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    "results": [
        {
            "id": 14401,
            "url": "https://svs.gsfc.nasa.gov/14401/",
            "result_type": "Produced Video",
            "release_date": "2023-10-31T10:00:00-04:00",
            "title": "NASA’s Eclipse Art",
            "description": "“The greatest scientists are artists as well.” ~Albert EinsteinArt and science have been treated as separate disciplines but have more in common than is often realized. Creativity is critical to making scientific breakthroughs, and art is often an expression (or product) of scientific knowledge. And both art and science begin in the experience of awe, of beholding something grand. The experience of a solar eclipse is a prime example of where these two human endeavors meet.Eclipses are celestial events we can predict with extreme precision, and their occurrence reveals fundamental truths about our place in the universe. Yet, as many eclipse watchers will attest, there is no anticipating how you will feel when experiencing one. The emotional resonance of eclipses is underlined by their presence in artforms in cultures across the world going back millennia.To celebrate the special role of eclipses in connecting art and science, creatives across NASA will be sharing their eclipse-inspired artwork in anticipation of two solar eclipses that will cross the United States on October 14, 2023, and April 8, 2024.The first two pieces in the series are presented below, with short biographies of their creators. || ",
            "hits": 80
        },
        {
            "id": 13340,
            "url": "https://svs.gsfc.nasa.gov/13340/",
            "result_type": "Produced Video",
            "release_date": "2019-10-10T13:55:00-04:00",
            "title": "How the Visually Impaired Experience Hubble Images",
            "description": "The Hubble Space Telescope is well known for its incredible images. But what of those among us who are visually impaired? To help spread awareness as a part of World Sight Day, this video is meant to share the importance of different ways to share Hubble's astounding images. The book, \"Touch the Universe\" by Noreen Grice features some of Hubble's most well-known photographs; but all of these photos were specially made to include everyone.For more information, visit https://nasa.gov/hubble.Credit: NASA's Goddard Space Flight CenterRebecca Roth: Lead ProducerCourtney Lee: Lead ProducerPaul R. Morris (USRA): Producer / EditorRob Andreoli: VideographerJohn Caldwell: VideographerBradley Hague: VideographerMusic Credits: \"Hercules' by Christian Ort [GEMA], Matthew Tasa [GEMA], Meyer Anthony [GEMA], Siulapwa Cisha [BMI]; Universal Production Music || ",
            "hits": 30
        },
        {
            "id": 31049,
            "url": "https://svs.gsfc.nasa.gov/31049/",
            "result_type": "Hyperwall Visual",
            "release_date": "2019-08-07T00:00:00-04:00",
            "title": "The A-Train & C-Train",
            "description": "A-Train_C-Train_TimeSeps2018_HW || A-Train_C-Train_TimeSeps2018_HW_print.jpg (1024x576) [932.9 KB] || A-Train_C-Train_TimeSeps2018_HW.jpg (5760x3240) [13.3 MB] || A-Train_C-Train_TimeSeps2018_HW_searchweb.png (320x180) [89.3 KB] || A-Train_C-Train_TimeSeps2018_HW_thm.png (80x40) [6.8 KB] || the-a-train-c-train-time-seps.hwshow [315 bytes] || ",
            "hits": 97
        },
        {
            "id": 30469,
            "url": "https://svs.gsfc.nasa.gov/30469/",
            "result_type": "Hyperwall Visual",
            "release_date": "2013-11-01T12:00:00-04:00",
            "title": "Landsat Data Help Water-Resource Managers",
            "description": "In the Western United States between 80 and 90% of freshwater is used for agriculture. In Southern California irrigated farmland stretches southward across the desert from the Salton Sea—an artificial inland sea—to the Mexico border. In the natural-color image [left] acquired on May 15, 2013, by Landsat 8’s Operational Land Imager, blocks of square farmland appear in shades of green and tan, while urban areas such as El Centro, California and Mexicali, Mexico appear in shades of gray. Accurate estimates of total crop area provided by Landsat satellites can be used to help forecast commodities in the United States and the world food market. On that same day, thermal measurements from Landsat 8’s Thermal Infrared Sensor [right] show different temperatures between crop fields as well as urban and desert areas. Cooler areas (e.g., irrigated crops) appear as dark purple and red shades, while warmer areas (e.g., urban and desert areas) appear as shades of bright yellow and white. Plants cool down when they transpire, so the combination of water evaporating from the plants and the ground (i.e., evapotranspiration) lowers the temperature of the irrigated land. Pixels representing cooler areas in thermal images from TIRS help water-resource managers determine where water is being used for irrigation, allowing them to make management decisions on water distribution to preserve this scarce resource. When an earlier design of Landsat 8 did not include a thermal infrared band, the Western States Water Council advocated for its inclusion.Used in 2014 Calendar. || ",
            "hits": 21
        },
        {
            "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": 103
        },
        {
            "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": 195
        },
        {
            "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": 78
        },
        {
            "id": 20169,
            "url": "https://svs.gsfc.nasa.gov/20169/",
            "result_type": "Animation",
            "release_date": "2008-07-22T12:00:00-04:00",
            "title": "LEX / Boomerang Mission",
            "description": "LEX is one of the candidates for inclusion in the LRO mission - LEX will sample the lunar soil as well as search for signs of water. || ",
            "hits": 28
        }
    ]
}