{ "count": 7, "next": null, "previous": null, "results": [ { "id": 4623, "url": "http://svs.gsfc.nasa.gov/4623/", "result_type": "Visualization", "release_date": "2018-04-30T10:00:00-04:00", "title": "The Dynamic Solar Magnetic Field with Introduction", "description": "This narrated visualization transitions from a view of the Sun in visible light, to a view in ultraviolet light showing the plasma flowing along solar magnetic structures, to the underlying magnetic field of the solar photosphere, to a model construction of magnetic fieldlines above the photosphere.This video is also available on our YouTube channel. || SolarMagnetism_UHD3840.04000_print.jpg (1024x576) [198.9 KB] || SolarMagnetism_UHD3840.04000_thm.png (80x40) [6.0 KB] || SolarMagnetism_UHD3840.04000_web.png (320x180) [84.1 KB] || SolarMagnetism_ProRes3_HD1080_p30_Narrated.webm (1280x720) [33.9 MB] || SolarMagnetism_ProRes3_HD1080_p30_Narrated.mov (1280x720) [7.4 GB] || SolarMagnetism_ProRes3_UHD2160_p30_Narrated.mov (3840x2160) [12.8 GB] || ", "hits": 147 }, { "id": 4391, "url": "http://svs.gsfc.nasa.gov/4391/", "result_type": "Visualization", "release_date": "2016-01-29T10:00:00-05:00", "title": "The Dynamic Solar Magnetic Field", "description": "A visualization of the slow changes of the solar magnetic field over the course of four years. || PFSSbasicView_inertial.HD1080i.0400_print.jpg (1024x576) [168.7 KB] || PFSSbasicView_inertial.HD1080i.0400_searchweb.png (180x320) [78.9 KB] || PFSSbasicView_inertial.HD1080i.0400_thm.png (80x40) [5.8 KB] || PFSSbasicView_inertial_1080p30.webm (1920x1080) [18.1 MB] || PFSSbasicView (1920x1080) [128.0 KB] || PFSSbasicView_inertial_1080p30.mp4 (1920x1080) [326.6 MB] || PFSSbasicView_inertial_1080p10.mp4 (1920x1080) [470.2 MB] || PFSSbasicView_HD1080p10.mov (1920x1080) [804.4 MB] || PFSSbasicView_inertial_1080p30.mp4.hwshow [232 bytes] || ", "hits": 197 }, { "id": 12104, "url": "http://svs.gsfc.nasa.gov/12104/", "result_type": "Produced Video", "release_date": "2016-01-29T10:00:00-05:00", "title": "The Dynamic Solar Magnetic Field - Narrated", "description": "Holly Gilbert, NASA GSFC solar scientist, explains a model of magnetic fields on the sun. || thumb.jpg (1280x720) [156.8 KB] || thumb_searchweb.png (320x180) [124.7 KB] || thumb_thm.png (80x40) [20.5 KB] || 12104_b-roll.mov (1280x720) [2.0 GB] || 12104_original.mov (1920x1080) [3.8 GB] || 12104_youtube_hq.mov (1920x1080) [1.7 GB] || 12104_appletv.m4v (1280x720) [63.5 MB] || 12104_b-roll.webm (1280x720) [24.5 MB] || 12104_lowres.mp4 (480x272) [19.2 MB] || ", "hits": 87 }, { "id": 11277, "url": "http://svs.gsfc.nasa.gov/11277/", "result_type": "Produced Video", "release_date": "2013-07-09T00:00:00-04:00", "title": "Hot Lines", "description": "Magnetic field lines dance above the surface of the sun. Called coronal loops, these lines are difficult to observe from afar, since they are invisible. Scientists can observe them in two ways: by watching the visible solar material that flows along the lines or by modeling them using computer simulations. Studying these formations help us understand the way energy travels on and around the sun. The Solar and Heliospheric Observatory, or SOHO, is a sun-observing spacecraft that can measure and depict distortions in the sun’s magnetic field. Using data collected by the spacecraft, scientists created a virtual, 3D model of the field lines. Watch the video to explore the loops. || ", "hits": 41 }, { "id": 3346, "url": "http://svs.gsfc.nasa.gov/3346/", "result_type": "Visualization", "release_date": "2006-03-30T00:00:00-05:00", "title": "Grand Tour of the Coronal Loops Model", "description": "This is a longer coronal loops tour combining components of the two previous versions (Animation IDs 3286 and 3287). The solar model is constructed from magnetogram data collected by SOHO/MDI. Because we do not see the full solar surface at any one time, the magnetograms collected over the course of a solar rotation are processed through a time-evolving solar surface model which provides a snapshot of the surface at a fixed time. The resulting magnetogram is then processed through the Potential Field Source Surface (PFSS) model which constructs the magnetic field above the solar surface. The magnetic field around the Sun is then analyzed for field lines, which creates the loop structures we see in the model. Hot plasma tends to flow along the magnetic field lines, creating the coronal loops. These loops are only visible at the higher temperatures corresponding to ultraviolet light, in this case, 195 angstroms, one of the filter wavelengths of SOHO/EIT. For this version, we color the coronal loops green for ready comparison to the EIT 195 angstrom imagery using the EIT standard color table. || ", "hits": 102 }, { "id": 3211, "url": "http://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": 18 }, { "id": 3212, "url": "http://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": 22 } ] }