{
    "count": 9,
    "next": null,
    "previous": null,
    "results": [
        {
            "id": 14707,
            "url": "https://svs.gsfc.nasa.gov/14707/",
            "result_type": "Produced Video",
            "release_date": "2024-11-25T11:00:00-05:00",
            "title": "XRISM's Resolve Instrument Gazes into Cygnus X-3",
            "description": "Cygnus X-3 is a high-mass X-ray binary system consisting of a compact object (likely a black hole) and a Wolf-Rayet star. This artist's concept shows one interpretation of the system. High-resolution X-ray spectroscopy indicates two gas components: a heavy background outflow, or wind, produced by the massive star and a turbulent structure — perhaps a wake carved into the wind — located close to the orbiting companion. As shown here, a black hole's gravity captures some of the wind into an accretion disk around it, and the disk's orbital motion sculpts a path (yellow arc) through the streaming gas. During strong outbursts, the companion emits jets of particles moving near the speed of light, seen here extending above and below the black hole.Credit: NASA’s Goddard Space Flight CenterAlt text: Illustration of the Cygnus X-3 systemImage description: On a cloudy reddish background, a bright blue-white circle — a representation of a hot, bright, massive star — sits near the center. Wisps of blue-white border its edges, and many lines of similar color radiate from it. In the foreground at about 4 o’clock lies a yellowish ring with a black hole in its center. From the ring trails a diffuse yellow arc, sweeping from right to left and exiting at the bottom of the illustration. Extending above and below the black hole are two blue-white triangles representing particle jets. || Cyg_X-3_illustration_4K.jpg (3840x2160) [505.1 KB] || Cyg_X-3_illustration_4K_print.jpg (1024x576) [58.5 KB] || Cyg_X-3_illustration_4K_searchweb.png (320x180) [64.7 KB] || Cyg_X-3_illustration_4K_web.png (320x180) [64.7 KB] || Cyg_X-3_illustration_4K_thm.png (80x40) [6.1 KB] || ",
            "hits": 233
        },
        {
            "id": 10406,
            "url": "https://svs.gsfc.nasa.gov/10406/",
            "result_type": "Produced Video",
            "release_date": "2009-04-01T00:00:00-04:00",
            "title": "GEMS X-Ray Detector Animation",
            "description": "X-Ray detector animation for proposed GEMS mission. || detectorNEWEST0600.00562_print.jpg (1024x576) [42.1 KB] || detectorNEWEST0600_web.png (320x180) [176.8 KB] || detectorNEWEST0600_thm.png (80x40) [15.0 KB] || detector_720p.webmhd.webm (960x540) [6.1 MB] || 1280x720_16x9_60p (1280x720) [128.0 KB] || detector_720p.m2v (1280x720) [28.3 MB] || a010406_detector_720p.mp4 (640x360) [4.0 MB] || detector_512x288.m1v (512x288) [6.1 MB] || ",
            "hits": 41
        },
        {
            "id": 1,
            "url": "https://svs.gsfc.nasa.gov/1/",
            "result_type": "Visualization",
            "release_date": "1990-07-10T12:00:00-04:00",
            "title": "Tidal Streams in Massive X-ray Binary Systems",
            "description": "A tiny neutron star orbits incessantly around a massive star with a diameter a million times larger than its own.  The high luminosity of the massive star drives a strong wind from its surface.  The neutron star crashes through this wind at over 300 kilometers per second.  The gravity and X-ray luminosity of the neutron star act to disrupt the wind, producing an extended wake of dense gas trailing behind the neutron star.  In this simulation, the tidal distortion of the primary star and the resultant tidal stream is shown.  The numerical simulations depicted here were computed using the Cray X-MP 48 at the National Center for Supercomputing Applications, University of Illinois, Urbana-Champaign. || ",
            "hits": 106
        },
        {
            "id": 2,
            "url": "https://svs.gsfc.nasa.gov/2/",
            "result_type": "Visualization",
            "release_date": "1990-07-10T12:00:00-04:00",
            "title": "Tidal Streams in Massive X-ray Binary Systems: Neutron Star Close-up",
            "description": "A tiny neutron star orbits incessantly around a massive star with a diameter a million times larger than its own.  The high luminosity of the massive star drives a strong wind from its surface.  The neutron star crashes through this wind at over 300 kilometers per second.  The gravity and X-ray luminosity of the neutron star act to disrupt the wind, producing an extended wake of dense gas trailing behind the neutron star.  In this simulation, the tidal distortion of the primary star and the resultant tidal stream is shown.  The numerical simulations depicted here were computed using the Cray X-MP 48 at the National Center for Supercomputing Applications, University of Illinois, Urbana-Champaign. || ",
            "hits": 81
        },
        {
            "id": 3,
            "url": "https://svs.gsfc.nasa.gov/3/",
            "result_type": "Visualization",
            "release_date": "1990-07-10T12:00:00-04:00",
            "title": "Stellar Wind Disruption by an Orbiting Neutron Star",
            "description": "A tiny neutron star orbits incessantly around a massive star with a diameter a million times larger than its own.  The high luminosity of the massive star drives a strong wind from its surface.  The neutron star crashes through this wind at over 300 kilometers per second.  The gravity and X-ray luminosity of the neutron star act to disrupt the wind, producing an extended wake of dense gas trailing behind the neutron star.The numerical simulations depicted here were computed using the Cray X-MP 48 at the National Center for Supercomputing Applications, University of Illinois, Urbana-Champaign. || ",
            "hits": 117
        },
        {
            "id": 4,
            "url": "https://svs.gsfc.nasa.gov/4/",
            "result_type": "Visualization",
            "release_date": "1990-07-10T12:00:00-04:00",
            "title": "Stellar Wind Disruption by an Orbiting Neutron Star: Low X-Ray Luminosity",
            "description": "A tiny neutron star orbits incessantly around a massive star with a diameter a million times larger than its own.  The high luminosity of the massive star drives a strong wind from its surface.  The neutron star crashes through this wind at over 300 kilometers per second.  The gravity and X-ray luminosity of the neutron star act to disrupt the wind, producing an extended wake of dense gas trailing behind the neutron star.  This simulation, in the reference frame of the neutron star, shows conditions of low X-ray luminosity. in which there is a small accretion radius, a slight asymmetry, and short timescales for variability.The numerical simulations depicted here were computed using the Cray X-MP 48 at the National Center for Supercomputing Applications, University of Illinois, Urbana-Champaign. || ",
            "hits": 68
        },
        {
            "id": 5,
            "url": "https://svs.gsfc.nasa.gov/5/",
            "result_type": "Visualization",
            "release_date": "1990-07-10T12:00:00-04:00",
            "title": "Stellar Wind Disruption by an Orbiting Neutron Star: Moderate X-Ray Luminosity",
            "description": "A tiny neutron star orbits incessantly around a massive star with a diameter a million times larger than its own.  The high luminosity of the massive star drives a strong wind from its surface.  The neutron star crashes through this wind at over 300 kilometers per second.  The gravity and X-ray luminosity of the neutron star act to disrupt the wind, producing an extended wake of dense gas trailing behind the neutron star.  This simulation, in the reference frame of the neutron star, shows conditions of low X-ray luminosity. in which there is a large accretion radius, significant asymmetry, and long timescales for variability.The numerical simulations depicted here were computed using the Cray X-MP 48 at the National Center for Supercomputing Applications, University of Illinois, Urbana-Champaign. || ",
            "hits": 70
        },
        {
            "id": 6,
            "url": "https://svs.gsfc.nasa.gov/6/",
            "result_type": "Visualization",
            "release_date": "1990-07-10T12:00:00-04:00",
            "title": "Stellar Wind Disruption by an Orbiting Neutron Star: High X-Ray Luminosity",
            "description": "A tiny neutron star orbits incessantly around a massive star with a diameter a million times larger than its own. The high luminosity of the massive star drives a strong wind from its surface. The neutron star crashes through this wind at over 300 kilometers per second. The gravity and X-ray luminosity of the neutron star act to disrupt the wind, producing an extended wake of dense gas trailing behind the neutron star. This simulation, in the reference frame of the neutron star, shows conditions of high X-ray luminosity, in which there is a weak bow shock, no oscillation, and a large photoionization wake. The numerical simulations depicted here were computed using the Cray X-MP 48 at the National Center for Supercomputing Applications, University of Illinois, Urbana-Champaign. || ",
            "hits": 58
        },
        {
            "id": 7,
            "url": "https://svs.gsfc.nasa.gov/7/",
            "result_type": "Visualization",
            "release_date": "1990-07-10T12:00:00-04:00",
            "title": "Stellar Wind Disruption by an Orbiting Neutron Star: Neutron Star Close-up",
            "description": "A tiny neutron star orbits incessantly around a massive star with a diameter a million times larger than its own.  The high luminosity of the massive star drives a strong wind from its surface.  The neutron star crashes through this wind at over 300 kilometers per second.  The gravity and X-ray luminosity of the neutron star act to disrupt the wind, producing an extended wake of dense gas trailing behind the neutron star.  The large scale structure seen in the accretion wake is powered by the release of gravitational potential energy near the surface of the neutron star.The numerical simulations depicted here were computed using the Cray X-MP 48 at the National Center for Supercomputing Applications, University of Illinois, Urbana-Champaign. || ",
            "hits": 67
        }
    ]
}