http://www.rssboard.org/rss-specification 720 http://ecuip-xtf.lib.uchicago.edu/xtf/search?docsPerPage%3D100;f78-type%3DArtwork Results for your query: docsPerPage=100;f78-type=Artwork Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/165469main_403GRBCollapsarModelPar_NASAWebV_1/165469main_403GRBCollapsarModelPar_NASAWebV_1.dc.xml The collapsing star scenario that is one of the leading contenders as the cause of gamma-ray bursts. This artist's concept of the collapsar model shows the center of a dying star collapsing minutes before the star implodes and emits a gamma-ray burst that is seen across the universe. Many scientists say longer bursts (more than four seconds in duration) are caused by massive star explosions. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/165469main_403GRBCollapsarModelPar_NASAWebV_1/165469main_403GRBCollapsarModelPar_NASAWebV_1.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/500px-Alfa_beta_gamma_radiation_penetration.svg/500px-Alfa_beta_gamma_radiation_penetration.dc.xml Gamma radiation (which includes gamma rays, X-rays, and ultraviolet radiation) cannot penetrate our atmosphere, but can travel through materials such as paper and aluminum. Only heavy metals (such as lead) and other materials like concrete can block gamma rays. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/500px-Alfa_beta_gamma_radiation_penetration.svg/500px-Alfa_beta_gamma_radiation_penetration.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/64325main_swift-si/64325main_swift-si.dc.xml Swift's three scientific instruments work together to learn as much as possible about gamma-ray bursts. The Burst Alert telescope (BAT) is the first instrument to detect gamma-rays in the quarter of the sky at which it is pointed. Then the satellite is reoriented using data from BAT so that XRT and UVOT, which have a much smaller field of view, can be pointed at the GRB. With this information, ground-based telescopes can be pointed directly at the source to gather more data about the GRB. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/64325main_swift-si/64325main_swift-si.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/68168main_swift-burst_m/6168main_swift-burst_m.dc.xml An artist's concept of the Swift Gamma-Ray Burst Explorer catching a gamma-ray burst. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/68168main_swift-burst_m/6168main_swift-burst_m.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/Air-Shower-Schematic-GC/Air-Shower-Schematic-GC.dc.xml A schematic diagram of particles in an extensive air shower (EAS), approaching an array of detectors at the speed of light. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/Air-Shower-Schematic-GC/Air-Shower-Schematic-GC.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/AtomicPileSketch_apf2-00501r/AtomicPileSketch_apf2-00501r.dc.xml On December 2, 1942 using a nuclear reactor erected under a section of the West Stands of the University of Chicago's Stagg Field, a group of scientists achieved the first self-sustaining chain reaction and thereby initiated a controlled release of nuclear energy. The reactor consisted of uranium and uranium oxide lumps spaced in a cubic lattice embedded in graphite. In 1943, the reactor was dismantled and reassembled at the Argonne National Laboratory. Photographic copy of drawing. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/AtomicPileSketch_apf2-00501r/AtomicPileSketch_apf2-00501r.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/Auger-Animation/Auger-Animation.dc.xml This animation models how an extensive air shower (EAS) is detected by the Pierre Auger Cosmic Ray Observatory Engineering Array. The cosmic ray particles spread out to form a shower front. The shower front is illustrated using green dots to represent electrons and positrons, and red dots to represent muons. Yellow indicates that particles have been detected coincidentally by one of the water tank detectors. Slight differences in the detection times at the various tank positions allow scientists to determine the cosmic ray arrival direction. See the sketch of the cosmic ray creating an air shower and heading towards the detector on the previous page. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/Auger-Animation/Auger-Animation.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/Auger-Animation/sas3_layout/sas3_layout.dc.xml Designed and built at M.I.T, the SAS-3 was a spinning satellite. The spin rate was controlled by a gyroscope that could be commanded to stop rotation so that all instruments could be pointed at a given source. Pointing could provide about 30 minutes of continuous data on a source, such as a pulsar, burster, or transient. This is a diagram of the instruments onboard the SAS-3. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/Auger-Animation/sas3_layout/sas3_layout.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/EMS-penetration-atmosphere/EMS-penetration-atmosphere.dc.xml Only visible, radio, and some infrared radiation penetrates the atmosphere. Ultraviolet photons, X-rays, and gamma rays do not. While observations at any wavelength benefit from instruments in space, detection of celestial of ultraviolet, X-ray, and gamma-ray sources require instruments in space. The development of rockets led to our ability to place these special instruments in space. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/EMS-penetration-atmosphere/EMS-penetration-atmosphere.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/GCN/GCN.dc.xml Schematic of the GRB Coordinates Network (GCN), a system that distributes information about the location of a gamma-ray burst (GRB). The spacecraft sends the GRB location information down to a ground station, which in turn relays it to the GCN at the NASA Goddard Space Flight Center. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/GCN/GCN.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/GRIS_config/GRIS_config.dc.xml Diagram illustrating the placement of the detectors and shields. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/GRIS_config/GRIS_config.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/Geiger_counter_patent/Geiger_counter_patent.dc.xml Friedman holds U.S. Patent No. 2,475,603, for an adaptation of the tube used in a Geiger-Mueller counter. His tube design increased the counter's sensitivity to weak radiation sources by lowering the background noise of the counter itself. Figure 1 (upper left) is a cut-away view of Friedman's counter tube mounted within a container, called a shield. Figure 2 (lower left) is a front-end view of the tube. Figure 3 (upper right) is a cross-section of the tube showing the arrangement of parts and the structure used for mounting the tube within the shield. Figure 4 (lower right) is a cross-section diagram showing the tube anode and cathode, and a plot of the electric field within the tube. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/Geiger_counter_patent/Geiger_counter_patent.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/George-Clark-Harvard/explorer-11_detector/explorer-11_detector.dc.xml Draushaar and Clark’s detector for Explorer 11 was designed to detect gamma rays above 50 MeV. The image on the left shows the detector. It measured 20 inches high, 10 inches in diameter, and weighed about 30 pounds. The image on the right is a diagram of the detector, which consisted of a sandwich crystal scintillator and a Lucite Cherenkov counter, surrounded by a plastic anticoincidence scintillator. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/George-Clark-Harvard/explorer-11_detector/explorer-11_detector.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/HEAO_1/HEAO_1.dc.xml The HEAO project involved the launching of three unmanned scientific observatories into low Earth orbit between 1977 and 1979 to study some of the most intriguing mysteries of the Universe: pulsars, black holes, neutron stars, and supernovae. This artist's conception depicts the High Energy Astronomy Observatory (HEAO)-1 in orbit. HEAO-1 was launched on August 12, 1977, to survey the sky for X-ray and gamma-ray sources, as well as to pinpoint their positions. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/HEAO_1/HEAO_1.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/NASA-Explorer-11-Flight/NASA-Explorer-11-Flight.dc.xml Explorer 11, the first gamma-ray detection satellite flown, was launched on April 27, 1961. The satellite could not be actively pointed, so it was put into a tumble in order to get a "rough" scan of the entire celestial sphere.. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/NASA-Explorer-11-Flight/NASA-Explorer-11-Flight.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/Nested-Paraboloid/Nested-Paraboloid.dc.xml This cutaway illustrates the grazing-incidence design and functioning of the High Resolution Mirror Assembly (HRMA) on the Chandra X-ray Observatory. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/Nested-Paraboloid/Nested-Paraboloid.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/Neutron_Star_Merge_H264_High_960x540/Neutron_Star_Merge_H264_High_960x540.dc.xml Gamma-ray bursts are common, yet random, and fleeting events that have mystified astronomers since their discovery in the late 1960s. Shorter bursts (less than two seconds in duration) are thought to be caused by mergers of binary systems with black holes or neutron stars. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/Neutron_Star_Merge_H264_High_960x540/Neutron_Star_Merge_H264_High_960x540.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/a010300_NeutronStar_NTSC/a010300_NeutronStar_NTSC.dc.xml Gamma-ray flares from SGR J1550-5418 may arise when the magnetar's surface suddenly cracks, releasing energy stored within its powerful magnetic field. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/a010300_NeutronStar_NTSC/a010300_NeutronStar_NTSC.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/aristotle-solar-system/aristotle-solar-system.dc.xml Illustration of Oronce Fine, Astronomy personified and an armillary sphere. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/aristotle-solar-system/aristotle-solar-system.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/chandra_labeled/chandra_labeled.dc.xml Renamed the Chandra X-ray Observatory after launch, this image shows the instruments onboard the observatory. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/chandra_labeled/chandra_labeled.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/coded_aperture/coded_aperture.dc.xml Incoming light hits the coded aperture mask, casting a shadow on the detector. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/coded_aperture/coded_aperture.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/explorer-11_detector/explorer-11_detector.dc.xml Draushaar and Clark’s detector for Explorer 11 was designed to detect gamma rays above 50 MeV. The image on the left shows the detector. It measured 20 inches high, 10 inches in diameter, and weighed about 30 pounds. The image on the right is a diagram of the detector, which consisted of a sandwich crystal scintillator and a Lucite Cherenkov counter, surrounded by a plastic anticoincidence scintillator. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/explorer-11_detector/explorer-11_detector.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/fig-26-ems-big/fig-26-ems-big.dc.xml Scale illustrating the order and size of the wavelengths in each band of the electromagnetic spectrum. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/fig-26-ems-big/fig-26-ems-big.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/firststars/firststars.dc.xml An artist's concept of the first stars forming after the Big Bang. The first stars should have been supermassive and metal poor stars that would end with a collapsar and a GRB, but there is currently no evidence of these earliest GRBs. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/firststars/firststars.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/gamma-ray_bursts/gamma-ray_bursts.dc.xml This graphic illustrates the different sources and processes that result in long and short gamma-ray bursts. The left panel shows the collapse of a giant star that is thought to lead to a long GRB. The right panel shows the inspiral and coalescence of two neutron stars, which is thought to result in a short GRB. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/gamma-ray_bursts/gamma-ray_bursts.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/giacconi-nobel/giacconi-nobel.dc.xml In 2002, Riccardo Giacconi shared the Nobel Prize in Physics, given to him for pioneering contributions to astrophysics, which have led to the discovery of cosmic X-ray sources. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/giacconi-nobel/giacconi-nobel.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/greatobs_spectrum_300/greatobs_spectrum_300.dc.xml Because the Earth's atmosphere prevents certain types of radiation from reaching the ground, NASA proposed a series of Great Observatories designed to conduct space-based astronomical studies over many different wavelengths. The program launched four observatories: the Hubble Space Telescope (visible and near ultraviolet); Compton Gamma Ray Observatory (gamma rays); Chandra X-ray Observatory (soft X-rays); and Spitzer Space Telescope (infrared). Each observatory was designed to push the state of technology in its intended wavelength region. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/greatobs_spectrum_300/greatobs_spectrum_300.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/heao2_diagram/heao2_diagram.dc.xml Renamed the Einstein Observatory after launch, the image on the left shows HEAO-2 during pre-flight testing. This image shows the placement of the instruments onboard the observatory. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/heao2_diagram/heao2_diagram.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/hubble/hubble.dc.xml Named after astronomer Edwin Hubble, one of the Hubble Space Telescope’s key projects was to determine the rate of expansion of the Universe, called the Hubble Constant. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/hubble/hubble.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/nustar1/nustar1.dc.xml The artist’s conception illustrates the orientation of the detectors and optics on the satellite. The solar panel on the left provides power to the telescope. The yellow module on the far right contains the new technology optics which consists of two mirrors. These mirrors focus the hard X-rays and soft gamma rays onto the detectors at the other end of the deployable mast. The optics and the detectors must be separated by 10 meters (30 feet). The detectors and optics are launched close together because they just fit in the existing rockets used to launch satellites into space; the mast is extended after launch. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/nustar1/nustar1.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/ptolemy_cosmos/ptolemy_cosmos.dc.xml This image depicts the slow evolution of thought about the physics of the solar system in the mid-17th century. The shield on the left represents Copernicus's view of the Universe (1543) with the Sun at the center of the Universe and all of the planets, including the Earth moving around it. Copernicus's model was opposed by the Church which held that the Earth was the center of the Universe. The shield on the right depicts Tycho Brahe's model of the Universe (1588) which reconciles the Copernican model with the early Ptolemaic model (ca. 150) in which the Sun, Moon, planets, and stars all revolve around the Earth. Brahe's model allows that the other planets revolve around the Sun, but maintains that the Earth is the stationary center of the Universe around which the Sun, dragging all of the planets with it, as well as the Moon, revolve. Brahe's shield carries more weight (tilts the balance) in this picture because the Church, a powerful arbiter of scientific thought in the 17th century, supported Brahe's mode... http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/ptolemy_cosmos/ptolemy_cosmos.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/sas3/sas3.dc.xml Designed and built at M.I.T, the SAS-3 was a spinning satellite. The spin rate was controlled by a gyroscope that could be commanded to stop rotation so that all instruments could be pointed at a given source. Pointing could provide about 30 minutes of continuous data on a source, such as a pulsar, burster, or transient. This is an artist’s conception of the satellite in orbit.. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/sas3/sas3.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/sas3_layout/sas3_layout.dc.xml Designed and built at M.I.T, the SAS-3 was a spinning satellite. The spin rate was controlled by a gyroscope that could be commanded to stop rotation so that all instruments could be pointed at a given source. Pointing could provide about 30 minutes of continuous data on a source, such as a pulsar, burster, or transient. This is a diagram of the instruments onboard the SAS-3. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/sas3_layout/sas3_layout.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/twoComponentJetStream_960x540/twoComponentJetStream_960x540.dc.xml Gamma-ray bursts that are longer than two seconds are caused by the detonation of a rapidly rotating massive star at the end of its life on the main sequence. Jets of particles and gamma radiation are emitted in opposite directions from the stellar core as the star collapses. In this model, a narrow beam of gamma rays is emitted, followed by a wider beam of gamma rays. The narrow beam for GRB 080319B was aimed almost precisely at the Earth, which made it the brightest gamma-ray burst observed to date by NASA's Swift satellite. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/twoComponentJetStream_960x540/twoComponentJetStream_960x540.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/uhuruExplode-72bigfromChandrasite/uhuruExplode-72bigfromChandrasite.dc.xml The Uhuru X-ray satellite, equipped with a relatively simple instrument - a sensitive X-ray detector similar to a Geiger counter attached to a viewing pipe to locate the source - made some astounding discoveries. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/uhuruExplode-72bigfromChandrasite/uhuruExplode-72bigfromChandrasite.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/voyager1/voyager1.dc.xml Voyager 1 and 2 were launched 16 days apart in 1977 to study Jupiter and Saturn. In September 2013, NASA reported that Voyager 1 had entered interstellar space, placing it more than 11 billion miles from the Sun and making it the most distant human-made object. As of 2013, Voyager 2 is in the heliosheath, the outermost layer of the immense magnetic bubble, called the heliosphere, that contains our solar system. Both Voyager 1 and 2 are still sending scientific information about their surroundings through the Deep Space Network (DSN). http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/voyager1/voyager1.dc.xml Thu, 01 Jan 1970 12:00:00 GMT