X-ray spectrometer
... with silicon strip detectors: GLAST is a transistor, vs. EGRET – a vacuum tube ...
... with silicon strip detectors: GLAST is a transistor, vs. EGRET – a vacuum tube ...
Neon Photoionization Experiments on the Z-Machine
... effort in the astrophysics community has focused on coronal plasmas. But with the advent of high-resolution (l/Dl ~ 1000) x-ray spectroscopy in the last several years, a wealth of spectroscopic data for photoionized sources has been generated, and the level of detail and accuracy demanded of models ...
... effort in the astrophysics community has focused on coronal plasmas. But with the advent of high-resolution (l/Dl ~ 1000) x-ray spectroscopy in the last several years, a wealth of spectroscopic data for photoionized sources has been generated, and the level of detail and accuracy demanded of models ...
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 ...
NGC 1808 - Rencontres de Moriond
... + The contribution to soft X-rays might be non-negligible, but is is any case below 30%. + The contribution to hard X-rays is negligible. + The SSC could produce only around 1/50 of the ionizing photons producing the observed emission line spectrum, and no more than 1/10 of the observed FIR luminosi ...
... + The contribution to soft X-rays might be non-negligible, but is is any case below 30%. + The contribution to hard X-rays is negligible. + The SSC could produce only around 1/50 of the ionizing photons producing the observed emission line spectrum, and no more than 1/10 of the observed FIR luminosi ...
This presentation - Fermi Gamma
... Began in 1962 with the discovery of first extra-solar X-ray source (Sco X-1) in a rocket flight by Giacconi et al. (Nobel prize in 2002) First satellite was SAS-A aka Uhuru (1970-3) ...
... Began in 1962 with the discovery of first extra-solar X-ray source (Sco X-1) in a rocket flight by Giacconi et al. (Nobel prize in 2002) First satellite was SAS-A aka Uhuru (1970-3) ...
The activities of the Astronomical Institute of the Slovak Academy of
... symbiotic star AG Draconis, consisting of a cool giant and a compact star, were selected hereafter as examples of solar/stellar research performed recently at AISAS. We used high-resolution images of the Sun taken by the Very high Angular resolution ULtraviolet Telescope (VAULT) in the spectral line ...
... symbiotic star AG Draconis, consisting of a cool giant and a compact star, were selected hereafter as examples of solar/stellar research performed recently at AISAS. We used high-resolution images of the Sun taken by the Very high Angular resolution ULtraviolet Telescope (VAULT) in the spectral line ...
X-ray polarimetry in Xenon gas filled detectors
... (18.25 keV graphite line falls under k=19.5 keV flx. peak from the x-ray tube Mo-anode) ...
... (18.25 keV graphite line falls under k=19.5 keV flx. peak from the x-ray tube Mo-anode) ...
L129 DISCOVERY OF A NEW 89 SECOND X
... respectively, multiplied by a neutral hydrogen absorption factor. The phase-averaged PCA and HEXTE data were fitted simultaneously to various continuum spectral models using XSPEC 10.0 and assuming that XTE J1906109 was at the center of the field of view. For the spectral fits, PCA and HEXTE data in ...
... respectively, multiplied by a neutral hydrogen absorption factor. The phase-averaged PCA and HEXTE data were fitted simultaneously to various continuum spectral models using XSPEC 10.0 and assuming that XTE J1906109 was at the center of the field of view. For the spectral fits, PCA and HEXTE data in ...
LETG Spring, 2015
... with a temperature of a million degrees, and 50 years since coronal X-ray emission was found to be clearly associated with sunspots in “active regions.” A detailed understanding of how the solar corona is heated is still lacking. Given the rate of progress on our closest astrophysical body that we c ...
... with a temperature of a million degrees, and 50 years since coronal X-ray emission was found to be clearly associated with sunspots in “active regions.” A detailed understanding of how the solar corona is heated is still lacking. Given the rate of progress on our closest astrophysical body that we c ...
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 ...
Study of the X-ray Source Population and the Dark Matter
... Owing to the large effective area, large field of view, and high spatial and time resolution, the Wide Field Imager of the Athena Xray Observatory will make it possible to study X-ray sources down to very low flux limits. In Draco dSph, e.g., we will be able to observe X-ray sources with luminositie ...
... Owing to the large effective area, large field of view, and high spatial and time resolution, the Wide Field Imager of the Athena Xray Observatory will make it possible to study X-ray sources down to very low flux limits. In Draco dSph, e.g., we will be able to observe X-ray sources with luminositie ...
Radio-quiet Isolated Neutron Stars
... • What skills have been used before ? • The upper limit of pulse fraction ? • What satellite & what software ? ...
... • What skills have been used before ? • The upper limit of pulse fraction ? • What satellite & what software ? ...
ppt - UCL
... inferred from the X-ray data. The companion was previously thought to be a main sequence B3 star ...
... inferred from the X-ray data. The companion was previously thought to be a main sequence B3 star ...
sources of hard and soft x-ray emission in solar flares: mhd simulation
... The model is based on the observations and on the results of numerical magnetohydrodynamical simulations. At the numerical simulations it is not used any assumptions about the solar flare. All initial and boundary conditions are taken from the observations. To stabilize numerical instabilities the s ...
... The model is based on the observations and on the results of numerical magnetohydrodynamical simulations. At the numerical simulations it is not used any assumptions about the solar flare. All initial and boundary conditions are taken from the observations. To stabilize numerical instabilities the s ...
Harvey`s presentation
... The Iron fluorescence emission line is created when X-rays scatter and are absorbed in dense matter, close to the event horizon of the black hole. ...
... The Iron fluorescence emission line is created when X-rays scatter and are absorbed in dense matter, close to the event horizon of the black hole. ...
X-ray heating of the chromosphere
... c) There are significant differences in height in the chromosphere between the layers where the core of H line profile is formed and the layers where deposited energy reach the maximum. In such a case the intensities of central parts of H line profiles should not be close related with the rates of ...
... c) There are significant differences in height in the chromosphere between the layers where the core of H line profile is formed and the layers where deposited energy reach the maximum. In such a case the intensities of central parts of H line profiles should not be close related with the rates of ...
Spectral-Type Trends: Absorption
... Or, is it due to increasing wind absorption of X-rays for hotter stars that have stronger winds? (Optional:) (Hydrodynamics simulations (left column) do not predict a trend in shock strength with stellar luminosity or surface temperature. So, an X-ray emission trend would be very surprising. But ste ...
... Or, is it due to increasing wind absorption of X-rays for hotter stars that have stronger winds? (Optional:) (Hydrodynamics simulations (left column) do not predict a trend in shock strength with stellar luminosity or surface temperature. So, an X-ray emission trend would be very surprising. But ste ...
WSRT*s contributions to knowledge of neutron stars and black holes
... Assuming a “normal” mass of 30 Msun for the supergiant, one finds (since there are no X-ray eclipses), that the minimum mass of the unseen companion is > 6 Msun. As this is larger than the upper mass limit of 3.4 Msun of neutron stars, the companion, if it is the X-ray source, must be a BLACK HOLE . ...
... Assuming a “normal” mass of 30 Msun for the supergiant, one finds (since there are no X-ray eclipses), that the minimum mass of the unseen companion is > 6 Msun. As this is larger than the upper mass limit of 3.4 Msun of neutron stars, the companion, if it is the X-ray source, must be a BLACK HOLE . ...
X-ray Sources in Nearby Galaxies Q. Daniel Wang University of Massachusetts
... • Feeding of AGNs • Evolution of HMXBs and LMXBs (talk by Andreas Zezas). • Discrete source populations such as SNe, SNRs, YSOs. • Effects of AGN energy injection, accretion from the IGM, clustering environment on diffuse hot plasma. • Diffuse hard X-rays: e.g., reflection, inverse Compton scat ...
... • Feeding of AGNs • Evolution of HMXBs and LMXBs (talk by Andreas Zezas). • Discrete source populations such as SNe, SNRs, YSOs. • Effects of AGN energy injection, accretion from the IGM, clustering environment on diffuse hot plasma. • Diffuse hard X-rays: e.g., reflection, inverse Compton scat ...
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 ...
X-Ray Astronomy Poster_Final
... X-rays are electromagnetic radiation of energy ranging from 0.1keV to a few 100keV. We see many objects in the sky that emit visible light but some objects emit X-rays and some are even more bright in X-rays than in visible light. ...
... X-rays are electromagnetic radiation of energy ranging from 0.1keV to a few 100keV. We see many objects in the sky that emit visible light but some objects emit X-rays and some are even more bright in X-rays than in visible light. ...
X-ray astronomy - University of Warwick
... • Assuming optically-thin thermal plasma emission with kT=6 keV and interstellar absorption of NH=1020cm-2, estimate the 2-10 keV energy flux of SU UMa • Further calculate the XMM-Newton RGS count rate, and determine how long an observation is required to accumulate ...
... • Assuming optically-thin thermal plasma emission with kT=6 keV and interstellar absorption of NH=1020cm-2, estimate the 2-10 keV energy flux of SU UMa • Further calculate the XMM-Newton RGS count rate, and determine how long an observation is required to accumulate ...
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.