What does X-ray light show us?
... in space. Things like supernova explosions (the way massive stars die), neutron stars and pulsars, and black holes are all sources of celestial gamma-rays. ...
... in space. Things like supernova explosions (the way massive stars die), neutron stars and pulsars, and black holes are all sources of celestial gamma-rays. ...
SSM hardware
... – Knowledge better than 1´ (at the end of boom, inclusive of tilt/resolver errors). – Proposed accuracy of position sensing ~ 5-10´ depending on intensity of the transient – Automation of ground software for preprocessing of the ...
... – Knowledge better than 1´ (at the end of boom, inclusive of tilt/resolver errors). – Proposed accuracy of position sensing ~ 5-10´ depending on intensity of the transient – Automation of ground software for preprocessing of the ...
ppt 2.6 - NRAO: Socorro, New Mexico
... (Lucy & Solomon 1970; Feldmeier 1998). Shocks can form and produce observable emission – X-rays: soft, non-variable – NT radio? ...
... (Lucy & Solomon 1970; Feldmeier 1998). Shocks can form and produce observable emission – X-rays: soft, non-variable – NT radio? ...
No Slide Title - Harvard-Smithsonian Center for Astrophysics
... T Tauri stars: complex geometry & activity • T Tauri stars show signatures of disk accretion, “magnetospheric accretion streams,” an X-ray corona, and polar (?) outflows from some combination of star & disk. ...
... T Tauri stars: complex geometry & activity • T Tauri stars show signatures of disk accretion, “magnetospheric accretion streams,” an X-ray corona, and polar (?) outflows from some combination of star & disk. ...
AMUSE-Virgo on the survival of super-massive black holes
... is the chance probability of having a LMXB Lx within the ACIS PSF, based on X-ray luminosity function of LMXBs: in the FIELD (Gilfanov 2004) in the absence of nuclear star clusters in GLOBULAR CLUSTERS (Sivakoff et al. 2007) in the presence of a nuclear cluster ...
... is the chance probability of having a LMXB Lx within the ACIS PSF, based on X-ray luminosity function of LMXBs: in the FIELD (Gilfanov 2004) in the absence of nuclear star clusters in GLOBULAR CLUSTERS (Sivakoff et al. 2007) in the presence of a nuclear cluster ...
THE DAWN OF X-RAY ASTRONOMY
... in 1972 that black holes would have masses greater than 3.4 times the mass of the Sun (Rhoades and Ruffini, 1974).27 Thus we could reach conclusions regarding Cyg X–1: the Cyg X–1 x–ray emitter is a compact object of less than 30 km radius due to the rapidity of the pulsations and the fact that the ...
... in 1972 that black holes would have masses greater than 3.4 times the mass of the Sun (Rhoades and Ruffini, 1974).27 Thus we could reach conclusions regarding Cyg X–1: the Cyg X–1 x–ray emitter is a compact object of less than 30 km radius due to the rapidity of the pulsations and the fact that the ...
AmiraPoster3
... • Long quasi stable period of 50-60 days - believed to be result of quasi periodic obscuration of the neutron star by a precessing accretion disk. • Mode of mass transfer believed to have significant contributions from Roche-lobe overflow, as the stellar winds observed in Sk 160 are not strong enoug ...
... • Long quasi stable period of 50-60 days - believed to be result of quasi periodic obscuration of the neutron star by a precessing accretion disk. • Mode of mass transfer believed to have significant contributions from Roche-lobe overflow, as the stellar winds observed in Sk 160 are not strong enoug ...
7 November 2012 X-ray Astrophysics
... thermal emission given off by the expanding clouds of incredibly hot debris from the exploded star. These clouds are then surrounded by a shell of much harder (higher energy) emission shown in blue, generated where electrons are accelerated behind the rapidly outward-moving shockwave from the supern ...
... thermal emission given off by the expanding clouds of incredibly hot debris from the exploded star. These clouds are then surrounded by a shell of much harder (higher energy) emission shown in blue, generated where electrons are accelerated behind the rapidly outward-moving shockwave from the supern ...
Source Variability - Center for Astrophysics and Space
... On the left is the probability distribution function for two sources in the same field of view. The central source has an energy half that of the source that is displaced to the lower left. The image on the right shows 9000 total events for this system with the lower energy source having twice the ...
... On the left is the probability distribution function for two sources in the same field of view. The central source has an energy half that of the source that is displaced to the lower left. The image on the right shows 9000 total events for this system with the lower energy source having twice the ...
Pallavicini - IASF Milano
... GO programmes, are starting to cover the full age-metallicity plane of nearby open clusters. They allow addressing the question whether a cluster of a given age is representative of all clusters with the same age. ...
... GO programmes, are starting to cover the full age-metallicity plane of nearby open clusters. They allow addressing the question whether a cluster of a given age is representative of all clusters with the same age. ...
Optical studies of an ultraluminous X-ray source: NGC1313 X-2 Jifeng Liu
... • emission lines from X-ray illuminated accretion disks are broad, >1200 km/s • radial velocity for a stellar mass black hole lower than 300 km/s • He II line from X-ray photoionized nebula/secondary • line shift severely affected by noise • need further observations • with higher signal-to-noise ra ...
... • emission lines from X-ray illuminated accretion disks are broad, >1200 km/s • radial velocity for a stellar mass black hole lower than 300 km/s • He II line from X-ray photoionized nebula/secondary • line shift severely affected by noise • need further observations • with higher signal-to-noise ra ...
X-ray Emission from Massive Stars
... The wind profile model provides statistically good fits to all the lines. The onset radii (left) are exactly what’s expected from the standard wind-shock picture. There is evidence for attenuation by the cold wind (right), but at levels nearly 10 times lower than expected. This is the same result th ...
... The wind profile model provides statistically good fits to all the lines. The onset radii (left) are exactly what’s expected from the standard wind-shock picture. There is evidence for attenuation by the cold wind (right), but at levels nearly 10 times lower than expected. This is the same result th ...
dtu7ech13 - Fort Thomas Independent Schools
... Will the Sun someday cease to exist? If so, how? The Sun will shed matter as a planetary nebula in about 6 billion years and then cease nuclear fusion. Its remnant white dwarf will dim over the succeeding billions of years. What is a nova? A nova is a relatively gentle explosion of hydrogen gas on t ...
... Will the Sun someday cease to exist? If so, how? The Sun will shed matter as a planetary nebula in about 6 billion years and then cease nuclear fusion. Its remnant white dwarf will dim over the succeeding billions of years. What is a nova? A nova is a relatively gentle explosion of hydrogen gas on t ...
ppt - SLAC
... • If the kinetic energy is carried by particles, the radiation environment of the AGN should be bulk-Compton-upscattered to X-ray energies by the cold electrons associated with the bulk motion of the jet • If Gjet = 10, the ~10 eV H Lya photons should appear bulk-upscattered to 102 x 10 eV ~ E > 1 k ...
... • If the kinetic energy is carried by particles, the radiation environment of the AGN should be bulk-Compton-upscattered to X-ray energies by the cold electrons associated with the bulk motion of the jet • If Gjet = 10, the ~10 eV H Lya photons should appear bulk-upscattered to 102 x 10 eV ~ E > 1 k ...
Slajd 1 - INFN-LNF
... the Magellanic Clouds (which is almost a half of the total number of the known NS binaries), but not a single Be/BH binary was found so far (although 58 BH candidate systems ...
... the Magellanic Clouds (which is almost a half of the total number of the known NS binaries), but not a single Be/BH binary was found so far (although 58 BH candidate systems ...
ChESS: ChaMP Extended Stellar Survey
... using the Ty ho, GSC, SDSS, and ChaMP opti al follow-up atalogs. We nd over 200 stellar X-ray sour es overing a magnitude range V = 10 19. This forms an X-ray sele ted, but otherwise unbiased sample of eld stars overing a wide range of spe tral types, ages, metalli ities, and rotations. We have ...
... using the Ty ho, GSC, SDSS, and ChaMP opti al follow-up atalogs. We nd over 200 stellar X-ray sour es overing a magnitude range V = 10 19. This forms an X-ray sele ted, but otherwise unbiased sample of eld stars overing a wide range of spe tral types, ages, metalli ities, and rotations. We have ...
Slide 1
... • What fraction of free energy goes into protons vs. electrons? • What are overall acceleration efficiencies? • What’s the electron energy spectrum? [Probably there are multiple acceleration/dissipation regions – what are energy >spectra< and how do they depend on ambient parameters?] • Marek believ ...
... • What fraction of free energy goes into protons vs. electrons? • What are overall acceleration efficiencies? • What’s the electron energy spectrum? [Probably there are multiple acceleration/dissipation regions – what are energy >spectra< and how do they depend on ambient parameters?] • Marek believ ...
The Super-slow Pulsation X-ray Pulsars in High Mass X
... magnetars above 20 keV: very hard, single power-law, Γ~1.0 -1.5 • Typical X-ray luminosity of magnetars : 1035 -1036 erg/s , 4U 2206+54/2S 0114+65: in the range of 1034 -1036 erg/s ; the source must be powered by accretion not by magnetar activity, requiring magnetar luminosity lower than 1034 erg/s ...
... magnetars above 20 keV: very hard, single power-law, Γ~1.0 -1.5 • Typical X-ray luminosity of magnetars : 1035 -1036 erg/s , 4U 2206+54/2S 0114+65: in the range of 1034 -1036 erg/s ; the source must be powered by accretion not by magnetar activity, requiring magnetar luminosity lower than 1034 erg/s ...
The Application of Forbidden Line X-Ray Diagnostics to the Hot Star
... X-Ray Diagnostics to the Hot Star Tau Sco ...
... X-Ray Diagnostics to the Hot Star Tau Sco ...
ppt
... M83 is a barred spiral galaxy with a starburst nucleus, located in the Centaurus A group, at a distance of 3.7 Mpc. It was observed by Chandra in 2000 April. About 55% of the total emission in the nuclear region is unresolved. About 80% of the unresolved nuclear emission can be attributed to hot the ...
... M83 is a barred spiral galaxy with a starburst nucleus, located in the Centaurus A group, at a distance of 3.7 Mpc. It was observed by Chandra in 2000 April. About 55% of the total emission in the nuclear region is unresolved. About 80% of the unresolved nuclear emission can be attributed to hot the ...
E/DE
... zones, magnetic fields, or the associated magnetic dynamo and corona that our sun has. Thus their discovery 20 years ago as relatively strong soft X-ray sources was a surprise. Hot stars do have strong radiation-driven winds. These winds are subject to a line-driving instability which can lead to sh ...
... zones, magnetic fields, or the associated magnetic dynamo and corona that our sun has. Thus their discovery 20 years ago as relatively strong soft X-ray sources was a surprise. Hot stars do have strong radiation-driven winds. These winds are subject to a line-driving instability which can lead to sh ...
che
... due to a very wide X-ray eclipse In the hard X-ray range (18-60 keV) the eclipse form and width are very variable. ...
... due to a very wide X-ray eclipse In the hard X-ray range (18-60 keV) the eclipse form and width are very variable. ...
ppt - MIT Haystack Observatory
... flaring introduces variability in correlated Lx-Lr which increases the spread , but generally falls within the order of magnitude range of GB relation radio variability appears to be a larger factor than X-ray variability there are situations where even these well-understood (?!) systems belie our e ...
... flaring introduces variability in correlated Lx-Lr which increases the spread , but generally falls within the order of magnitude range of GB relation radio variability appears to be a larger factor than X-ray variability there are situations where even these well-understood (?!) systems belie our e ...
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.