What does the EUV and thin film group do?
... The Earth’s magnetosphere in the EUV Images from www.schott.com/magazine/english/info99/ and www.lbl.gov/Science-Articles/Archive/xray-inside-cells.html. ...
... The Earth’s magnetosphere in the EUV Images from www.schott.com/magazine/english/info99/ and www.lbl.gov/Science-Articles/Archive/xray-inside-cells.html. ...
Far Ultraviolet Spectroscopic Explorer
... Search data set for interesting individual objects that represent rare classes of objects. ...
... Search data set for interesting individual objects that represent rare classes of objects. ...
"Characterization of 3D-integrated Active Pixel Sensor for X-ray Detection."
... The crosstalk signal is very different in the left and right pixels. On the left side, the level of crosstalk is very small (only 0.85%), while on the right, it is 8.8%. We verified this result by reversing the addressing sequence and reading columns in the opposite direction. This did not affect th ...
... The crosstalk signal is very different in the left and right pixels. On the left side, the level of crosstalk is very small (only 0.85%), while on the right, it is 8.8%. We verified this result by reversing the addressing sequence and reading columns in the opposite direction. This did not affect th ...
Neutron Stars PowerPoint
... ~ 1,837 times the mass of an electron Proton mass + Electron mass = Neutron mass ...
... ~ 1,837 times the mass of an electron Proton mass + Electron mass = Neutron mass ...
PHYS3380_111615_bw - The University of Texas at Dallas
... Initial rotation period uncertain, but lets say similar to typical white dwarfs (e.g. 40Eri B has PWD=1350s). Hence PNS ~ 4 ms Magnetic field strengths in white dwarfs typically measured at B=5x108 Gauss, hence BNS~1014 Gauss (compare with B ~2 Gauss!) Similar luminosity to Sun, but mostly in X-ray ...
... Initial rotation period uncertain, but lets say similar to typical white dwarfs (e.g. 40Eri B has PWD=1350s). Hence PNS ~ 4 ms Magnetic field strengths in white dwarfs typically measured at B=5x108 Gauss, hence BNS~1014 Gauss (compare with B ~2 Gauss!) Similar luminosity to Sun, but mostly in X-ray ...
Neutron Stars PowerPoint
... ~ 1,837 times the mass of an electron Proton mass + Electron mass = Neutron mass ...
... ~ 1,837 times the mass of an electron Proton mass + Electron mass = Neutron mass ...
The ultracompact nature of the black hole candidate X
... be a white dwarf. We report simultaneous observations of X9 performed by Chandra, NuSTAR and Australia Telescope Compact Array. We find a clear 28.18±0.02-min periodic modulation in the Chandra data, which we identify as the orbital period, confirming this system as an ultracompact X-ray binary. Our ...
... be a white dwarf. We report simultaneous observations of X9 performed by Chandra, NuSTAR and Australia Telescope Compact Array. We find a clear 28.18±0.02-min periodic modulation in the Chandra data, which we identify as the orbital period, confirming this system as an ultracompact X-ray binary. Our ...
Associated Spectral and Temporal State Transition of the
... Stellar mass black hole X-ray binaries exhibit X-ray spectral states which also have distinct and characteristic temporal properties. These states are believed to correspond to different accretion disc geometries. We present analysis of two XMM-Newton observations of the Ultra-Luminous X-ray source ...
... Stellar mass black hole X-ray binaries exhibit X-ray spectral states which also have distinct and characteristic temporal properties. These states are believed to correspond to different accretion disc geometries. We present analysis of two XMM-Newton observations of the Ultra-Luminous X-ray source ...
arXiv:1502.04693v1 [gr
... WISE candidates has only been capable with the Wide Field Camera 3 (WFC3) aboard the Hubble Space Telescope (HST). HST grism spectroscopy of the latest type brown dwarfs has been invaluable in the study and classification of these objects (Cushing et al. 2011, Kirkpatrick et al. 2012, Kirkpatrick et ...
... WISE candidates has only been capable with the Wide Field Camera 3 (WFC3) aboard the Hubble Space Telescope (HST). HST grism spectroscopy of the latest type brown dwarfs has been invaluable in the study and classification of these objects (Cushing et al. 2011, Kirkpatrick et al. 2012, Kirkpatrick et ...
A CHANDRA X-RAY STUDY OF THE DENSE GLOBULAR CLUSTER TERZAN... C. O. Heinke, P. D. Edmonds, J. E. Grindlay, and...
... Their X-ray colors, luminosities, and spectral fitting indicate that five of them are probably cataclysmic variables and four are likely quiescent LMXBs containing neutron stars. We estimate the total number of sources between LX ð0:5 2:5 keVÞ ¼ 1032 and 1033 ergs s1 as 11:4þ4:7 1:8 by the use of ar ...
... Their X-ray colors, luminosities, and spectral fitting indicate that five of them are probably cataclysmic variables and four are likely quiescent LMXBs containing neutron stars. We estimate the total number of sources between LX ð0:5 2:5 keVÞ ¼ 1032 and 1033 ergs s1 as 11:4þ4:7 1:8 by the use of ar ...
Which Stars Form Black Holes and Neutron Stars?
... of these has their own strengths and complications. In principle, if one has identified a supernova associated with a known compact object, it should be possible to infer the mass of the star that exploded from the masses and abundances of metals in the remnant. The Crab nebula is best modeled as de ...
... of these has their own strengths and complications. In principle, if one has identified a supernova associated with a known compact object, it should be possible to infer the mass of the star that exploded from the masses and abundances of metals in the remnant. The Crab nebula is best modeled as de ...
X-ray and Gamma-ray Studies of the Millisecond Pulsar and
... We present X-ray observations of the “redback” eclipsing radio millisecond pulsar (MSP) and candidate radio pulsar/X-ray binary transition object PSR J1723–2837. The X-ray emission from the system is predominantly non-thermal and exhibits pronounced variability as a function of orbital phase, with a ...
... We present X-ray observations of the “redback” eclipsing radio millisecond pulsar (MSP) and candidate radio pulsar/X-ray binary transition object PSR J1723–2837. The X-ray emission from the system is predominantly non-thermal and exhibits pronounced variability as a function of orbital phase, with a ...
IGR J18483-0311: a new intermediate supergiant fast X
... X-ray transients (SFXTs, Negueruela et al. 2006). IGR J18483−0311 was discovered during observations performed with INTEGRAL in 2003 April 23-28 (Chernyakova et al. 2003), and it was found to have average fluxes of about 10 mCrab and 5 mCrab in the 15−40 keV and 40−100 keV bands, respectively. Molko ...
... X-ray transients (SFXTs, Negueruela et al. 2006). IGR J18483−0311 was discovered during observations performed with INTEGRAL in 2003 April 23-28 (Chernyakova et al. 2003), and it was found to have average fluxes of about 10 mCrab and 5 mCrab in the 15−40 keV and 40−100 keV bands, respectively. Molko ...
Cool Stars in the Galaxy — A ROSAT and ASCA View.
... soft X-ray image of the solar corona obtained using the Japanese Yohkoh satellite. The bright regions are active (emit in the X-ray band) whilst the dark regions are much less so. The large dark polar regions are coronal holes, regions which when compared to their surroundings have lower tem peratur ...
... soft X-ray image of the solar corona obtained using the Japanese Yohkoh satellite. The bright regions are active (emit in the X-ray band) whilst the dark regions are much less so. The large dark polar regions are coronal holes, regions which when compared to their surroundings have lower tem peratur ...
Lecture 2: ppt, 5 MB
... If Colorado were as smooth as Chandra's mirrors, Pikes Peak would be less than one inch tall! Chandra's resolving power is equivalent to the ability to read a stop sign at a distance of twelve miles. The electrical power required to operate the Chandra spacecraft and instruments is 2 kilowatts ...
... If Colorado were as smooth as Chandra's mirrors, Pikes Peak would be less than one inch tall! Chandra's resolving power is equivalent to the ability to read a stop sign at a distance of twelve miles. The electrical power required to operate the Chandra spacecraft and instruments is 2 kilowatts ...
Astronomy Astrophysics Astrophysical parameters and orbital solution of the peculiar X-ray
... Of course, a clumpy spherical wind can exist together with an eccentric orbit (Blay et al. 2012), and this scenario would also explain the quasi-stable X-ray luminosity of SGXBs, since they have circular orbits. Furthermore, Bozzo et al. (2008) proposed a model that makes use of transitions between ...
... Of course, a clumpy spherical wind can exist together with an eccentric orbit (Blay et al. 2012), and this scenario would also explain the quasi-stable X-ray luminosity of SGXBs, since they have circular orbits. Furthermore, Bozzo et al. (2008) proposed a model that makes use of transitions between ...
Measuring the orbital periods of low mass X-ray binaries in the X
... However, there are still some difficulties with measuring the orbital periods in the optical band. First, some X-ray binaries have no identified optical counterparts. The Galactic HMXBs are mostly distributed around the Galactic plane where the extinction in the optical band is high. For LMXBs, some ...
... However, there are still some difficulties with measuring the orbital periods in the optical band. First, some X-ray binaries have no identified optical counterparts. The Galactic HMXBs are mostly distributed around the Galactic plane where the extinction in the optical band is high. For LMXBs, some ...
The star-forming environment of an ultraluminous X-ray
... a small group of OB stars, but is not associated with any massive young clusters nor with any extraordinary massive stars. The brightest point source in the Chandra error circle is consistent with a single blue supergiant (BSG) of mass ≈20 M and age ≈10 Myr. A few other stars are resolved inside th ...
... a small group of OB stars, but is not associated with any massive young clusters nor with any extraordinary massive stars. The brightest point source in the Chandra error circle is consistent with a single blue supergiant (BSG) of mass ≈20 M and age ≈10 Myr. A few other stars are resolved inside th ...
Neutron Stars
... Periods shorter than this do not exist (such as in the previous calculation) because the object would have to rotate so fast it would overcome gravity and fly apart. ...
... Periods shorter than this do not exist (such as in the previous calculation) because the object would have to rotate so fast it would overcome gravity and fly apart. ...
Accretion Processes of Binaries of White Dwarfs
... Binarity of the central star system? • Severe mass loss rate through slow stellar wind from the giant. • Fast stellar wind from the white dwarf component • Collision of slow stellar wind and fast wind ...
... Binarity of the central star system? • Severe mass loss rate through slow stellar wind from the giant. • Fast stellar wind from the white dwarf component • Collision of slow stellar wind and fast wind ...
Educator`s Guide - Ott Planetarium
... energy ultraviolet radiation. The atmosphere also blocks much of the infrared spectrum. That’s great for living things, but it also means there’s a lot to “see” beyond what our atmosphere allows. If we want to observe in these wavelengths, we need to position our instruments above the atmosphere. Th ...
... energy ultraviolet radiation. The atmosphere also blocks much of the infrared spectrum. That’s great for living things, but it also means there’s a lot to “see” beyond what our atmosphere allows. If we want to observe in these wavelengths, we need to position our instruments above the atmosphere. Th ...
copyright 2002 scientific american, inc.
... because it occurred on May 8, 1997. Radio observations of its afterglow provided an essential clue. The glow varied erratically by roughly a factor of two during the first three weeks, after which it stabilized and then began to diminish. The large variations probably had nothing to do with the burs ...
... because it occurred on May 8, 1997. Radio observations of its afterglow provided an essential clue. The glow varied erratically by roughly a factor of two during the first three weeks, after which it stabilized and then began to diminish. The large variations probably had nothing to do with the burs ...
X-ray sources in the starburst spiral galaxy M 83
... and a power-law spectrum with photon index Γ = 1.5 for all the sources, the detection threshold of '15 net counts places an upper limit of fx ' 2.0 × 10−15 erg cm−2 s−1 for the observed flux in the 0.3–8.0 keV band. Those three transients were therefore at least an order of magnitude fainter than th ...
... and a power-law spectrum with photon index Γ = 1.5 for all the sources, the detection threshold of '15 net counts places an upper limit of fx ' 2.0 × 10−15 erg cm−2 s−1 for the observed flux in the 0.3–8.0 keV band. Those three transients were therefore at least an order of magnitude fainter than th ...
Extreme Physics Explorer - High Energy Astrophysics
... Black Holes, Magnetars & Neutron Stars are cosmic laboratories for Extreme Physics: • Gravity at the event horizon -- Black Holes Frame dragging, metric in strong gravity -- AGNs, BH binaries ...
... Black Holes, Magnetars & Neutron Stars are cosmic laboratories for Extreme Physics: • Gravity at the event horizon -- Black Holes Frame dragging, metric in strong gravity -- AGNs, BH binaries ...
Mass Estimate of Black Hole Candidates GRS 1758
... Santa Cruz Institute for Particle Physics Seminar May 23, 2006 ...
... Santa Cruz Institute for Particle Physics Seminar May 23, 2006 ...
X-ray astronomy
X-ray astronomy is an observational branch of astronomy which deals with the study of X-ray observation and detection from astronomical objects. X-radiation is absorbed by the Earth's atmosphere, so instruments to detect X-rays must be taken to high altitude by balloons, sounding rockets, and satellites. X-ray astronomy is the space science related to a type of space telescope that can see farther than standard light-absorption telescopes, such as the Mauna Kea Observatories, via x-ray radiation.X-ray emission is expected from astronomical objects that contain extremely hot gasses at temperatures from about a million kelvin (K) to hundreds of millions of kelvin (MK). Although X-rays have been observed emanating from the Sun since the 1940s, the discovery in 1962 of the first cosmic X-ray source was a surprise. This source is called Scorpius X-1 (Sco X-1), the first X-ray source found in the constellation Scorpius. The X-ray emission of Scorpius X-1 is 10,000 times greater than its visual emission, whereas that of the Sun is about a million times less. In addition, the energy output in X-rays is 100,000 times greater than the total emission of the Sun in all wavelengths. Based on discoveries in this new field of X-ray astronomy, starting with Scorpius X-1, Riccardo Giacconi received the Nobel Prize in Physics in 2002. It is now known that such X-ray sources as Sco X-1 are compact stars, such as neutron stars or black holes. Material falling into a black hole may emit X-rays, but the black hole itself does not. The energy source for the X-ray emission is gravity. Infalling gas and dust is heated by the strong gravitational fields of these and other celestial objects.Many thousands of X-ray sources are known. In addition, the space between galaxies in galaxy clusters is filled with a very hot, but very dilute gas at a temperature between 10 and 100 megakelvins (MK). The total amount of hot gas is five to ten times the total mass in the visible galaxies.