of the more harmful effects of energetic particles streaming out from the sun in the solar wind.  Some of the earliest hints of this interaction go back to the 1850s with the work of Richard Carrington, and in the early 1900s with the work of Kristian Birkeland and Carl Stormer.  That this field might form a type of 'bubble' around Earth was hypothesized by Sidney Chapman and Vincent Ferraro in the 1930s.  The term 'magnetosphere' was applied to magnetic bubble by Thomas Gold in 1959.  But it wasn't until the Space Age, when we sent the first probes to other planets, that we found clear evidence of their magnetic fields (though there were hints of a magnetic field for Jupiter in the 1950s, due to observations from radio telescopes).  The Voyager program , two spacecraft launched in 1977, and successors to the Pioneer 10 and 11 missions, completed flybys of the giant outer planets.  They became the implementation of the 'Grand Tour' of the outer planets originally proposed in the late 1960s.  The Voyagers provided some of the first detailed measurments of the strength, extent and diversity of the magnetospheres of the outer planets.In these visualizations, we present simplified models of these planetary magnetospheres, designed to illustrate their scale, and basic features of their structure and impacts of the magnetic axes offset from the planetary rotation axes. The rotation axis of Neptune is highly tilted relative to the revolution axis of the solar system, but nowhere near as extreme as Uranus.  It's magnetic axis also has a large tilt relative to the rotation axis.  These effects combine to not only give Uranus a more a more variable magnetosphere, but suggest the planet's magnetic field may be generated by a different mechanism than that of Earth, Jupiter and Saturn.For these visualizations, the magnetic field structure is represented by gold/copper lines.  Some additional glyphs are provided to indicate some key directions in the field model.The Yellow arrow points towards the sun.  The magnetotail is pointed in the opposite direction.The Cyan arrow represents the magnetic axis, usually tilted relative to the rotation axis.  The arrow indicates the NORTH magnetic pole (convention has field lines moving north to south as the north pole of bar magnet (and compass pointer) points to the south magnetic pole).The Blue arrow represents the north rotation axis.  It is part of the 3-D axis glyph (red, green, and blue arrows) included to make the planetary rotation more apparent.The semi-transparent grey mesh in the distance represents the boundary of the magnetosphere.Major satellites of the planetary system are also included.  When appropriate for the time window of the visualization, the Voyager flyby trajectories are indicated.The models are constructed by combining the fields of a simple magnetic dipole, a current sheet (whose intensity is tuned match the scale of the magnetotail), and occasionally a ring current.  This is a variation of the simple Luhmann-Friesen magnetosphere model.  They are meant to be representative of the basic characteristics of the planetary magnetic fields.  Some features NOT included are longitudes of magnetic poles to a standard planetary coordinate system and offsets of the dipole center from the planetary center.  ReferencesT. Gold, Motions in the Magnetosphere of the EarthLuhmann & Friesen, A simple model of the magnetosphereMagnetic reconnection at Neptune's magnetopauseLASP: Polarity of planetary magnetic fieldsWikipedia: The Solar Storm of 1859Wikipedia: Kristian BirkelandWikipedia: Carl StørmerSpecial thanks to Arik Posner (NASA/HQ) and Gina DiBraccio (UMBC/GSFC) for helpful pointers on orientation of planetary rotation and magnetic axes. || ",
            "hits": 272
        },
        {
            "id": 4333,
            "url": "https://svs.gsfc.nasa.gov/4333/",
            "result_type": "Visualization",
            "release_date": "2015-07-29T10:00:00-04:00",
            "title": "MMS Spacecraft Transition to Tetrahedral Flying Formation",
            "description": "This movie illustrates two orbits of the four MMS spacecraft. || Helio2015A.MMSPursuit.fieldlines_RigRHS.HD1080i.0570_print.jpg (1024x576) [111.7 KB] || Helio2015A.MMSPursuit.fieldlines_RigRHS.HD1080i.0570_searchweb.png (320x180) [72.4 KB] || Helio2015A.MMSPursuit.fieldlines_RigRHS.HD1080i.0570_thm.png (80x40) [4.3 KB] || 1920x1080_16x9_30p (1920x1080) [0 Item(s)] || Helio2015A.MMSPursuit.fieldlines.HD1080.webm (1920x1080) [5.8 MB] || Helio2015A_1080p30.mp4 (1920x1080) [79.2 MB] || Helio2015A.MMSPursuit.fieldlines.HD1080.mov (1920x1080) [313.6 MB] || ",
            "hits": 54
        },
        {
            "id": 11003,
            "url": "https://svs.gsfc.nasa.gov/11003/",
            "result_type": "Produced Video",
            "release_date": "2012-06-19T00:00:00-04:00",
            "title": "Excerpt from \"Dynamic Earth\"",
            "description": "A giant explosion of magnetic energy from the sun, called a coronal mass ejection, slams into and is deflected completely by the Earth's powerful magnetic field. The sun also continually sends out streams of light and radiation energy. Earth's atmosphere acts like a radiation shield, blocking quite a bit of this energy.Much of the radiation energy that makes it through is reflected back into space by clouds, ice and snow and the energy that remains helps to drive the Earth system, powering a remarkable planetary engine — the climate. It becomes the energy that feeds swirling wind and ocean currents as cold air and surface waters move toward the equator and warm air and water moves toward the poles — all in an attempt to equalize temperatures around the world.A jury appointed by the National Science Foundation (NSF) and Science magazine has selected \"Excerpt from Dynamic Earth\" as the winner of the 2013 NSF International Science and Engineering Visualization Challenge for the Video category. This animation will be highlighted in the February 2014 special section of Science and will be hosted on ScienceMag.org and NSF.govThis animation was selected for the Computer Animation Festival's Electronic Theater at the Association for Computer Machinery's Special Interest Group on Computer Graphics and Interactive Techniques (SIGGRAPH), a prestigious computer graphics and technical research forum. This is an excerpt from the fulldome, high-resolution show 'Dynamic Earth: Exploring Earth's Climate Engine.' The Dynamic Earth dome show was selected as a finalist in the Jackson Hole Wildlife Film Festival Science Media Awards under the category \"Best Immersive Cinema - Fulldome\". || ",
            "hits": 110
        },
        {
            "id": 3902,
            "url": "https://svs.gsfc.nasa.gov/3902/",
            "result_type": "Visualization",
            "release_date": "2012-01-24T00:00:00-05:00",
            "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. || ",
            "hits": 153
        },
        {
            "id": 3822,
            "url": "https://svs.gsfc.nasa.gov/3822/",
            "result_type": "Visualization",
            "release_date": "2011-02-14T00:00:00-05:00",
            "title": "Stereoscopic Magnetic Field Lines",
            "description": "This stereoscopic visualization shows a simple model of the Earth's magnetic field. The magnetic field partially shields the Earth from harmful charged particles emanating from the sun. The field is stretched back away from Sun by solar particle and radiation pressures.The geomagnetic field is generated (and regenerated) as the conducting fluid of the Earth's mantle and core, driven by convection of heat from deeper in the interior, induces an electromotive force (EMF) with the existing magnetic field.  This process is very similar to the way an electric generator generates a voltage.  That voltage then drives an induced current in the conducting fluid, which also produces a magnetic field.  This feedback mechanism helps maintain the field, continuously converting the thermal energy in the Earth into magnetic field energy.The magnetic field line data used in this visualization is from a simplified static model. More complex models deform the magnetic field over time as the Earth rotates and experiences solar pressures. Many of the field lines (particulary near the back, away from the Sun) should eventually connect (north and south poles), but the 3d model used in this visualization does not extend far enough to see this.The day/night terminator is aligned with the Sun and is therefore aligned with the magnetic field too. This visualization is based on a previous monoscopic visualizaton that included magnetic field line data. || ",
            "hits": 225
        },
        {
            "id": 3605,
            "url": "https://svs.gsfc.nasa.gov/3605/",
            "result_type": "Visualization",
            "release_date": "2009-07-06T00:00:00-04:00",
            "title": "Magnetospheric Multiscale Mission (MMS) Dayside Orbit Animation for the Preliminary Design Review (PDR)",
            "description": "This visualization uses simulated ephemerides to show the proposed orbits of the Magnetospheric Multiscale Mission (MMS) during the \"dayside magnetosheath/magnetopause\" orbit phase. The movie initially shows the general orientation of the orbit with respect to the Earth, Moon, and Sun. It then zooms in to \"ride\" along with the spacecraft. We then zoom in even closer to show that there are actually four spacecraft flying in a tetrahedral formation. Finally, we see how the 4 spacecraft skim the magnetosheath such that, occasionally, some of the spacecraft are inside (e.g., MMS #1) and some are outside (e.g., MMS #2, #3, and #4) of the magnetosheath boundary.This visualization was created in support of the MMS Preliminary Design Review (PDR) which was held May 4 - 7, 2009. || ",
            "hits": 35
        },
        {
            "id": 3606,
            "url": "https://svs.gsfc.nasa.gov/3606/",
            "result_type": "Visualization",
            "release_date": "2009-07-06T00:00:00-04:00",
            "title": "Magnetospheric Multiscale Mission (MMS) Nightside Orbit Animation for the Preliminary Design Review (PDR)",
            "description": "This visualization uses simulated ephemerides to show the proposed orbits of the Magnetospheric Multiscale Mission (MMS) during the \"nightside\" orbit phase. The movie initially shows the general orientation of the orbit with respect to the Earth, Moon, and Sun. It then moves in towards the Earth revealing Earth's magnetic field. The camera then moves down towards the dark side of the Earth showing how MMS will fly through the tail of the magnetosphereThis visualization was created in support of the MMS Preliminary Design Review (PDR) which was held May 4th through May 7th of 2009. || ",
            "hits": 36
        }
    ]
}