3 edition of Small-scale spatial fluctuations in the soft X-ray background found in the catalog.
Small-scale spatial fluctuations in the soft X-ray background
by National Aeronautics and Space Administration, Goddard Space Flight Center, Available from NASA Center for AeroSpace Information in Greenbelt, Md, Hanover, MD
Written in English
|Other titles||Small scale spatial fluctuations in the soft X-ray background|
|Statement||Kip D. Kuntz.|
|Series||[NASA technical memorandum] -- NASA/TM-2001-209981, NASA technical memorandum -- 209981.|
|Contributions||Goddard Space Flight Center.|
|The Physical Object|
Whistler modes are excited in the solar wind plasma when the characteristic plasma fluctuations propagate along a mean or background magnetic field with frequency ω > ω ci and the length-scales are c/ω pi Cited by: A small soft X-ray bright point appears during the impulsive phase of a flare (Shibata et al., ), about a few 10 4 km away from a soft X-ray loop. It is suggested that this bright point corresponds to one of the footpoints of an erupting flux rope forming a Cited by:
Right: Yohkoh image of soft X-ray loop and hard X-ray footpoint and loop top emission. Figure 3. A laboratory spontaneous magnetic reconnection event in the Massachusetts Institute of Technology VTF [ 28 ], depicted by measured contours of the plasma density, floating potential, current density, and the reconnection : Jill Dahlburg, William Amatucci, Michael Brown, Vincent Chan, James Chen, Christopher Cothran, Damie. Making use of the large number of X-ray sources, we update the "classic locus" of active galactic nuclei (AGNs) defined 20years ago in soft X-ray surveys and define a new locus containing 90% of the AGNs in the survey with full-band luminosity >10 42ergs
The efficiency of gratings for soft X-ray optics was discussed in Attwood et al. (). One characteristic feature was the low overall efficiency of this type of set-up at the X-ray energies discussed here: there was a 10% efficiency of the gratings and another order of magnitude was lost in optics by: The Wide-Field X-ray Telescope6 would provide an analog to SDSS in the X-ray band, detecting > X-ray AGN over >10, deg2 in the energy range keV (possibly extending to 6 keV). Further, the enormous sensitivity of the International X-ray Observatory7 would allow us to study in detail the spectra of large numbers of faint AGN.
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Title: Small-scale Spatial Fluctuations In The Soft X-ray Background Format: Paperback Product dimensions: pages, X X in Shipping dimensions: pages, X X in Published: Ma Publisher: BiblioScholar Language: English. Small-scale spatial fluctuations in the soft x-ray background (OCoLC) Microfiche version: Kuntz, Kip D.
Small-scale spatial fluctuations in the soft X-ray background (OCoLC) Material Type: Document, Thesis/dissertation, Government publication, National government publication, Internet resource: Document Type: Internet Resource.
Small-scale spatial fluctuations in the soft x-ray background (OCoLC) Online version: Kuntz, Kip D. Small-scale spatial fluctuations in the soft x-ray background (OCoLC) Material Type: Government publication, National government publication, Internet resource: Document Type: Book, Internet Resource: All Authors / Contributors.
We have studied the fluctuations of the soft ( keV) X-ray background intensity for ~10 arcmin and ~2 arcmin beam sizes, using 80 high galactic latitude medium-deep images from the ROSAT. Large Scale Fluctuations in the X-Ray Background Marie T reyer 1, Caleb Scharf 2, Ofer Lahav 3, Keith Jahod a 4, Elihu Boldt 4, Tsvi Piran 5 1 Astrophysik alisches Institut Potsdam, An der.
Solar and Space Physics: Space Science in the Twenty-First Century Past attempts have been frustrated by the low efficiency of soft x-ray polarimeters and especially by a complete lack of (and temperatures) thus far observed.
The dynamics of flares is linked to their small-scale spatial structure. SMM data have shown that lines such as. The arrival of pulsed X-rays from the Vulcan X-ray laser led to our development of a laser X-ray microscope. Again there was a clear potential advantage, for greatly reduced radiation damage from the very short X-ray pulse.
It was a triumph when, with our experimental X-ray laser microscope, the first image was recorded in a single laser : Ronald E. Burge. field fluctuations along the background magnetic field direction being used as inputs in addition to the traditional vector components of the magnetic field.
This analysis is performed on two streams of solar wind, one which can be classed as a slow stream, and one which can be classed as a fast streamFile Size: KB. Optical System for Diffraction-Limited Focusing of Soft X-Rays. The ALS developmental beamline and its endstation were configured for development of in situ metrology techniques.
12, 14, 15 The endstation chamber was designed to isolate the internal optical elements from the outside environment, in order to reduce the effects of vibrations and thermal by: The most important characteristics of the ideal microscope are summarized in Fig. “spatial resolution” at the left in the figure determines the 2D or 3D spatial discrimination level of the evolution of synchrotron X-ray imaging methods has achieved chemical imaging with a spatial resolution of 10 nm or better, close to the supramolecular interaction level of Cited by: Phase-contrast imaging using X-ray sources with high spatial coherence is an emerging tool in biology and material science.
Much of this research is Author: Bo Guo, Xiaohui Zhang, Jie Zhang, Jianfei Hua, Chih-Hao Pai, Chaojie Zhang, Hsu-Hsin Chu, Warren Mor. The X-ray background as a probe of density fluctuations at high redshift A&ASCB: Small-scale fluctuations and angular correlations of the X-ray background in the HEAO 1 A-2 energy band - Constraints on clustering of X-ray sources HEAO-1 LED maps of the Eridanus soft X-ray enhancement.
BAAS S: LIGO's discovery of a gravitational wave from two merging black holes (BHs) of similar masses rekindled suggestions that primordial BHs (PBHs) make up the dark matter (DM). If so, PBHs would add a Poissonian isocurvature density fluctuation component to the inflation-produced adiabatic density.
These fields consists of the smooth background fields, which can be modeled by the MHD equations governing the expansion of the solar wind, and of the small-scale fluctuations (waves or turbulence) that scatter the particles in pitch angle and act as agents enabling their acceleration at IP shock by: 6.
X-ray imaging spectrometers for Astro-E: ground calibration in the soft x-ray range. Kiyoshi Hayashida, Observed on-orbit background of the ACIS instrument on the Chandra X-ray Observatory. Paul P. Plucinsky, Shanil N. Virani. Proc. SPIEX-Ray Optics, Instruments, and Missions III, pg (18 July ); doi: / The U.S.
Department of Energy's Office of Scientific and Technical Information. Report of the Panel on Solar and Heliospheric Physics.
To grasp immediately the nature of the field of solar and heliospheric physics, one need only look at the striking image of the solar eclipse shown in Figure The solar atmosphere extends outward from the Sun’s surface, apparently without end.
Cambridge Core - Astrophysics - The Cosmic Century - by Malcolm S. Longair. Stanford Libraries' official online search tool for books, media, journals, databases, government documents and more. Fundamental parameter methods give the best results when a full X-ray spectrum is calculated, rather than just the characteristic X-ray lines of interest; this uses physical theory to calculate the spectrum background, so can give improved sensitivity for trace elements whose characteristic X-ray lines might be hidden in a high background, or Cited by: 8.
UNESCO – EOLSS SAMPLE CHAPTERS ASTRONOMY AND ASTROPHYSICS - “Let there be Light”: The Emergence of Structure Out of the Dark Ages in the Early Universe - Abraham Loeb ©Encyclopedia of Life Support Systems (EOLSS) of (1)+z in linear dimension since the galaxy emitted the observed light, and cosmologists can calculate the corresponding distance and cosmic age for the source.X-ray Scattering.
Soft X-Ray Scattering. Soft X-ray scattering is a photon-in, photon-out technique. The sample is illuminated with monochromatic soft X-rays, and the scattered photons are detected over a small angular range, in either the elastic or the inelastic mode.The source-subtracted CIB ﬂuctuations at and m appear strongly coherent with soft ( keV) unresolved cosmic X-ray background (CXB) [27, 95, 28, 86], which cannot be accounted for by the remaining known populations .
The CIB signal thus must arise in populations having a much higher fraction of BHs than known sources.