http://www.rssboard.org/rss-specification 720 http://ecuip-xtf.lib.uchicago.edu/xtf/search?docsPerPage%3D100;f4-associated-Lesson%3DGamma%20Ray%20Science Results for your query: docsPerPage=100;f4-associated-Lesson=Gamma Ray Science 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/534058main_NS_six_panel_17/534058main_NS_six_panel_17.dc.xml Short gamma-ray bursts are difficult to study because they are so short. Less than 2 seconds is not a lot of time to find the burst and capture some data. These images show the merger of two neutron stars recently simulated using a new supercomputer model. Redder colors indicate lower densities. Green and white ribbons and lines represent magnetic fields. The orbiting neutron stars rapidly lose energy by emitting gravitational waves and merge after about three orbits, or in less than 8 milliseconds. The merger amplifies and scrambles the merged magnetic field. A black hole forms and the magnetic field becomes more organized, eventually producing structures capable of supporting the jets that power short gamma-ray bursts. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/534058main_NS_six_panel_17/534058main_NS_six_panel_17.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/6870605/6870605.dc.xml On May 25, 1961, President John F. Kennedy announced the ambitious goal of sending an American safely to the Moon before the end of the decade. This challenge guided the work of NASA and accelerated technology development through 17 Apollo Missions that took place between the years of 1967 and 1972. The President’s goal was achieved on July 20, 1969, when Apollo 11 commander Neil Armstrong stepped off the Lunar Module's ladder and onto the Moon's surface. This image shows the launch of Apollo 7 in 1968, the first Apollo mission to carry a crew into space. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/6870605/6870605.dc.xml Tue, 01 Oct 1968 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/CassA_NuStar/CassA_NuStar.dc.xml This new view of the historical supernova remnant Cassiopeia A was taken by NASA's Nuclear Spectroscopic Telescope Array, or NuSTAR. Blue indicates where NuSTAR has made the first resolved image ever of this source at the highest energy X-ray light, between 10 and 20 kiloelectron volts. Red and green show the lower end of NuSTAR's energy range, which overlaps with NASA's high-resolution Chandra X-ray Observatory. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/CassA_NuStar/CassA_NuStar.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/DHJRPPeru2011/DHJRPPeru2011.dc.xml Dieter Hartmann with his wife in Peru on one of their many travels. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/DHJRPPeru2011/DHJRPPeru2011.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/DieterHartmann1060/DieterHartmann1060.dc.xml Dieter Hartmann stands next to his mother on his first day of school holding an Easter cone full of candy. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/DieterHartmann1060/DieterHartmann1060.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/GLAST_GRB_multiwavelength/GLAST_GRB_multiwavelength.dc.xml The typical spectrum of a gamma burst delineates the spectral range of two instruments on the Fermi Space Telescope: the Gamma-ray Burst Monitor (GBM) and Large Area Telecope (LAT). http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/GLAST_GRB_multiwavelength/GLAST_GRB_multiwavelength.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/New_Array/New_Array.dc.xml VERITAS (Very Energetic Radiation Imaging Telescope Array System) is a system of four ground-based telescopes focused on gamma-ray science. Since gamma-rays cannot penetrate the atmosphere, the telescopes are detecting the particles created when gamma-ray photons collide with the atmosphere. Optical telescopes can then image the display the secondary particles make when passing through the atmosphere. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/New_Array/New_Array.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/ernestrutherford/ernestrutherford.dc.xml Ernest Rutherford sitting in his lab (right) with his assistant, Hans Geiger. Circa 1913. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/ernestrutherford/ernestrutherford.dc.xml Mon, 27 Mar 1905 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/grayEarth_petry/grayEarth_petry.dc.xml The pixelated planet above is actually our own planet Earth seen in gamma rays--the most energetic form of light. In fact, the gamma rays used to construct this view pack over 35 million electron volts (MeV) compared to a mere two electron volts (eV) for a typical visible light photon. The Earth's gamma-ray glow is indeed very faint, and this image was constructed by combining data from seven years of exposure during the life of the Compton Gamma Ray Observatory, operating in Earth orbit from 1991 to 2000. Brightest near the edge and faint near the center, the picture indicates that the gamma rays are coming from high in Earth's atmosphere. The gamma rays are produced as the atmosphere interacts with high energy cosmic rays from space, blocking the harmful radiation from reaching the surface. Astronomers need to understand Earth's gamma-ray glow well as it can interfere with observations of cosmic gamma-ray sources like pulsars, supernova remnants, and distant active galaxies powered by supermassive black hol... http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/grayEarth_petry/grayEarth_petry.dc.xml Thu, 01 Jan 1970 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/grb050709/grb050709.dc.xml Gamma-ray bursts longer than two seconds are the most common type and are widely thought to be triggered by the collapse of a massive star into a black hole. As matter falls toward the black hole, some of it forms jets in the opposite direction that move near the speed of light. These jets bore through the collapsing star along its rotational axis and produce a blast of gamma rays after they emerge. This artist's rendering depicts a GRB that was discovered on July 9, 2005, by NASA's High-Energy Transient Explorer (HETE). http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/grb050709/grb050709.dc.xml Sat, 09 Jul 2005 12:00:00 GMT http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/mwmw_8x10/mwmw_8x10.dc.xml Imagine that you are looking up at the night sky and can see the arms of the Milky Way Galaxy bisecting the sky. The image of the sky labelled optical in this graphic is what you would see with your eyes. Now, observe the images of the same view of the Milky Way, but in through the lens of a telescope that sees in a different wavelength than our eyes. The amount and type of information, or data, available in each waveband varies as illustrated in this graphic. You can see why it is so important that we look at the universe through eyes that see wavebands other than optical light. http://ecuip-xtf.lib.uchicago.edu/xtf/view?docId=grxr/mwmw_8x10/mwmw_8x10.dc.xml Thu, 01 Jan 1970 12:00:00 GMT