PowerPoint - Chandra X
... Chandra Science Highlight Stephan’s Quintet: A Compact Group of Galaxies about 280 Million Light Years from Earth Chandra X-ray Observatory ACIS Image. ...
... Chandra Science Highlight Stephan’s Quintet: A Compact Group of Galaxies about 280 Million Light Years from Earth Chandra X-ray Observatory ACIS Image. ...
Complex Spatio-Spectral Structure of Diffuse X-Ray
... - Hard X-ray light curve increases with a lower rate of ~20% /yr (f ~ t4). As of 2008-1, f (3-10 keV) = 5.2 x 10-13 erg/cm2/s, Lx = 1.6 x 1035 erg/s. - Cross-comparisons among different X-ray instruments are consistent. - Radio emission shows an evolution of the spectral index: currently S ~ -0.8 ...
... - Hard X-ray light curve increases with a lower rate of ~20% /yr (f ~ t4). As of 2008-1, f (3-10 keV) = 5.2 x 10-13 erg/cm2/s, Lx = 1.6 x 1035 erg/s. - Cross-comparisons among different X-ray instruments are consistent. - Radio emission shows an evolution of the spectral index: currently S ~ -0.8 ...
The High Resolution Camera CXC Newsletter
... search for time variability of the sources, we included 23 observations from November 1999 to February 2005 (adding about 250 ks exposure time). We detected 318 X-ray sources and created long term light curves for all of them. We classified sources as highly variable or outbursting (with subclasses ...
... search for time variability of the sources, we included 23 observations from November 1999 to February 2005 (adding about 250 ks exposure time). We detected 318 X-ray sources and created long term light curves for all of them. We classified sources as highly variable or outbursting (with subclasses ...
WSRT*s contributions to knowledge of neutron stars and black holes
... HD 226868, and discovered in Nov. 1971 this star to be a 5.6 day period spectroscopic binary with a radial velocity amplitude of 64 km/sec (now: 72km/s) [Nature, 7 Jan.1972]. Assuming a “normal” mass of 30 Msun for the supergiant, one finds (since there are no X-ray eclipses), that the minimum mass ...
... HD 226868, and discovered in Nov. 1971 this star to be a 5.6 day period spectroscopic binary with a radial velocity amplitude of 64 km/sec (now: 72km/s) [Nature, 7 Jan.1972]. Assuming a “normal” mass of 30 Msun for the supergiant, one finds (since there are no X-ray eclipses), that the minimum mass ...
Black Holes in M83 - Astronomical Society of the Pacific
... • The X-ray characteristics imply this black hole must be 40-100 times the mass of the sun. • Evidence suggests that the companion star is a red giant several times the mass of the Sun that has expanded enough for the black hole to drag material from it to create a bluish accretion disk as it consum ...
... • The X-ray characteristics imply this black hole must be 40-100 times the mass of the sun. • Evidence suggests that the companion star is a red giant several times the mass of the Sun that has expanded enough for the black hole to drag material from it to create a bluish accretion disk as it consum ...
- Fermi Gamma-ray Space Telescope
... bars as shown in yellow, improving data until about Leff = l000 ...
... bars as shown in yellow, improving data until about Leff = l000 ...
A Chandra Observation of the Massive Star-Forming
... from an evaporating gaseous globule (EGG) for the first time A significant population of X-ray emitting low mass stars (~700) detected, increasing the cluster known members by a factor of 40 ...
... from an evaporating gaseous globule (EGG) for the first time A significant population of X-ray emitting low mass stars (~700) detected, increasing the cluster known members by a factor of 40 ...
PPT
... Solar-B data, together with analysis software tools, will be opened to the world solar physics (and related) communities as quickly as possible. (hopefully in a few months after data acquisition) We welcome proposals for observation plans from outside the Solar-B team. (Details TBD) Collaborative ob ...
... Solar-B data, together with analysis software tools, will be opened to the world solar physics (and related) communities as quickly as possible. (hopefully in a few months after data acquisition) We welcome proposals for observation plans from outside the Solar-B team. (Details TBD) Collaborative ob ...
PowerPoint - Chandra X
... occurred when the core of a massive star collapsed to form a neutron star or black hole (core-collapse supernova). The estimated age of the remnant is 3,000 years. Most of the oxygen in the universe is thought to be dispersed into space by core-collapse supernovas. The oxygen ejecta from such supern ...
... occurred when the core of a massive star collapsed to form a neutron star or black hole (core-collapse supernova). The estimated age of the remnant is 3,000 years. Most of the oxygen in the universe is thought to be dispersed into space by core-collapse supernovas. The oxygen ejecta from such supern ...
Dublin - University of Warwick
... tmin ~ R*3/2 MBH1/2 Duration of event: WD = hours MS = months - years RG = decades - centuries ...
... tmin ~ R*3/2 MBH1/2 Duration of event: WD = hours MS = months - years RG = decades - centuries ...
Solar Flares
... 4. The reconnection of the field below the rising filament provides plasma heating and particle acceleration that we call the flare. 5. The accelerated particles follow the field lines and interact with the chromosphere, heating it and causing the evaporation upflows of the plasma. 6. “Post-flare lo ...
... 4. The reconnection of the field below the rising filament provides plasma heating and particle acceleration that we call the flare. 5. The accelerated particles follow the field lines and interact with the chromosphere, heating it and causing the evaporation upflows of the plasma. 6. “Post-flare lo ...
Discovering X-ray Bright Neutron Stars for Current and Next-Generation
... • A new, X-ray bright neutron star • The hottest INS known • As an INS: High in the Galactic halo and too hot for its age • As an X-ray bright MSP: Possibly closer than RXS J1856 • Possibly the closest neutron star to Earth – good for LIGO • Not detected as radio pulsar (Hessels+07, A&A, ...
... • A new, X-ray bright neutron star • The hottest INS known • As an INS: High in the Galactic halo and too hot for its age • As an X-ray bright MSP: Possibly closer than RXS J1856 • Possibly the closest neutron star to Earth – good for LIGO • Not detected as radio pulsar (Hessels+07, A&A, ...
Astrosat (India) - X-ray Astronomy Group at ISAS
... 4. Measuring magnetic fields of neutron stars By detection and studies of cyclotron lines, most of which lie in 10 – 60 keV region in the spectra of X-ray pulsars. ...
... 4. Measuring magnetic fields of neutron stars By detection and studies of cyclotron lines, most of which lie in 10 – 60 keV region in the spectra of X-ray pulsars. ...
Discovery of 7-13 HZ quasi-periodic oscillations in the new X
... correlation between X-ray count rate and the QPO parameters. In the X-ray colorcolor diagram a two-branched structure was traced out. The QPO parameters are well correlated with the position of the source on these branches. During earlier observations on 1998 April 27, 28 and 29 the count rates were ...
... correlation between X-ray count rate and the QPO parameters. In the X-ray colorcolor diagram a two-branched structure was traced out. The QPO parameters are well correlated with the position of the source on these branches. During earlier observations on 1998 April 27, 28 and 29 the count rates were ...
NASA`s X-ray Eye on the Universe
... times Sun’s mass • SMBH size ~ our solar system (15 lt mins) • SMBH grows as material falls in ...
... times Sun’s mass • SMBH size ~ our solar system (15 lt mins) • SMBH grows as material falls in ...
Polarimeter - Raman Research Institute
... position sensitive proportional counter detectors and works in the 5-30 keV energy band. This instrument will be suitable for X-ray polarisation measurement in about 50 hard X-ray sources. The accretion powered X-ray pulsars, black hole X-ray binaries, rotation powered pulsars and non-thermal SNR wi ...
... position sensitive proportional counter detectors and works in the 5-30 keV energy band. This instrument will be suitable for X-ray polarisation measurement in about 50 hard X-ray sources. The accretion powered X-ray pulsars, black hole X-ray binaries, rotation powered pulsars and non-thermal SNR wi ...
Presentazione di PowerPoint
... Detailed X-ray Spectral Analysis of faint X-ray sources: Towards an universal distribution of intrinsic absorption (selection effects can be easily modelled in X-rays) >~80% of the AGNs agree with simple unification models (TypeI/TypeII Unobscured/Obscured corr.) Evidence for strongly absorbed, C-th ...
... Detailed X-ray Spectral Analysis of faint X-ray sources: Towards an universal distribution of intrinsic absorption (selection effects can be easily modelled in X-rays) >~80% of the AGNs agree with simple unification models (TypeI/TypeII Unobscured/Obscured corr.) Evidence for strongly absorbed, C-th ...
hotstar_xrays
... In the next panel I show synthetic line profiles for a family of coronal models (left) and wind-shock models (right). Line profiles as a function of the scaled wind velocity (x=cDl/lov) are shown for different instrumental resolutions in each sub-panel. The panels have wind attenuation increasing d ...
... In the next panel I show synthetic line profiles for a family of coronal models (left) and wind-shock models (right). Line profiles as a function of the scaled wind velocity (x=cDl/lov) are shown for different instrumental resolutions in each sub-panel. The panels have wind attenuation increasing d ...
The Ultraluminous X-ray Source in Holmberg IX and its Environment
... The two main hypotheses to explain the high luminosity of ULXs are intermediate mass black holes (IMBHs) having 102 to 105 solar masses (Colbert & Mushotzky 1999) or non-isotropic emission beamed into our line-of-sight (King et al. 2001). Here, we are interested in one of these objects, Holmberg IX ...
... The two main hypotheses to explain the high luminosity of ULXs are intermediate mass black holes (IMBHs) having 102 to 105 solar masses (Colbert & Mushotzky 1999) or non-isotropic emission beamed into our line-of-sight (King et al. 2001). Here, we are interested in one of these objects, Holmberg IX ...
PowerPoint - Chandra X
... Chandra are in blue, broadband optical emission in yellow and optical H-alpha emission from hydrogen atoms in red. ...
... Chandra are in blue, broadband optical emission in yellow and optical H-alpha emission from hydrogen atoms in red. ...
Hitomi Observation of the Highly Obscured High-Mass X-ray
... from SXS spectrum thanks to its outstanding energy resolution. We put a constraint on the Kα1 centroid to be 6404.8 +1.7 −1.3 eV, which is tightest among the past observations. Combining the best-fit parameters obtained with SXI and HXI, neutral or slightly ionizing state of Fe is plausible, althoug ...
... from SXS spectrum thanks to its outstanding energy resolution. We put a constraint on the Kα1 centroid to be 6404.8 +1.7 −1.3 eV, which is tightest among the past observations. Combining the best-fit parameters obtained with SXI and HXI, neutral or slightly ionizing state of Fe is plausible, althoug ...
X-ray Astronomy
... (red) from the Spitzer Space Telescope. The Sombrero Galaxy is about 28 million light-years away, near the southern edge of the extensive Virgo cluster of galaxies. ...
... (red) from the Spitzer Space Telescope. The Sombrero Galaxy is about 28 million light-years away, near the southern edge of the extensive Virgo cluster of galaxies. ...
History of X-ray astronomy
The history of X-ray astronomy begins in the 1920s, with interest in short wave communications for the U.S. Navy. This was soon followed by extensive study of the earth's ionosphere. By 1927, interest in the detection of X-ray and ultraviolet (UV) radiation at high altitudes inspired researchers to launch Goddard's rockets into the upper atmosphere to support theoretical studies and data gathering. The first successful rocket flight equipped with instrumentation able to detect solar ultraviolet radiation occurred in 1946. X-ray solar studies began in 1949. By 1973 a solar instrument package orbited on Skylab providing significant solar data.In 1965 the Goddard Space Flight Center program in X-ray astronomy was initiated with a series of balloon-borne experiments. In the 1970s this was followed by high altitude sounding rocket experiments, and that was followed by orbiting (satellite) observatories.The first rocket flight to successfully detect a cosmic source of X-ray emission was launched in 1962 by a group at American Science and Engineering (AS&E).X-ray wavelengths reveal information about the bodies (sources) that emit them.