3. Neutron Star X-ray Binaries
... Straightforward dependency of the magnetic field strength with the mass of the BH allowing us to establish its upper limit for the jet formation in the case of supermassive BHs as well: Schwarzschild and Kerr Supermassive BHs ...
... Straightforward dependency of the magnetic field strength with the mass of the BH allowing us to establish its upper limit for the jet formation in the case of supermassive BHs as well: Schwarzschild and Kerr Supermassive BHs ...
Document
... INTRODUCTIONu The hot, diffuse, x-ray emitting interstellar medium of the Milky Way Galaxy appears almost featureless, unless it is observed in the soft x-ray band. In 1995, complex structures, visible only between 0.1 and 2.0keV, were revealed by the ROSAT all-sky survey. The XMM-Newton observatory ...
... INTRODUCTIONu The hot, diffuse, x-ray emitting interstellar medium of the Milky Way Galaxy appears almost featureless, unless it is observed in the soft x-ray band. In 1995, complex structures, visible only between 0.1 and 2.0keV, were revealed by the ROSAT all-sky survey. The XMM-Newton observatory ...
Frequency x Energy Spectral fitting is degenerate : timing
... Problem!! SM09 used 70ks of data from Obs 2 - dominated by bgd flaring. Lets look at the observations again with more appropriate GTIs ...
... Problem!! SM09 used 70ks of data from Obs 2 - dominated by bgd flaring. Lets look at the observations again with more appropriate GTIs ...
ppt - Astronomy at Swarthmore College
... Some of the other hot stars observed with Chandra show broad, blueshifted, and asymmetric line profiles, similar to those seen in ζ Pup But…some hot stars have x-ray spectra with quite narrow lines, that are especially strong and high energy - not consistent with line-force instability wind shocks ...
... Some of the other hot stars observed with Chandra show broad, blueshifted, and asymmetric line profiles, similar to those seen in ζ Pup But…some hot stars have x-ray spectra with quite narrow lines, that are especially strong and high energy - not consistent with line-force instability wind shocks ...
A Legacy Study of Stellar Life Cycles in the Galactic Center
... • Unusual for an XRB to be in outburst for so long (Chen et al. 1997). • Microquasars and some pulsars might have required luminosity and hard spectrum in high state • Fluorescent line seen in Sgr B2, Sgr C, and central parsecs of Galaxy, so would need multiple microquasars, such as GRS 1915+10, but ...
... • Unusual for an XRB to be in outburst for so long (Chen et al. 1997). • Microquasars and some pulsars might have required luminosity and hard spectrum in high state • Fluorescent line seen in Sgr B2, Sgr C, and central parsecs of Galaxy, so would need multiple microquasars, such as GRS 1915+10, but ...
AMUSE-Virgo on the survival of super-massive black holes
... Duty cycle of super-massive black hole (highly sub-Eddington) activity ...
... Duty cycle of super-massive black hole (highly sub-Eddington) activity ...
Optical studies of an ultraluminous X-ray source: NGC1313 X-2 Jifeng Liu
... • need further observations • with higher signal-to-noise ratios and higher spectral ...
... • need further observations • with higher signal-to-noise ratios and higher spectral ...
AAS_WFXT_Solar_System_11Jan2010
... study. Most objects have been detected with only a few photons. • There is an important list of solar system objects that have yet to be detected in the x-ray : Mercury, the ice giants Uranus/Neptune, the Main Belt comets,KBOs, and the heliopause. • Large Scale WFXT Imaging will allow for direct, co ...
... study. Most objects have been detected with only a few photons. • There is an important list of solar system objects that have yet to be detected in the x-ray : Mercury, the ice giants Uranus/Neptune, the Main Belt comets,KBOs, and the heliopause. • Large Scale WFXT Imaging will allow for direct, co ...
GEARS Workshop Monday - Georgia Southern University
... • This composite image uses data from three of NASA's Great Observatories. The Chandra X-ray image is shown in blue, the Hubble Space Telescope optical image is in red and yellow, and the Spitzer Space Telescope's infrared image is in purple. The X-ray image is smaller than the others because extrem ...
... • This composite image uses data from three of NASA's Great Observatories. The Chandra X-ray image is shown in blue, the Hubble Space Telescope optical image is in red and yellow, and the Spitzer Space Telescope's infrared image is in purple. The X-ray image is smaller than the others because extrem ...
Introduction to Accretion Phenomena in Astrophysics
... surface of the Roche lobe filling component (donor) is transferred to the other, accreting star. The mass transfer dominates the evolution of the system; the inflowing gas may form accretion disc around the accreting star. Examples: X-ray binaries and Cataclysmic variable stars. • A contact binary: ...
... surface of the Roche lobe filling component (donor) is transferred to the other, accreting star. The mass transfer dominates the evolution of the system; the inflowing gas may form accretion disc around the accreting star. Examples: X-ray binaries and Cataclysmic variable stars. • A contact binary: ...
ppt - SLAC
... • Jets are clearly visible in high-resolution radio images • Blazars are commonly detected as MeV – GeV and even TeV g-ray emitters (~ 60 detected by EGRET) • Rapidly variable in all bands including g-rays ...
... • Jets are clearly visible in high-resolution radio images • Blazars are commonly detected as MeV – GeV and even TeV g-ray emitters (~ 60 detected by EGRET) • Rapidly variable in all bands including g-rays ...
Slajd 1 - INFN-LNF
... Another possible factor may be related to the previous evolution of a Be star. If, indeed, a B star must be a member of a binary system and undergo a mass transfer in order to become a Be star, then one can imagine that the systems composed of a Be star and a relatively less massive companion (which ...
... Another possible factor may be related to the previous evolution of a Be star. If, indeed, a B star must be a member of a binary system and undergo a mass transfer in order to become a Be star, then one can imagine that the systems composed of a Be star and a relatively less massive companion (which ...
X-Ray Binaries
... companion (neutron star, black hole, [white dwarf ]) • traditionally two main classes: high-mass X-ray binaries (HMXBs; M2 > ∼ 10 M¯) and low-mass X-ray binaries (LMXBs; M2 < ∼ 1.5 M¯) . missing intermediate-mass systems? . probably not: most systems classified as LMXBs almost certainly originate fr ...
... companion (neutron star, black hole, [white dwarf ]) • traditionally two main classes: high-mass X-ray binaries (HMXBs; M2 > ∼ 10 M¯) and low-mass X-ray binaries (LMXBs; M2 < ∼ 1.5 M¯) . missing intermediate-mass systems? . probably not: most systems classified as LMXBs almost certainly originate fr ...
EXTREME NEUTRON STARS Christopher Thompson Canadian Institute for Theoretical Astrophysics University of Toronto
... Helicity Injection into the Magnetosphere Actively bursting magnetars show: Strong non-thermal X-ray emission when not bursting Long term (up to years) stable variations in X-ray pulse profile and spindown torque after outbursts ...
... Helicity Injection into the Magnetosphere Actively bursting magnetars show: Strong non-thermal X-ray emission when not bursting Long term (up to years) stable variations in X-ray pulse profile and spindown torque after outbursts ...
Puzzling X-rays from the new colliding wind binary Wolf–Rayet 65
... has a period of a few days: the two data points obtained in 2003 April indicate constant count rates over at least a week. Moreover, two data points in the light curve separated by two months (2004 December and 2005 February) are similar, while there is an increase in emission by nearly 70 per cent ...
... has a period of a few days: the two data points obtained in 2003 April indicate constant count rates over at least a week. Moreover, two data points in the light curve separated by two months (2004 December and 2005 February) are similar, while there is an increase in emission by nearly 70 per cent ...
X-ray output should be time variable
... Bright stars in the spectral range earlier than about B3 are soft X-ray sources, with LX ~ 10-7 LBol THEORY •O star X-ray emission comes from shock-heated gas present in their stellar winds; for B stars, the situation is more uncertain, and their Xrays may be related to magnetic fields, at least in ...
... Bright stars in the spectral range earlier than about B3 are soft X-ray sources, with LX ~ 10-7 LBol THEORY •O star X-ray emission comes from shock-heated gas present in their stellar winds; for B stars, the situation is more uncertain, and their Xrays may be related to magnetic fields, at least in ...
205 Advances in Natural and Applied Sciences, 4(2): 205-209, 2010 ISSN 1995-0772
... Fig. 1: A schematic view of an X-ray binary. Gas is pulled off the normal star by the gravity of the compact object The actual study of the X-ray binary stars began in the 1970s with the use of satellites equipped with Xray detectors. The first one, UHURU, was launched in 1970 (Giacconi et al., 1972 ...
... Fig. 1: A schematic view of an X-ray binary. Gas is pulled off the normal star by the gravity of the compact object The actual study of the X-ray binary stars began in the 1970s with the use of satellites equipped with Xray detectors. The first one, UHURU, was launched in 1970 (Giacconi et al., 1972 ...
PG_Lecture_Dec18_2008
... He, C, N, O, Ne, Mg, Al, Si, S, Ar, Ca, Fe. Elements normally ionized, e.g. in stellar coronae: C in form of C+3, C+4, C+5; Fe is in form of Fe+9, Fe+10… Fe+16. Often use iso-electronic series to describe an ion, e.g. C+4 is “He-like” (2 electrons), C+5 is “H-like” (1 electron). Only ions with at le ...
... He, C, N, O, Ne, Mg, Al, Si, S, Ar, Ca, Fe. Elements normally ionized, e.g. in stellar coronae: C in form of C+3, C+4, C+5; Fe is in form of Fe+9, Fe+10… Fe+16. Often use iso-electronic series to describe an ion, e.g. C+4 is “He-like” (2 electrons), C+5 is “H-like” (1 electron). Only ions with at le ...
Unique observations of a newborn star provide information on the
... been caught in the act of flaring, it is the first that has occurred in modern times when its behavior could be monitored not only in visible light, but also in radio, infrared and X-ray wavelengths. “In FU-Orionis stars, these outbursts are very brief,” says Weintraub, associate professor of astron ...
... been caught in the act of flaring, it is the first that has occurred in modern times when its behavior could be monitored not only in visible light, but also in radio, infrared and X-ray wavelengths. “In FU-Orionis stars, these outbursts are very brief,” says Weintraub, associate professor of astron ...
Article PDF - IOPscience
... the effects on the average rate of variations in the effective detection efficiency for a point source as its image passes over the grid structure of the PSPC window. The count rate varies about the overall average of 3.79 counts s21 on timescales from several minutes to hours. (For comparison, we c ...
... the effects on the average rate of variations in the effective detection efficiency for a point source as its image passes over the grid structure of the PSPC window. The count rate varies about the overall average of 3.79 counts s21 on timescales from several minutes to hours. (For comparison, we c ...
lecture2 - X-Ray
... The old zoo of neutron stars In 60s the first X-ray sources have been discovered. They were neutron stars in close binary systems, BUT ... .... they were «not recognized».... Now we know hundreds of X-ray binaries with neutron stars in the Milky Way and in other galaxies. ...
... The old zoo of neutron stars In 60s the first X-ray sources have been discovered. They were neutron stars in close binary systems, BUT ... .... they were «not recognized».... Now we know hundreds of X-ray binaries with neutron stars in the Milky Way and in other galaxies. ...
Nobuyuki Kawai
... Strong beaming x100 unseen (off beam axis) short GRB! • many more target events for GW! • no regular “GRB”: how to identify? – may have delayed X-ray/optical afterglow ...
... Strong beaming x100 unseen (off beam axis) short GRB! • many more target events for GW! • no regular “GRB”: how to identify? – may have delayed X-ray/optical afterglow ...
rastieee
... and spatial variations of a number of key constituents and parameters in the lower thermosphere (90-320 km). The QB50 project is supported by the EU 7th Framework Program. ...
... and spatial variations of a number of key constituents and parameters in the lower thermosphere (90-320 km). The QB50 project is supported by the EU 7th Framework Program. ...
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.