PDF only - at www.arxiv.org.
... models of radiation-driven accretion disk winds (17). An independent corroboration of the above estimate comes from the variability timescale of ~1 week of the Fe-K absorption feature, probed during the monitoring of PDS 456 by the Suzaku X-ray satellite in early 2013 (18). Indeed, the historical be ...
... models of radiation-driven accretion disk winds (17). An independent corroboration of the above estimate comes from the variability timescale of ~1 week of the Fe-K absorption feature, probed during the monitoring of PDS 456 by the Suzaku X-ray satellite in early 2013 (18). Indeed, the historical be ...
The Historical X-ray Transient KY TrA in quiescence
... and δ = −61:52:58.1 (2000) by Murdin et al. (1977) 12 d after the outburst. These authors showed a Schmidt plate of the proposed counterpart but no deep image with the target in quiescence has been published to date. In Fig. 1 we show an improved finding chart of KY TrA (I-band, 1800 s exposure and ...
... and δ = −61:52:58.1 (2000) by Murdin et al. (1977) 12 d after the outburst. These authors showed a Schmidt plate of the proposed counterpart but no deep image with the target in quiescence has been published to date. In Fig. 1 we show an improved finding chart of KY TrA (I-band, 1800 s exposure and ...
pdf
... A general, insightful, and useful introduction to X-ray imaging systems and zone plates is given by Spiller.6 The specific status of diffractive optics for X-rays is reviewed by Michette11 where the use of zone plates for microscopy is emphasized. He points out the use of a central stop and axial ap ...
... A general, insightful, and useful introduction to X-ray imaging systems and zone plates is given by Spiller.6 The specific status of diffractive optics for X-rays is reviewed by Michette11 where the use of zone plates for microscopy is emphasized. He points out the use of a central stop and axial ap ...
ppt - chris.engelbrecht.nithep.ac.za
... 1E 0102.2-7219 (Figure 1) is an oxygen-rich supernova remnant in the Small Magellanic Cloud. X-ray observations reveal the blast wave andyield a shock radius of 22 arcseconds at the 60 kpc distance of the SMC. The spectrum of the blast wave yields a temperature of kTx 0.8 keV and an ionization tim ...
... 1E 0102.2-7219 (Figure 1) is an oxygen-rich supernova remnant in the Small Magellanic Cloud. X-ray observations reveal the blast wave andyield a shock radius of 22 arcseconds at the 60 kpc distance of the SMC. The spectrum of the blast wave yields a temperature of kTx 0.8 keV and an ionization tim ...
A STRONGLY MAGNETIZED PULSAR WITHIN THE GRASP OF THE MILKY... SUPERMASSIVE BLACK HOLE Rea ,
... 19 AIM (CEA/DSM-CNRS-Université Paris Diderot), Irfu/Service d’Astrophysique, Saclay, F-91191 Gif-sur-Yvette, France Received 2013 June 21; accepted 2013 August 15; published 2013 September 11 ...
... 19 AIM (CEA/DSM-CNRS-Université Paris Diderot), Irfu/Service d’Astrophysique, Saclay, F-91191 Gif-sur-Yvette, France Received 2013 June 21; accepted 2013 August 15; published 2013 September 11 ...
$doc.title
... in the same model). If we assume that the Gaussian component is the result of an expanding source that originated at the onset of the major outburst, that is about 13 days before our observations, and that the expansion velocity of the jet is constant, the derived velocity, taking into account the s ...
... in the same model). If we assume that the Gaussian component is the result of an expanding source that originated at the onset of the major outburst, that is about 13 days before our observations, and that the expansion velocity of the jet is constant, the derived velocity, taking into account the s ...
Astronomy Astrophysics The accretion environment in Vela X-1 during a flaring period using
... with a phenomenological model formed by three absorbed power laws plus three emission lines. After analysing the variations with orbital phase of the column density of each component, as well as those in the Fe and Ni fluorescence lines, we provide a physical interpretation for each spectral compone ...
... with a phenomenological model formed by three absorbed power laws plus three emission lines. After analysing the variations with orbital phase of the column density of each component, as well as those in the Fe and Ni fluorescence lines, we provide a physical interpretation for each spectral compone ...
Chandra HETGS Multiphase Spectroscopy Of The Young
... X-ray–emitting plasma in the circumstellar environment of this young, magnetized O star and thus to assess the mechanism responsible for generating the unusual levels of X-ray emission in 1 Ori C. The time-independent nature of the original Babel & Montmerle model leads to a steady state configurat ...
... X-ray–emitting plasma in the circumstellar environment of this young, magnetized O star and thus to assess the mechanism responsible for generating the unusual levels of X-ray emission in 1 Ori C. The time-independent nature of the original Babel & Montmerle model leads to a steady state configurat ...
Phenomenon of total external reflection of x rays
... an important and often a unique source of information on the fundamental properties of solids, liquids, and interfaces. The phenomenon of total external reflection underlies a traditional branch of x-ray optics which is being used increasingly in research and physics, astrophysics, and biology.4 We ...
... an important and often a unique source of information on the fundamental properties of solids, liquids, and interfaces. The phenomenon of total external reflection underlies a traditional branch of x-ray optics which is being used increasingly in research and physics, astrophysics, and biology.4 We ...
From: BXSVR0::OWOCKI 12-JAN-2001 10:16:41.12 To: DCOHEN
... a toy model. Sure enough, I got profiles that are reasonably symmetric, with slight blueshifts of the peak line emission. There is still some asymmetry between red and blue wings, as there must, but optical depth effects do introduce a new 'knob', and the lines being shown in papers are presumably t ...
... a toy model. Sure enough, I got profiles that are reasonably symmetric, with slight blueshifts of the peak line emission. There is still some asymmetry between red and blue wings, as there must, but optical depth effects do introduce a new 'knob', and the lines being shown in papers are presumably t ...
ertan et al 11cesme
... AXP/SGRs indeed require strong magnetic fields. We proposed in a series of earlier papers on fallback disk model that the magnetar fields powering the bursts could be in higher multipole components of the magnetic field which are localized close to the surface of the star rather than in the large sc ...
... AXP/SGRs indeed require strong magnetic fields. We proposed in a series of earlier papers on fallback disk model that the magnetar fields powering the bursts could be in higher multipole components of the magnetic field which are localized close to the surface of the star rather than in the large sc ...
3011800000360
... unpulsed optical / IR emission from the AXP 4U 0142+61 is in agreement with the expectations of a standard thin-disk model (Ertan & Cheng 2004a). In the disk models, the inner radius of the disk is consistent with a dipole component of the magnetic field with a strength of 1012 G on the stellar sur ...
... unpulsed optical / IR emission from the AXP 4U 0142+61 is in agreement with the expectations of a standard thin-disk model (Ertan & Cheng 2004a). In the disk models, the inner radius of the disk is consistent with a dipole component of the magnetic field with a strength of 1012 G on the stellar sur ...
"Experimental study of charge diffusion in the undepleted silicon of X-ray CCDs"
... along the row. The full width at half maximum (FWHM, denoted hereafter as ) of the Gaussian and the total charge in all the pixels related to the event can characterize both the depth in the neutral bulk at which an event happened and the total charge in the original electron cloud. This relation be ...
... along the row. The full width at half maximum (FWHM, denoted hereafter as ) of the Gaussian and the total charge in all the pixels related to the event can characterize both the depth in the neutral bulk at which an event happened and the total charge in the original electron cloud. This relation be ...
GRB EXPERIMENT
... • To explain SGRs and AXPs, however, B must be greater than the quantum critical value 4.4 x 1013 G, where the energy between electron Landau levels equals their rest mass • Some AXPs and SGRs require B~1015 Gauss, so these magnetars have the strongest cosmic magnetic fields that we know of in the u ...
... • To explain SGRs and AXPs, however, B must be greater than the quantum critical value 4.4 x 1013 G, where the energy between electron Landau levels equals their rest mass • Some AXPs and SGRs require B~1015 Gauss, so these magnetars have the strongest cosmic magnetic fields that we know of in the u ...
What does the EUV and thin film group do?
... Images from www.schott.com/magazine/english/info99/ and www.lbl.gov/Science-Articles/Archive/xray-inside-cells.html. ...
... Images from www.schott.com/magazine/english/info99/ and www.lbl.gov/Science-Articles/Archive/xray-inside-cells.html. ...
Swift and NuSTAR observations of XTE J1859+083
... The latest outburst of XTE J1859+083 was reported on February 8th 2015 by the MAXI/GSC nova alert system (Negoro et al., 2015) and confirmed by the BAT hard X-ray transient monitor (Krimm et al., 2015). Observations with Swift followed right after and the observations of NuSTAR and Swift used in thi ...
... The latest outburst of XTE J1859+083 was reported on February 8th 2015 by the MAXI/GSC nova alert system (Negoro et al., 2015) and confirmed by the BAT hard X-ray transient monitor (Krimm et al., 2015). Observations with Swift followed right after and the observations of NuSTAR and Swift used in thi ...
0004-637X 778 2 119
... calculations imply that magnetized neutron stars could accrete matter from the disk even in the fast-rotator phase (see, e.g., Rappaport et al. 2004). The critical value of the fastness parameter ω∗ = Ω∗ /ΩK (rA ), above which accretion is completely hindered, is not well known. Here, ΩK (rA ) is th ...
... calculations imply that magnetized neutron stars could accrete matter from the disk even in the fast-rotator phase (see, e.g., Rappaport et al. 2004). The critical value of the fastness parameter ω∗ = Ω∗ /ΩK (rA ), above which accretion is completely hindered, is not well known. Here, ΩK (rA ) is th ...
1. INTRODUCTION
... as these stars often show several distinct stochastic events. We have focused our analysis on young, active stars that do not display rotationally modulated light curves and that can be considered as single X-ray sources. Some stars in the sample are detected or known binary systems, in which only o ...
... as these stars often show several distinct stochastic events. We have focused our analysis on young, active stars that do not display rotationally modulated light curves and that can be considered as single X-ray sources. Some stars in the sample are detected or known binary systems, in which only o ...
Power Point - Stanford University
... extends very close to the hole, and the hole has spin in the direction of the rotation of the accretion disk. The right most line has no break point (Dc2 = 0.8). Thus it is not likely that we have yet seen the inner edge of the disk, thought our best fit suggests the possibility. Systematic errors a ...
... extends very close to the hole, and the hole has spin in the direction of the rotation of the accretion disk. The right most line has no break point (Dc2 = 0.8). Thus it is not likely that we have yet seen the inner edge of the disk, thought our best fit suggests the possibility. Systematic errors a ...
Massive close binaries, observational characteristics - UvA-DARE
... Figure 1 depicts the subsequent evolutionary stages through which a massive close binary system with a not too small initial mass ratio (q = M2/M1 >_0.4) is, theoretically, expected to pass (see for example Van den Heuvel 1974, 1978, 1983 and 1993 and references therein). For such systems the first ...
... Figure 1 depicts the subsequent evolutionary stages through which a massive close binary system with a not too small initial mass ratio (q = M2/M1 >_0.4) is, theoretically, expected to pass (see for example Van den Heuvel 1974, 1978, 1983 and 1993 and references therein). For such systems the first ...
JC Beamín1,2, RA Mendez3,2, RL Smart4, R. Jara3, R
... eighteen previously known high proper motion sources, including precise parallaxes for these sources for the first time. In this pioneer study we show the capability of the VVV project to measure high precision trigonometric parallaxes for very low mass stars (VLMS) up to distances of ~400 pc reachi ...
... eighteen previously known high proper motion sources, including precise parallaxes for these sources for the first time. In this pioneer study we show the capability of the VVV project to measure high precision trigonometric parallaxes for very low mass stars (VLMS) up to distances of ~400 pc reachi ...
IXO as an observatory in the large telescopes era
... the very phenomena where black holes grow by mass accretion, we need to uncover all populations of AGN over a broad range of redshifts, luminosities, and obscuration, to understand the whole growth history of supermassive black holes and their relation to galaxy formation. Theories suggest that a si ...
... the very phenomena where black holes grow by mass accretion, we need to uncover all populations of AGN over a broad range of redshifts, luminosities, and obscuration, to understand the whole growth history of supermassive black holes and their relation to galaxy formation. Theories suggest that a si ...
Radio observations of the 13hXMM–Newton/ROSAT Deep X
... and references therein). Our field has a handful of sources of flux density 10 mJy within, or close to the edge of, its primary beam and so is quite satisfactory for self-calibration, so here we include all the sources in our field, including source 1. To obtain an input model on which to self-cali ...
... and references therein). Our field has a handful of sources of flux density 10 mJy within, or close to the edge of, its primary beam and so is quite satisfactory for self-calibration, so here we include all the sources in our field, including source 1. To obtain an input model on which to self-cali ...
Spacecraft Navigation Using X-Ray Pulsars
... and with their faint emissions, radio-based systems would require large antennas (on the order of 25 m in diameter or larger) to detect sources, which would be impractical for most spacecraft. Also, neighboring celestial objects including the sun, moon, Jupiter, and close stars, as well as distance ...
... and with their faint emissions, radio-based systems would require large antennas (on the order of 25 m in diameter or larger) to detect sources, which would be impractical for most spacecraft. Also, neighboring celestial objects including the sun, moon, Jupiter, and close stars, as well as distance ...
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.