Gamma-Ray Astroparticle Physics
... Also the colors we don’t see have names familiar to us: we listen to the radio, we heat food in the microwave, we take pictures of our bones through X-rays… ...
... Also the colors we don’t see have names familiar to us: we listen to the radio, we heat food in the microwave, we take pictures of our bones through X-rays… ...
lesson 5_test
... 1. What is Swift? What is it composed of? 2. Explain the role of each part of the telescope. 1:05 to 3:25 3. What are Gamma Ray Bursts? 4. How were they discovered? 5. What was the aim of the nuclear test ban treaty? When was it signed? 3:25 to the end 6. What are the two theories used to explain GR ...
... 1. What is Swift? What is it composed of? 2. Explain the role of each part of the telescope. 1:05 to 3:25 3. What are Gamma Ray Bursts? 4. How were they discovered? 5. What was the aim of the nuclear test ban treaty? When was it signed? 3:25 to the end 6. What are the two theories used to explain GR ...
File
... 22) What is a galaxy? 23) What are the three classifications of galaxies? What do each look like? Which is most common? 24) What shape is the Milky Way? 25) What is the local group? 26) How many stars are in the Milky Way? 27) Approximately how big is the Milky Way 28) The largest known galaxy is wh ...
... 22) What is a galaxy? 23) What are the three classifications of galaxies? What do each look like? Which is most common? 24) What shape is the Milky Way? 25) What is the local group? 26) How many stars are in the Milky Way? 27) Approximately how big is the Milky Way 28) The largest known galaxy is wh ...
Signals from the Beginnings of the World - Max-Planck
... The GROND detector developed by Jochen Greiner radically improves this situation: “The instrument combines the detection of the afterglow with a rough determination of the distance. We can now determine the distance of a gamma-ray burst within minutes, or within one to two hours at worst, to within ...
... The GROND detector developed by Jochen Greiner radically improves this situation: “The instrument combines the detection of the afterglow with a rough determination of the distance. We can now determine the distance of a gamma-ray burst within minutes, or within one to two hours at worst, to within ...
Earth - Capital High School
... – core collapses and then rebounds outward with a shock wave that makes a bright explosion (supernova) – at this point, heavier elements are created ...
... – core collapses and then rebounds outward with a shock wave that makes a bright explosion (supernova) – at this point, heavier elements are created ...
GRB prompt emission
... • GRBs are Isotropic – The beginning of the end for Galactic Models, but persistent theorists move the Galactic Models to the Halo • GRBs come in all shapes and sizes but two obvious subgroups exist I) Short, Hard Bursts II) Long, Soft Bursts ...
... • GRBs are Isotropic – The beginning of the end for Galactic Models, but persistent theorists move the Galactic Models to the Halo • GRBs come in all shapes and sizes but two obvious subgroups exist I) Short, Hard Bursts II) Long, Soft Bursts ...
GRB prompt emission
... • GRBs are Isotropic – The beginning of the end for Galactic Models, but persistent theorists move the Galactic Models to the Halo • GRBs come in all shapes and sizes but two obvious subgroups exist I) Short, Hard Bursts II) Long, Soft Bursts ...
... • GRBs are Isotropic – The beginning of the end for Galactic Models, but persistent theorists move the Galactic Models to the Halo • GRBs come in all shapes and sizes but two obvious subgroups exist I) Short, Hard Bursts II) Long, Soft Bursts ...
Small images
... Starting in May 2005, about a half dozen short hard bursts were localized by the HETE-2 and SWIFT satellites. These bursts did not come from star forming regions, and in fact showed all the characteristics expected of merging neutron stars. It is widely believed that merging neutron stars (and neutr ...
... Starting in May 2005, about a half dozen short hard bursts were localized by the HETE-2 and SWIFT satellites. These bursts did not come from star forming regions, and in fact showed all the characteristics expected of merging neutron stars. It is widely believed that merging neutron stars (and neutr ...
Visit to Monroe County High Schools
... A Source of Gamma Rays: The Crab Nebula Supernova seen in 1054 AD Still shining: light particles with 1 trillion times more energy than sunlight photons ...
... A Source of Gamma Rays: The Crab Nebula Supernova seen in 1054 AD Still shining: light particles with 1 trillion times more energy than sunlight photons ...
Life and Evolution of a Massive Star
... • First discovered in the 60s by US spy satellites looking for nuclear bomb tests • Astronomers first thought GRBs were just more energetic versions of X-ray binaries – X-ray binaries are concentrated in the disk of the Milky Way – GRBs are not, so they must be extragalactic ...
... • First discovered in the 60s by US spy satellites looking for nuclear bomb tests • Astronomers first thought GRBs were just more energetic versions of X-ray binaries – X-ray binaries are concentrated in the disk of the Milky Way – GRBs are not, so they must be extragalactic ...
the summary
... of starlight is in general not much different from that of a glowing wire in a light bulb or a white hot piece of iron: a thermal spectrum. The outermost layer of the star, the atmosphere, contains atoms and ions that absorb part of the light at very specific wavelengths, creating atmospheric absorp ...
... of starlight is in general not much different from that of a glowing wire in a light bulb or a white hot piece of iron: a thermal spectrum. The outermost layer of the star, the atmosphere, contains atoms and ions that absorb part of the light at very specific wavelengths, creating atmospheric absorp ...
High-Energy Astrophysics - University of Iowa Astrophysics
... Gamma-rays • Formal definition of X-ray versus gamma-ray is that X-rays come from electronic transitions while gamma-rays come from nuclear transitions. • In practice, gamma-rays in the X-ray band are usually referred to as X-rays • Gamma-rays typically have energies above about 100 keV ...
... Gamma-rays • Formal definition of X-ray versus gamma-ray is that X-rays come from electronic transitions while gamma-rays come from nuclear transitions. • In practice, gamma-rays in the X-ray band are usually referred to as X-rays • Gamma-rays typically have energies above about 100 keV ...
Gamma Ray Bursts (GRB)
... Long duration bursts – Gamma Ray Bursts that last more than 2 seconds. Short-duration bursts – Gamma Ray Bursts that last less than 2 seconds. Short duration bursts range from a few milliseconds to 2 seconds with an average duration time of about 0.3 seconds (300 milliseconds). The longduration burs ...
... Long duration bursts – Gamma Ray Bursts that last more than 2 seconds. Short-duration bursts – Gamma Ray Bursts that last less than 2 seconds. Short duration bursts range from a few milliseconds to 2 seconds with an average duration time of about 0.3 seconds (300 milliseconds). The longduration burs ...
Introduction - University of Iowa Astrophysics
... • Photons are emitted at the characteristic energy of particles in a system. • For a blackbody, we have Wien’s Law: – Wavelength of peak (Ang) = 2.9 x 107 / T(K) • In general, a system tends to produce radiation up to around the maximum energy of its particles • Thus, high energy photons are probes ...
... • Photons are emitted at the characteristic energy of particles in a system. • For a blackbody, we have Wien’s Law: – Wavelength of peak (Ang) = 2.9 x 107 / T(K) • In general, a system tends to produce radiation up to around the maximum energy of its particles • Thus, high energy photons are probes ...
The Swift satellite lives up to its name, revealing cosmic
... subarcsecond position of the optical afterglow led to successful identification of the host galaxy, lying at a distance z=0.16. Thereafter several more afterglow detections were made at both X-ray and optical wavelengths. The sample shows that while short GRB afterglows are generally less distant, t ...
... subarcsecond position of the optical afterglow led to successful identification of the host galaxy, lying at a distance z=0.16. Thereafter several more afterglow detections were made at both X-ray and optical wavelengths. The sample shows that while short GRB afterglows are generally less distant, t ...
Cosmological Transient Objects
... • At the time of explosion, the supernova can shine brighter than the host galaxy consisting of billions of stars. • In one month, a supernova can emit as much energy as Sun would emit in its entire life span of billions of years. • GRBs: biggest source of gamma-rays in universe and 100 times more e ...
... • At the time of explosion, the supernova can shine brighter than the host galaxy consisting of billions of stars. • In one month, a supernova can emit as much energy as Sun would emit in its entire life span of billions of years. • GRBs: biggest source of gamma-rays in universe and 100 times more e ...
XLII RENCONTRES DE MORIOND WORKSHOP ON …
... • An “anti-Malmquist” bias is observed: that is GRBs at high-z are easier to see than expected • To reconcile this trend, simulations suggest that GRBs at high-z must be relatively brighter than those at small-z ...
... • An “anti-Malmquist” bias is observed: that is GRBs at high-z are easier to see than expected • To reconcile this trend, simulations suggest that GRBs at high-z must be relatively brighter than those at small-z ...
Gamma Ray Burst Afterglows and Host Galaxies
... • The central engine emits a large amount of energy (in almost any form). • Most of that energy accelerates a small mass (about the mass of the Earth) to speeds > 99.99% of lightspeed. • Collisions between different shells of ejected debris creates the gamma rays. • Collisions between ejected debris ...
... • The central engine emits a large amount of energy (in almost any form). • Most of that energy accelerates a small mass (about the mass of the Earth) to speeds > 99.99% of lightspeed. • Collisions between different shells of ejected debris creates the gamma rays. • Collisions between ejected debris ...
USRA - MSU Solar Physics
... extragalactic distances was largely based on the randomness of the distribution, but at that time, there was no way to test this theory because once the burst was gone, all that was left was a lightcurve which tells nothing of its origin or distance. The introduction of the Italian BeppoSAX mission ...
... extragalactic distances was largely based on the randomness of the distribution, but at that time, there was no way to test this theory because once the burst was gone, all that was left was a lightcurve which tells nothing of its origin or distance. The introduction of the Italian BeppoSAX mission ...
Circumstellar interaction of supernovae and gamma-ray bursts
... Blast wave shock : Ejecta expansion speed is much higher than sound speed. Shocked CSM: Interaction of blast wave with CSM . CSM is accelerated, compressed, heated and shocked. ...
... Blast wave shock : Ejecta expansion speed is much higher than sound speed. Shocked CSM: Interaction of blast wave with CSM . CSM is accelerated, compressed, heated and shocked. ...
Gamma-ray burst
Gamma-ray bursts (GRBs) are flashes of gamma rays associated with extremely energetic explosions that have been observed in distant galaxies. They are the brightest electromagnetic events known to occur in the universe. Bursts can last from ten milliseconds to several hours. The initial burst is usually followed by a longer-lived ""afterglow"" emitted at longer wavelengths (X-ray, ultraviolet, optical, infrared, microwave and radio).Most observed GRBs are believed to consist of a narrow beam of intense radiation released during a supernova or hypernova as a rapidly rotating, high-mass star collapses to form a neutron star, quark star, or black hole. A subclass of GRBs (the ""short"" bursts) appear to originate from a different process – this may be due to the merger of binary neutron stars. The cause of the precursor burst observed in some of these short events may be due to the development of a resonance between the crust and core of such stars as a result of the massive tidal forces experienced in the seconds leading up to their collision, causing the entire crust of the star to shatter.The sources of most GRBs are billions of light years away from Earth, implying that the explosions are both extremely energetic (a typical burst releases as much energy in a few seconds as the Sun will in its entire 10-billion-year lifetime) and extremely rare (a few per galaxy per million years). All observed GRBs have originated from outside the Milky Way galaxy, although a related class of phenomena, soft gamma repeater flares, are associated with magnetars within the Milky Way. It has been hypothesized that a gamma-ray burst in the Milky Way, pointing directly towards the Earth, could cause a mass extinction event.GRBs were first detected in 1967 by the Vela satellites, a series of satellites designed to detect covert nuclear weapons tests. Hundreds of theoretical models were proposed to explain these bursts in the years following their discovery, such as collisions between comets and neutron stars. Little information was available to verify these models until the 1997 detection of the first X-ray and optical afterglows and direct measurement of their redshifts using optical spectroscopy, and thus their distances and energy outputs. These discoveries, and subsequent studies of the galaxies and supernovae associated with the bursts, clarified the distance and luminosity of GRBs. These facts definitively placed them in distant galaxies and also connected long GRBs with the explosion of massive stars, the only possible source for the energy outputs observed.