{ "count": 18, "next": null, "previous": null, "results": [ { "id": 4164, "url": "https://svs.gsfc.nasa.gov/4164/", "result_type": "Visualization", "release_date": "2014-05-07T10:00:00-04:00", "title": "A Multi-Mission View of a Solar Flare: Optical to Gamma-rays", "description": "To improve our understanding of complex phenomena such as solar flares, a wide variety of tools are needed. In the case of astronomy, those tools enable us to analyze the light in many different wavelengths and many different ways.Many different instruments are observing the Sun almost continuously, both from space and on the surface of the Earth. On March 29, 2014, the Dunn Solar Telescope at Sacramento Peak, New Mexico was observing a solar active region and requested other observatories to watch as well. As a result of this coordination, the region was being observed by a large number of different instruments, ground and space-based, when it subsequently erupted with an X-class flare. This visualization presents various combinations of the datasets collected during this effort. The color text represents the dominant color of the dataset in the imagery.Solar Dynamics Observatory (SDO): HMI (617.1nm). This data represents the Sun is visible light similar to how we see it from the ground.Solar Dynamics Observatory (SDO): AIA (17.1nm). Solar ultraviolet emission, which can only be seen from space, reveals plasma flowing, and escaping, along magnetic fields.IRIS Slit-Jaw Imager: 140.0nm. This high-resolution imager also contains a slit (the dark vertical line in the center of the field) which directs the light to an ultraviolet spectrometer which is used to extract even more information about the light. The imager slews back-and-forth across the region, providing spectra over a larger area of the Sun.Hinode/X-ray Telescope: x-ray band. Indicates very hot plasma.RHESSI: 50-100 keV. High-energy gamma-ray emission. Emission from these locations represent the very highest energy photons from the flare event.Dunn Solar Telescope: G-band filter. This filter, showing much of the solar surface (photosphere) in visible light, provides a detailed view of the sunspots and convection cells. The view moves because the instrument was repointed several times during the observation.Dunn Solar Telescope: IBIS ( Hydrogen alpha, 656.3nm; Calcium 854.2 nm; Iron 630.15nm). This is the small rectangular view within the Dunn Solar Telescope G-band view. This instrument can tune the wavelength during the observation, which provides views of the solar atmosphere at different depths. || ", "hits": 30 }, { "id": 3595, "url": "https://svs.gsfc.nasa.gov/3595/", "result_type": "Visualization", "release_date": "2009-07-27T00:00:00-04:00", "title": "Sentinels of the Heliosphere", "description": "Heliophysics is a term to describe the study of the Sun, its atmosphere or the heliosphere, and the planets within it as a system. As a result, it encompasses the study of planetary atmospheres and their magnetic environment, or magnetospheres. These environments are important in the study of space weather.As a society dependent on technology, both in everyday life, and as part of our economic growth, space weather becomes increasingly important. Changes in space weather, either by solar events or geomagnetic events, can disrupt and even damage power grids and satellite communications. Space weather events can also generate x-rays and gamma-rays, as well as particle radiations, that can jeopardize the lives of astronauts living and working in space.This visualization tours the regions of near-Earth orbit; the Earth's magnetosphere, sometimes called geospace; the region between the Earth and the Sun; and finally out beyond Pluto, where Voyager 1 and 2 are exploring the boundary between the Sun and the rest of our Milky Way galaxy. Along the way, we see these regions patrolled by a fleet of satellites that make up NASA's Heliophysics Observatory Telescopes. Many of these spacecraft do not take images in the conventional sense but record fields, particle energies and fluxes in situ. Many of these missions are operated in conjunction with international partners, such as the European Space Agency (ESA) and the Japanese Space Agency (JAXA).The Earth and distances are to scale. Larger objects are used to represent the satellites and other planets for clarity.Here are the spacecraft featured in this movie:Near-Earth Fleet:Hinode: Observes the Sun in multiple wavelengths up to x-rays. SVS pageRHESSI : Observes the Sun in x-rays and gamma-rays. SVS pageTRACE: Observes the Sun in visible and ultraviolet wavelengths. SVS pageTIMED: Studies the upper layers (40-110 miles up) of the Earth's atmosphere.FAST: Measures particles and fields in regions where aurora form.CINDI: Measures interactions of neutral and charged particles in the ionosphere. AIM: Images and measures noctilucent clouds. SVS pageGeospace Fleet:Geotail: Conducts measurements of electrons and ions in the Earth's magnetotail. Cluster: This is a group of four satellites which fly in formation to measure how particles and fields in the magnetosphere vary in space and time. SVS pageTHEMIS: This is a fleet of five satellites to study how magnetospheric instabilities produce substorms. SVS pageL1 Fleet: The L1 point is a Lagrange Point, a point between the Earth and the Sun where the gravitational pull is approximately equal. Spacecraft can orbit this location for continuous coverage of the Sun.SOHO: Studies the Sun with cameras and a multitude of other instruments. SVS pageACE: Measures the composition and characteristics of the solar wind. Wind: Measures particle flows and fields in the solar wind. Heliospheric FleetSTEREO-A and B: These two satellites observe the Sun, with imagers and particle detectors, off the Earth-Sun line, providing a 3-D view of solar activity. SVS pageHeliopause FleetVoyager 1 and 2: These spacecraft conducted the original 'Planetary Grand Tour' of the solar system in the 1970s and 1980s. They have now travelled further than any human-built spacecraft and are still returning measurements of the interplanetary medium. SVS pageThis enhanced, narrated visualization was shown at the SIGGRAPH 2009 Computer Animation Festival in New Orleans, LA in August 2009; an eariler version created for AGU was called NASA's Heliophysics Observatories Study the Sun and Geospace. || ", "hits": 89 }, { "id": 3570, "url": "https://svs.gsfc.nasa.gov/3570/", "result_type": "Visualization", "release_date": "2008-12-15T00:00:00-05:00", "title": "NASA's Heliophysics Observatories Study the Sun and Geospace", "description": "Heliophysics is a term to describe the study of the Sun, its atmosphere or the heliosphere, and the planets within it as a system. As a result, it encompasses the study of planetary atmospheres and their magnetic environment, or magnetospheres. These environments are important in the study of space weather.As a society dependent on technology, both in everyday life, and as part of our economic growth, space weather becomes increasingly important. Changes in space weather, either by solar events or geomagnetic events, can disrupt and even damage power grids and satellite communications. Space weather events can also generate x-rays and gamma-rays, as well as particle radiations, that can jeopardize the lives of astronauts living and working in space.This visualization tours the regions of near-Earth orbit; the Earth's magnetosphere, sometimes called geospace; the region between the Earth and the Sun; and finally out beyond Pluto, where Voyager 1 and 2 are exploring the boundary between the Sun and the rest of our Milky Way galaxy. Along the way, we see these regions patrolled by a fleet of satellites that make up NASA's Heliophysics Observatory Telescopes. Many of these spacecraft do not take images in the conventional sense but record fields, particle energies and fluxes in situ. Many of these missions are operated in conjunction with international partners, such as the European Space Agency (ESA) and the Japanese Space Agency (JAXA).The Earth and distances are to scale. Larger objects are used to represent the satellites and other planets for clarity.Here are the spacecraft featured in this movie:Near-Earth Fleet:Hinode: Observes the Sun in multiple wavelengths up to x-rays. SVS pageRHESSI : Observes the Sun in x-rays and gamma-rays. SVS pageTRACE: Observes the Sun in visible and ultraviolet wavelengths. SVS pageTIMED: Studies the upper layers (40-110 miles up) of the Earth's atmosphere.FAST: Measures particles and fields in regions where aurora form.CINDI: Measures interactions of neutral and charged particles in the ionosphere. AIM: Images and measures noctilucent clouds. SVS pageGeospace Fleet:Geotail: Conducts measurements of electrons and ions in the Earth's magnetotail. Cluster: This is a group of four satellites which fly in formation to measure how particles and fields in the magnetosphere vary in space and time. SVS pageTHEMIS: This is a fleet of five satellites to study how magnetospheric instabilities produce substorms. SVS pageL1 Fleet: The L1 point is a Lagrange Point between the Sun and the Earth. Spacecraft can orbit this location for continuous coverage of the Sun.SOHO: Studies the Sun with cameras and a multitude of other instruments. SVS pageACE: Measures the composition and characteristics of the solar wind. Wind: Measures particle flows and fields in the solar wind. Heliospheric FleetSTEREO-A and B: These two satellites observe the Sun, with imagers and particle detectors, off the Earth-Sun line, providing a 3-D view of solar activity. SVS pageHeliopause FleetVoyager 1 and 2: These spacecraft conducted the original 'Planetary Grand Tour' of the solar system in the 1970s and 1980s. They have now travelled further than any human-built spacecraft and are still returning measurements of the interplanetary medium. SVS pageA refined and narrated version of this visualization, Sentinels of the Heliosphere, is now available. || ", "hits": 103 }, { "id": 3162, "url": "https://svs.gsfc.nasa.gov/3162/", "result_type": "Visualization", "release_date": "2005-05-24T12:00:00-04:00", "title": "RHESSI and TRACE View of January 20, 2005 Solar Flare", "description": "RHESSI spacecraft images of gamma-rays (blue) and X-rays (red) thrown off by the hottest part of the flare are shown with UV images from the TRACE spacecraft. The gamma rays are made by energetic protons at the Sun. Scientists were surprised that the gamma rays matched the energy spectrum of protons at Earth: the proton storm may have come directly from the Sun and not from the CME as anticipated. || ", "hits": 42 }, { "id": 3111, "url": "https://svs.gsfc.nasa.gov/3111/", "result_type": "Visualization", "release_date": "2005-02-18T12:00:00-05:00", "title": "Connections: Terrestrial Gamma Flashes and Lightning?", "description": "The RHESSI instrument not only views the Sun but can detect gamma-rays from sources on Earth as well. || ", "hits": 16 }, { "id": 2750, "url": "https://svs.gsfc.nasa.gov/2750/", "result_type": "Visualization", "release_date": "2003-09-02T12:00:00-04:00", "title": "RHESSI Observes 2.2 MeV Line Emission from a Solar Flare", "description": "The solar flare at Active Region 10039 on July 23, 2002 exhibits many exceptional high-energy phenomena including the 2.223 MeV neutron capture line and the 511 keV electron-positron (antimatter) annihilation line. In the animation, the RHESSI low-energy channels (12-25 keV) are represented in red and appears predominantly in coronal loops. The high-energy flux appears as blue at the footpoints of the coronal loops. Violet is used to indicate the location and relative intensity of the 2.2MeV emission. || ", "hits": 35 }, { "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": 25 }, { "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": 14 }, { "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": 24 }, { "id": 2458, "url": "https://svs.gsfc.nasa.gov/2458/", "result_type": "Visualization", "release_date": "2002-06-05T12:00:00-04:00", "title": "RHESSI Observes the Flare over AR9906 - Time Tagged", "description": "Close-up view of the solar active region AR9906 on April 21, 2002 with TRACE and RHESSI data. RHESSI observes x-rays from this flare. The red contours represent the 12-25 keV photon energy range and the blue contours represent 50-100 keV. || ", "hits": 13 }, { "id": 2459, "url": "https://svs.gsfc.nasa.gov/2459/", "result_type": "Visualization", "release_date": "2002-06-05T12:00:00-04:00", "title": "RHESSI Observes the Flare over AR9906 - No time tags", "description": "Close-up view of the solar active region AR9906 on April 21, 2002 with TRACE data and RHESSI. RHESSI observes x-rays from this flare. The red contours represent the 12-25 keV photon energy range and the blue contours represent 50-100 keV. || ", "hits": 15 }, { "id": 2460, "url": "https://svs.gsfc.nasa.gov/2460/", "result_type": "Visualization", "release_date": "2002-06-05T12:00:00-04:00", "title": "RHESSI Observes the Flare over AR9906 - zoom with times", "description": "Zoom in to solar active region AR9906 on April 21, 2002 with SOHO/EIT, TRACE and RHESSI data. RHESSI observes x-rays from this flare. The red contours represent the 12-25 keV photon energy range and the blue contours represent 50-100 keV. || Movie of RHESSI and TRACE data. || a002460.00100_print.png (720x480) [447.6 KB] || ar9906-zoom-dates_pre.jpg (320x240) [6.9 KB] || a002460.webmhd.webm (960x540) [6.9 MB] || ar9906-zoom-dates.mpg (640x480) [15.0 MB] || a002460.dv (720x480) [118.8 MB] || ", "hits": 25 }, { "id": 2461, "url": "https://svs.gsfc.nasa.gov/2461/", "result_type": "Visualization", "release_date": "2002-06-05T12:00:00-04:00", "title": "RHESSI Observes the Flare over AR9906 - zoom without times", "description": "Zoom in to solar active region AR9906 on April 21, 2002 with SOHO/EIT, TRACE and RHESSI data. RHESSI observes x-rays from this flare. The red contours represent the 12-25 keV photon energy range and the blue contours represent 50-100 keV. || ", "hits": 21 }, { "id": 2462, "url": "https://svs.gsfc.nasa.gov/2462/", "result_type": "Visualization", "release_date": "2002-06-05T12:00:00-04:00", "title": "RHESSI Observes the Flare over AR9906 - rotate view with times", "description": "Zoom in (with rotation) to solar active region AR9906 on April 21, 2002 with SOHO/EIT,TRACE and RHESSI data. RHESSI observes x-rays from this flare. The red contours represent the 12-25 keV photon energy range and the blue contours represent 50-100 keV. || ", "hits": 36 }, { "id": 2463, "url": "https://svs.gsfc.nasa.gov/2463/", "result_type": "Visualization", "release_date": "2002-06-05T12:00:00-04:00", "title": "RHESSI Observes the Flare over AR9906 - Rotate View Without Times", "description": "Zoom in (with rotation) to solar active region AR9906 on April 21, 2002 with SOHO/EIT, TRACE and RHESSI data. RHESSI observes x-rays from this flare. The red contours represent the 12-25 keV photon energy range and the blue contours represent 50-100 keV. || ", "hits": 22 }, { "id": 2402, "url": "https://svs.gsfc.nasa.gov/2402/", "result_type": "Visualization", "release_date": "2002-03-20T12:00:00-05:00", "title": "First Flare movie for the RHESSI Instrument (Speed 105x Normal)", "description": "An animation of an M-class flare viewed by the RHESSI instrument on February 20, 2002. On tape, this version plays at the maximum speed of one frame corresponding to 3.5 seconds of data collection time. The flare was located at -17.8 degrees South, 9.8 degrees West (heliographic coordinates) in NOAA active region number 9830. || ", "hits": 19 }, { "id": 2403, "url": "https://svs.gsfc.nasa.gov/2403/", "result_type": "Visualization", "release_date": "2002-03-20T12:00:00-05:00", "title": "First Flare Movie for the RHESSI Instrument (Speed 52x Normal)", "description": "An animation of an M-class flare viewed by the RHESSI instrument on February 20, 2002. On tape, this version plays at a speed of two video frames corresponding to 3.5 seconds of data collection time. The flare was located at -17.8 degrees South, 9.8 degrees West (heliographic coordinates) in NOAA active region number 9830. || ", "hits": 16 }, { "id": 2404, "url": "https://svs.gsfc.nasa.gov/2404/", "result_type": "Visualization", "release_date": "2002-03-20T12:00:00-05:00", "title": "First Flare Movie for the RHESSI Instrument (Speed 26x Normal)", "description": "An animation of an M-class flare viewed by the RHESSI instrument on February 20, 2002. On tape, this version plays at a speed of four video frames corresponding to 3.75 seconds of data collection time. The flare was located at -17.8 degrees South, 9.8 degrees West (heliographic coordinates) in NOAA active region number 9830. || ", "hits": 13 } ] }