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 ...
SSM hardware
... • Most other experiments on ASTROSAT are pointed to a specific object for relatively long periods of time (~hours to days). • Scanning mechanism necessary for monitors to scan the sky multiple times per day. • FOV of two monitors forms an ‘X’ in the sky. Third detector views the perpendicular direct ...
... • Most other experiments on ASTROSAT are pointed to a specific object for relatively long periods of time (~hours to days). • Scanning mechanism necessary for monitors to scan the sky multiple times per day. • FOV of two monitors forms an ‘X’ in the sky. Third detector views the perpendicular direct ...
Neon Photoionization Experiments on the Z-Machine
... primarily to model astrophysical photoionized plasmas and benchmark codes used to study astrophysical sources, but there are also basic physics applications, as well as potential applications to gas filled hohlraums and x-ray laser sources. ...
... primarily to model astrophysical photoionized plasmas and benchmark codes used to study astrophysical sources, but there are also basic physics applications, as well as potential applications to gas filled hohlraums and x-ray laser sources. ...
Astronomy Astrophysics + Infrared identification of 2XMM J191043.4
... He ii 1.6918 μm or He i 1.7002 μm clearly. Other hydrogen lines are not detected, probably because their intensities would be below the continuum noise level. On the other hand, cool supergiant stars show CO-band absorption lines between 2.29 and 2.35 μm that are not present in our spectrum. We ther ...
... He ii 1.6918 μm or He i 1.7002 μm clearly. Other hydrogen lines are not detected, probably because their intensities would be below the continuum noise level. On the other hand, cool supergiant stars show CO-band absorption lines between 2.29 and 2.35 μm that are not present in our spectrum. We ther ...
Do flares in Saggitarius A* reflect the last stage of tidal capture
... Radiation diffusion time of a light source (tg) : Let the source be a homogeneous sphere made of the most transparent material available – hydrogen at a high enough temperature -, so that its opacity is due only to Thomson scattering (k = 0.4cm2/g), and assume that photons are loosing no energy wh ...
... Radiation diffusion time of a light source (tg) : Let the source be a homogeneous sphere made of the most transparent material available – hydrogen at a high enough temperature -, so that its opacity is due only to Thomson scattering (k = 0.4cm2/g), and assume that photons are loosing no energy wh ...
X-ray Astronomy and the search for Black Holes
... From 2005 summer to present, CH Cyg appears to have been in a second type of low state: the soft X-ray probably is still bright while the hard X-rays appear to be low ...
... From 2005 summer to present, CH Cyg appears to have been in a second type of low state: the soft X-ray probably is still bright while the hard X-rays appear to be low ...
Gravitationally redshifted absorption lines in the x
... The lines would then all have a gravitational redshift of z = 0.35, which would correspond to a neutron star in the mass range of 1.4–1.8 M๏ and in the radius range of 9–12 km. ...
... The lines would then all have a gravitational redshift of z = 0.35, which would correspond to a neutron star in the mass range of 1.4–1.8 M๏ and in the radius range of 9–12 km. ...
X-ray binaries
... • When a strongly magnetic neutron star accretes plasma from a companion star or the interstellar medium, its magnetic field becomes dynamically important close to the stellar surface and determines the properties of the accretion flow. The radius at which the effects of the magnetic field dominate all ...
... • When a strongly magnetic neutron star accretes plasma from a companion star or the interstellar medium, its magnetic field becomes dynamically important close to the stellar surface and determines the properties of the accretion flow. The radius at which the effects of the magnetic field dominate all ...
The Sun`s X- ray Emission During the Recent Solar
... that gives rise to the X-ray emissions. A 441- second period on 21 February was chosen for analysis when the X-ray level was extremely low (4.7 × 10 -10 watts per square meter; for comparison, during much of the previous solar minimum the X-ray level was at least 2 orders of magnitude greater). Duri ...
... that gives rise to the X-ray emissions. A 441- second period on 21 February was chosen for analysis when the X-ray level was extremely low (4.7 × 10 -10 watts per square meter; for comparison, during much of the previous solar minimum the X-ray level was at least 2 orders of magnitude greater). Duri ...
Harvey`s presentation
... Study dynamics of Cosmic Feedback (outflow of mechanical energy, radiation, and chemical elements from star formation and black holes to the interstellar and intergalactic medium) ...
... Study dynamics of Cosmic Feedback (outflow of mechanical energy, radiation, and chemical elements from star formation and black holes to the interstellar and intergalactic medium) ...
Program_files/40 Years of Microquasarsembed
... satellites at ~1-10 kev (van Paradis 1995, Liu et al. 2000, 2001 catalogues) • High Mass ~ 10 Msun • Low Mass ~ 1 Msun • .All powered by accretion onto a compact object (neutron star or black hole). • Roche Lobe overflow or wind? • ~20 % have been found to have radio emission ...
... satellites at ~1-10 kev (van Paradis 1995, Liu et al. 2000, 2001 catalogues) • High Mass ~ 10 Msun • Low Mass ~ 1 Msun • .All powered by accretion onto a compact object (neutron star or black hole). • Roche Lobe overflow or wind? • ~20 % have been found to have radio emission ...
Altair - the hottest `cool` star in X-rays
... at temperatures in the range of 1 – 4 MK, additionally a weak hotter component seems to contribute at a few percent level. These properties are quite typical for weakly active stars and similar to those of the quiescent Sun. This suggests that large active regions or significant flaring components a ...
... at temperatures in the range of 1 – 4 MK, additionally a weak hotter component seems to contribute at a few percent level. These properties are quite typical for weakly active stars and similar to those of the quiescent Sun. This suggests that large active regions or significant flaring components a ...
Barger - Chandra X-Ray Observatory (CXC)
... Conclude: if one is going to split X-ray luminosity functions by class, one should do it based on optical spectral class alone or by X-ray color alone, but one should not try to mix them, because we do not understand how to relate one to the other But, maybe it would make sense just to split X-ray ...
... Conclude: if one is going to split X-ray luminosity functions by class, one should do it based on optical spectral class alone or by X-ray color alone, but one should not try to mix them, because we do not understand how to relate one to the other But, maybe it would make sense just to split X-ray ...
X-ray heating of the chromosphere
... a) Spectral distribution of the soft X-ray intensity in 1–300 Å spectral range with the step of 1 Å at upper boundary of the chromosphere within the analyzed parts of the flares (plane-parellel approximation, sources are isothermal) - Mewe et al., 1985; Mewe et al., 1986 (Solar-Soft) - emissivity ...
... a) Spectral distribution of the soft X-ray intensity in 1–300 Å spectral range with the step of 1 Å at upper boundary of the chromosphere within the analyzed parts of the flares (plane-parellel approximation, sources are isothermal) - Mewe et al., 1985; Mewe et al., 1986 (Solar-Soft) - emissivity ...
A Proposed Collaboration Between LIGO
... detecting the corresponding gravitational wave (GW) emissions by the laser interferometer gravitational wave observatory, LIGO. GWs are extremely hard to detect because they are weak signals in a floor of instrument noise. Optical observations of CCSNe are already used in coincidence with LIGO data, ...
... detecting the corresponding gravitational wave (GW) emissions by the laser interferometer gravitational wave observatory, LIGO. GWs are extremely hard to detect because they are weak signals in a floor of instrument noise. Optical observations of CCSNe are already used in coincidence with LIGO data, ...
High Energy Processes in Young Stellar Objects
... Field lines above corotation radius Magnetic loop with both feet in the disk Binary YSOs but less important Reconnection and displacement of footprint are more likely to occur in YSOs due to more possible magnetic configuration offered by star-star, star-disk, disk-disk interaction ...
... Field lines above corotation radius Magnetic loop with both feet in the disk Binary YSOs but less important Reconnection and displacement of footprint are more likely to occur in YSOs due to more possible magnetic configuration offered by star-star, star-disk, disk-disk interaction ...
What is X-ray Astronomy? - Extreme Universe Laboratory
... Plerion: is derived from the Greek word “pleres” which means “full”. Crab nebula is the remnant of Sne explosion (perhaps type II) observed by the Chinese Astronomers in 1054 (July 4th). The pulsar at the center has a period of 33milli-sec. Crab shows pulsed emission from radio to optical to >50 Mev ...
... Plerion: is derived from the Greek word “pleres” which means “full”. Crab nebula is the remnant of Sne explosion (perhaps type II) observed by the Chinese Astronomers in 1054 (July 4th). The pulsar at the center has a period of 33milli-sec. Crab shows pulsed emission from radio to optical to >50 Mev ...
PowerPoint - Chandra X
... With an age of about 200 million years this is the oldest isolated pulsar ever detected in X-rays. Among pulsar that have not been spun-up in a binary system, it is over 10 times older than the previous record holder with an X-ray detection. At a distance of 770 light years, it is one of the nearest ...
... With an age of about 200 million years this is the oldest isolated pulsar ever detected in X-rays. Among pulsar that have not been spun-up in a binary system, it is over 10 times older than the previous record holder with an X-ray detection. At a distance of 770 light years, it is one of the nearest ...
Feigelson, E. (PSU)
... on protoplanetary disks • PMS X-ray ionization will heat gas and change chemistry in disk outer layers. • PMS X-rays may be an important ionization source at the base of bipolar outflows. • X-ray ionization is likely to induce MRI turbulence affecting accretion, planetesimal formation, migration, .. ...
... on protoplanetary disks • PMS X-ray ionization will heat gas and change chemistry in disk outer layers. • PMS X-rays may be an important ionization source at the base of bipolar outflows. • X-ray ionization is likely to induce MRI turbulence affecting accretion, planetesimal formation, migration, .. ...
X-ray polarimetry in Xenon gas filled detectors
... azimuthal angles relative to the polarization direction, β is the dipole asymmetry parameter and P2 is the 2nd Legendre polynomial) Derevianko et. al., At.Dat.Nucl.Dat. Tables 73 (1999) 153 ...
... azimuthal angles relative to the polarization direction, β is the dipole asymmetry parameter and P2 is the 2nd Legendre polynomial) Derevianko et. al., At.Dat.Nucl.Dat. Tables 73 (1999) 153 ...
Deep O/IR Survey Of Chandra Galactic Bulge Fields
... analysis suggest that a large subset of the sources are intrinsically hard, and reasonably described by a power law with photon index =0. The typical luminosities of these objects are in the range 10 3133 erg/s. The largest well studied class of objects fitting this description are high magnetic fie ...
... analysis suggest that a large subset of the sources are intrinsically hard, and reasonably described by a power law with photon index =0. The typical luminosities of these objects are in the range 10 3133 erg/s. The largest well studied class of objects fitting this description are high magnetic fie ...
X-Ray Astronomy Poster_Final
... 3. Charge Coupled Devices (CCD) A CCD chip consists of an array of pixels. Each ...
... 3. Charge Coupled Devices (CCD) A CCD chip consists of an array of pixels. Each ...
A Decade in the Life of the Massive Black-Hole Binary... Silas Laycock !
... galaxy IC 10. The Wolf Rayet + BH binary known as IC10 X-1 is regarded as one of the most massive stellar black holes; a class of objects representing the pinnacle of the stellar mass function. BH binaries occupy key roles in seeding SMBHs, producing long GRBs at birth, and gravitational waves at de ...
... galaxy IC 10. The Wolf Rayet + BH binary known as IC10 X-1 is regarded as one of the most massive stellar black holes; a class of objects representing the pinnacle of the stellar mass function. BH binaries occupy key roles in seeding SMBHs, producing long GRBs at birth, and gravitational waves at de ...
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.