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Ultraluminous

Ultraluminous Author Katherine Faw
ISBN-10 9780374716646
Release 2017-12-05
Pages 208
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Girlfriend. Prostitute. Addict. Terrorist? Who is K? The daring new novel from Katherine Faw, the brilliant author of Young God, is a scintillating story of money, sex, and power told in Faw’s viciously sharp prose. A high-end, girlfriend-experience prostitute has just returned to her native New York City after more than a decade abroad—in Dubai, with a man she recalls only as the Sheikh—but it’s unclear why exactly she’s come back. Did things go bad for her? Does she have scores to settle? Regardless, she has quickly made herself at home. She’s set up a rotation of clients—all of them in finance—each of whom has different delusions of how he is important to her. And she’s also met a man whom she doesn’t charge—a damaged former Army Ranger, back from Afghanistan. Her days are strangely orderly: A repetition of dinners, personal grooming, museum exhibitions, sex, Duane Reades (she likes the sushi), cosmology, sex, gallery shows, nightclubs, heroin, sex, and art films (which she finds soothing). She finds the pattern confirming, but does she really believe it’s sustainable? Or do the barely discernible rifts in her routine suggest that something else is percolating under the surface? Could she have fallen for one of her bankers? Or do those supposed rifts suggest a pattern within the pattern, a larger scheme she’s not showing us, a truth that won’t be revealed until we can see everything?



Ultraluminous X ray Sources

Ultraluminous X ray Sources Author Andrew Sutton
ISBN-10 OCLC:870422963
Release 2013
Pages
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Accretion Disk Spectra of the Ultra Luminous X Ray Sources in Nearby Spiral Galaxies and Galactic Superluminal Jet Sources

Accretion Disk Spectra of the Ultra Luminous X Ray Sources in Nearby Spiral Galaxies and Galactic Superluminal Jet Sources Author Taiji Mizuno
ISBN-10 OCLC:316495617
Release 2003
Pages 5
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Ultra-luminous Compact X-ray Sources (ULXs) in nearby spiral galaxies and Galactic superluminal jet sources share the common spectral characteristic that they have unusually high disk temperatures which cannot be explained in the framework of the standard optically thick accretion disk in the Schwarzschild metric. On the other hand, the standard accretion disk around the Kerr black hole might explain the observed high disk temperature, as the inner radius of the Kerr disk gets smaller and the disk temperature can be consequently higher. However, we point out that the observable Kerr disk spectra becomes significantly harder than Schwarzschild disk spectra only when the disk is highly inclined. This is because the emission from the innermost part of the accretion disk is Doppler-boosted for an edge-on Kerr disk, while hardly seen for a face-on disk. The Galactic superluminal jet sources are known to be highly inclined systems, thus their energy spectra may be explained with the standard Kerr disk with known black hole masses. For ULXs, on the other hand, the standard Kerr disk model seems implausible, since it is highly unlikely that their accretion disks are preferentially inclined, and, if edge-on Kerr disk model is applied, the black hole mass becomes unreasonably large (> 300 M{sub solar}). Instead, the slim disk (advection dominated optically thick disk) model is likely to explain the observed super-Eddington luminosities, hard energy spectra, and spectral variations of ULXs. We suggest that ULXs are accreting black holes with a few tens of solar mass, which is not unexpected from the standard stellar evolution scenario, and that their X-ray emission is from the slim disk shining at super-Eddington luminosities.



Ultra luminous x ray sources

Ultra luminous x ray sources Author Jifeng Liu
ISBN-10 UOM:39015062470383
Release 2005
Pages
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Ultraluminous X ray Sources and Their Environment

Ultraluminous X ray Sources and Their Environment Author Ciprian T. Berghea
ISBN-10 OCLC:528768398
Release 2009
Pages 338
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The Cold Universe

The Cold Universe Author Th MONTMERLE (Ed)
ISBN-10 2863321501
Release 1994
Pages 442
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The Physics of Ultra Luminous Infrared Galaxies

The Physics of Ultra Luminous Infrared Galaxies Author Hazel Marina Sopp
ISBN-10 OCLC:60113205
Release 1991
Pages
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Color magnitude Relation and Morphology of Ultraluminous Infrared Galaxies from Z 0 to Z 1

Color magnitude Relation and Morphology of Ultraluminous Infrared Galaxies from Z   0 to Z   1 Author Yuxi Chen
ISBN-10 OCLC:795819922
Release 2011
Pages 134
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Ultraluminous infrared galaxies (ULIRGs) are among the most powerful galaxies and play an important role in galaxy formation and evolution. In this dissertation, I present by far the most detailed and latest studies of ULIRGs both in the nearby universe and at epochs only half of today's universe's age, through their color-magnitude relation (CMR) and morphology. I studied the most luminous local ULIRGs in the SDSS, and found that local ULIRGs are optically luminous, on average 1 magnitude brighter than field galaxies, and they are as blue as the blue cloud in the color-magnitude diagram of galaxies. Only few ULIRGs appear in the green valley, the low density region between the red sequence and blue cloud, and none of which harbors an AGN. Therefore, we are not witnessing the AGN quenching of star formation, and the blue colors of ULIRGs is consistent with a working hypothesis in which the dust geometry is patchy and blue lights originate from unshielded stellar components, many of which are at large distances. We also imaged nine most luminous ULIRGs at z ~ 1 using HST in ACS/F814W and NICMOS2/F160W filters. The z ~ 1 ULIRGs, unlike the z ~ 0 ULIRGs, appear to be more concentrated in the green valley. The concentration of z ~ 1 ULIRGs in the green valley is possible due to the color selection in studying the CMR. Quantitative morphology measurements have been widely used in describing galaxy morphology and classifying galaxies, but their limitations have not been systematically studied. In this dissertation I present detailed studies of the limitations of non-parametric quantitative morphology measurements, the Gini coefficient (G) and M 20. Both z ~ 0 and z ~ 1 ULIRGs distribute heterogeneously in G - M20 space, which is unexpected from the proposed effectiveness of G -M 20 in selecting merging galaxies. I performed a series simulations, which shows that seen against higher background noise, G decreases and M20 increases systematically. Observationally G and M20 are also more sensitive to certain merging stages, consistent with the findings from other numerical simulations. As a conclusion, cautions must be made when applying the quantitative morphology measurements. There are strong color gradients across almost all z ~ 0 and z ~ 1 ULIRGs. Benefited from high spatial resolutions of HST, I developed a new technique to investigate the pixel-based color distribution and produced pixel-based color-magnitude diagrams (pCMDs) for the z ~ 1 ULIRGs. A unique feature in the pCMD, "horizontal blue shelf", has been discovered among all z ~ 1 ULIRGs, which is consistent with typical colors of today's disk, and can be modeled by young stellar populations with an age between 10 Myr and 500 Myr with moderate extinction.



On the Nature of Ultraluminous X Ray Sources Or What a Black Hole Should Look Like

On the Nature of Ultraluminous X Ray Sources  Or What a Black Hole Should Look Like Author
ISBN-10 OCLC:727345893
Release 2006
Pages 5
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We derive the luminosity-temperature relation for the accreting black holes (BHs). At the accretion rates below the critical Eddington, the BHs are described by the standard Shakura-Sunyaev model resulting in the L (infinity) T4 (infinity) M relation. At super-Eddington rates, {dot m} = {dot M}/{dot M}{sub Edd}” 1, a strong outflow forms within the spherization radius R{sub sp} (infinity) {dot M}. If the angular momentum of the outflowing matter is conserved and typical outflow velocities are of the order of Keplerian, the wind occupies 50-85 per cent of the sky as viewed from the BH, while the region around the rotation axis remains transparent. The bolometric luminosity in such a case is known to exceed the Eddington luminosity by a factor 1 + ln {dot m} and the observed luminosity is 2-7 times higher because of geometrical beaming. An edge-on observer sees only the soft emission from the extended envelope, with the photosphere radius exceeding R{sub sp} by orders of magnitude. The photosphere temperature follows the T{sub ph} (infinity) {dot M}−34 or {dot M}−1 relation depending on the velocity profile at R> R{sub sp} (constant velocity or a Keplerian profile). The resulting L-T{sub ph} dependence is consistent with that observed in the super-Eddington accreting BHs SS 433 and V4641 Sgr. A face-on observer has a direct view of the inner hot accretion disc which in stellar-mass BHs has temperature T{sub max} of a few keV. The effective temperature depends on radius as (infinity) R−12 (up to the spherization radius) and the emitted spectrum is a power-law F{sub E} (infinity) E−1 extending from (almost equal to) 3T{sub max} down to the temperature at the spherization radius T{sub sp} (almost equal to) {dot m}−12 keV. It continues further as a power-law F{sub E} (infinity) E13 to the photospheric temperature T{sub ph}. We associate T{sub max} with a few keV spectral components and T{sub sp} with the soft, 0.1-0.2 keV components observed in the ultraluminous X-ray sources (ULX). The strong outflows combined with the large intrinsic X-ray luminosity of the central BH explain naturally the presence of the photoionized nebulae around ULX. An excellent agreement between the model and the observational data on ULX strongly argues in favour of ULX being super-critically accreting, stellar-mass BHs similar to SS 433, but viewed along the symmetry axis.



Dynamics of Galaxies and Their Molecular Cloud Distributions

Dynamics of Galaxies and Their Molecular Cloud Distributions Author International Astronomical Union. Symposium
ISBN-10 0792310969
Release 1991-01-31
Pages 467
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Papers of the Paris meeting in June 1990 on Local Group Galaxies, molecules in early-type galaxies, observations of spiral structure in molecular clouds, a comparison with other gaseous components and IR emission, interacting galaxies and starbursts, gas and star dynamics, galaxy evolution, IRAS ult



High Energy Astrophysics

High Energy Astrophysics Author Walter H. G. Lewin
ISBN-10 NAP:12470
Release 1991-01-01
Pages 415
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During the past decade, the field of astrophysics has progressed at an impressive rate. This was reflected by the topics discussed at the workshop from which this book eminated. These topics include the inflationary universe; the large-scale structure of the universe; the diffuse X-ray background; gravitational lenses, quasars and active galactic nuclei; infrared galaxies; results from infrared astronomical satellites; supernova 1987A; millisecond radio pulsars; quasi-periodic oscillations in the X-ray flux of low-mass X-ray binaries; and gamma-ray bursts.



QSO Hosts and Their Environments

QSO Hosts and Their Environments Author Isabel Márquez
ISBN-10 0306466627
Release 2001-01-01
Pages 376
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Proceedings of an International workshop on QSO Hosts and their Environments, held January 10-12, 2001, in Granada, Spain



Astronomie Extragalactique Dans L infrarouge

Astronomie Extragalactique Dans L infrarouge Author Gary Allen Mamon
ISBN-10 2863322265
Release 1997-01-01
Pages 629
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Astronomie Extragalactique Dans L infrarouge has been writing in one form or another for most of life. You can find so many inspiration from Astronomie Extragalactique Dans L infrarouge also informative, and entertaining. Click DOWNLOAD or Read Online button to get full Astronomie Extragalactique Dans L infrarouge book for free.



The Central Regions of the Galaxy and Galaxies

The Central Regions of the Galaxy and Galaxies Author International Astronomical Union. Symposium
ISBN-10 079235060X
Release 1998-08-31
Pages 521
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Proceedings of the 184th Symposium of the International Astronomical Union, held in Tokyo, Japan, 18-22 August 1997



Black Holes IAU S238

Black Holes  IAU S238 Author Vladimir Karas
ISBN-10 0521863473
Release 2007-07-30
Pages 482
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IAU S238 report on the physics of black holes, by leading researchers in the field.



ISO Surveys of a Dusty Universe

ISO Surveys of a Dusty Universe Author D. Lemke
ISBN-10 9783540455530
Release 2008-01-11
Pages 434
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Many of the ISO observers who assembled for this workshop at Ringberg c- tle met for the third time in the Bavarian Alps. At two previous meetings in 1989 and 1990 surveys were only a minor topic. At that time we were excited by the discoveries of the IRAS survey mission and wanted to follow it up with pointed observations using an observatory telescope equipped with versatile instruments. With the rapid development of detector arrays and stimulated by ISO’s Observing Time Allocation Committee, however, surveys eventually became an issue for the upcoming mission. In a review paper on “Infrared S- veys - the Golden Age of Exploration” given at an IAU meeting in 1996, Chas Beichman already mentioned that there are ISO surveys. They were at the bottom of his hit list, while the winners were future space missions (Planck, SIRTF, etc. ) and ground-based surveys in preparation (Sloan, 2MASS, DE- NIS, etc. ). He organized his table according to the relative explorable volume, calculated from the solid angle covered on the sky and the maximum distance derived from the detection sensitivity. Clearly, with this ?gure of merit, ISO, as a pointed observatory, is rated low. Applying the classical de?nition of a survey, i. e. to search in as large a volume as possible for new or rare objects and/or study large numbers of objects of various classes in order to obtain statistical properties, ISO was indeed limited.



Galaxy Interactions at Low and High Redshift

Galaxy Interactions at Low and High Redshift Author International Astronomical Union. Symposium
ISBN-10 0792358325
Release 1999-09-30
Pages 519
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Proceedings of the 186th Symposium of the International Astronomical Union, held at Kyoto, Japan, 26-30 August 1997