A search for rapidly modulated emission in bright x-ray sources using the HEAO A-1 data base final report to National Aeronautics and Space Administration for NASA grant NAG8-490

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Published by National Aeronautics and Space Administration, National Technical Information Service, distributor in [Washington, D.C, Springfield, Va .

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SeriesNASA contractor report -- NASA CR-180148
ContributionsUnited States. National Aeronautics and Space Administration
The Physical Object
Pagination1 v
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Open LibraryOL14986004M

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A search for rapidly modulated emission in bright x-ray sources using the HEAO A-1 data base: final report to National Aeronautics and Space Administration for NASA grant NAG NATIONAL AERONAUTICS AND SPACE ADMINISTRATION for NASA Grant NAG "A Search for Rapidly Modulated Emission in Bright X-Ray Sources Using the HEAO A-1 Data Base" c William M.

Fairbank Professor of Physics Principal Investigator (SASA-CR) A SEAkiCE ECE fiAFICLY NB 7- 1 75 93 FlOlIULATED EMISSlL6 IN ERIGHT 1-EAY SOUBCES. A search for rapidly modulated emission in bright X-ray sources using the HEAO A-1 data base First Author: Fairbank, William M.

Final Report Stanford Univ., CA. Dept. of Physics. A search was performed in the HEAO A-1 Data Base (located at the Naval Research Laboratory in Washington, D.C.) for evidence of rapidly-rotating neutron stars that could be sources of coherent gravitational radiation. A new data analysis algorithm, which was developed, is : William M.

Fairbank. With the soft X-ray detector (∼– keV) aboard the Astronomical Netherlands Satellite (ANS) we have searched for X-ray emission from hot star coronae and peculiar stars. On Sirius (α CMa) and Capella (α Aur) X-ray emission has been measured at 6σ and 5σ level, respectively, above by: 6.

The total X-ray emission in 4π-geometry is J, which corresponds to the system efficiency of about %. The X-ray emission is found dominantly as a result of the interaction of energetic electrons in the current sheath with the anode tip.

Images recorded by the pinhole camera confirm the emission of X-rays from the tip of the by: X-ray sources with greater than keV photon energy and sufficient brilliance to perform X-ray crystallography are based on relativisitic electron bunches from synchrotrons or linear accelerators.

The relativistic motion confines the angle of emission to a narrow cone dramatically increasing source. Abstract. We report on thefirst firm detection of pulsed-ray emission from PSR B in the MeV en-ergy range in CGRO COMPTEL data collected over more than 6 years.

The modulation significance in the MeV pulse-phase distribution is 5: 4 and the lightcurve is similar to thelightcurves found earlier between and purpose: is to remove low energy X-rays in primary beam. Primary xray beam quality is increased, quantity is decreased. X-ray quality (energy level or penetrability of the X-ray beam) the penetrability of the beam is the X-ray quality.

as the X-ray energy level is. The amplitude of the bremsstrahlung x-ray emission spectrum: Has maximum value at energy approximaely 1/3 of the kVp If an x-ray emission spectrum represented operation at 85 kVp with a. A search for rapidly modulated emission in bright X-ray sources using the HEAO A-1 data base ApJ S: 02/ The Ophiuchus cluster - A bright X-ray cluster of galaxies at low galactic latitude NaturS: 04/ A bright, relatively inexpensive X-ray source (as compared to a synchrotron emitter) for A search for rapidly modulated emission in bright x-ray sources using the HEAO A-1 data base book, technological, and medical purposes.

A stack of foils of high density and moderate atomic number are bombarded with high-energy electrons of 25 to MeV to produce a flux of transition X-rays of 2 keV Cited by: A set of experiments were performed on the National Ignition Facility (NIF) to develop and optimize a bright, 17 keV x-ray backlighter probe using laser-irradiated Nb foils.

1 FRII SOURCES AT: X-RAY PROPERTIES OF THE CORE AND EXTENDED EMISSION E. Belsole1, J.H. Croston2,3, D.M. Worrall1, and M. Hardcastle3 1H.H. Wills Phyisics Laboratory, Uni versity of Bristol, Tyndall A enue, Bristol BS8 1TL, UK 2Service d’Astrophysique, bat CEA- Saclay, L’orme des Merisiers, Gif sur Yvette Cedex, France 3School of Physics, Astronomy and Mathematics.

The HEAO 1 A2 full sky, 2 È 10 keV X-ray map was searched for emission correlated with the plane of the Local Supercluster of galaxies. After removing strong point and moderately extended sources. Soft X-ray emission from the X-ray source Per X-1 was observed in the –2 keV energy interval from a rocket borne X-ray detector.

Spectral analysis of the data indicates that in the –2 keV band the X-ray emission from Per X-1 can be fitted either with a power law of slope-(±) or a thermal bremsstrahlung spectrum with akT value of ( − +) : P.

Agrawal, K. Long, G. Garmire. Impact Factor The Journal of X-Ray Science and Technology is an international journal designed for the diverse community (biomedical, industrial and academic) of users and developers of novel x-ray imaging purpose of the journal is to provide clear and full coverage of new developments and applications in the field.

A ray in the emission spectrum has a wavelength of x meters. Given that the speed of light is x m/s, what is the frequency of the ray. x HZ b. x HZ c. x HZ d. x HZ. High-resolution soft X-ray emission spectrograph at advanced light source.

Driven by such demand, we have developed a soft X-ray emission spectrograph based on variable line spacing (VLS) gratings to work in the soft X-ray and deep UV (the M edge of transition metals) regime. the dashed line is the theoretical value with 5° blazed Cited by: the overall improvement in data quality has lead to better standard source analysis [Bregeon, Charles & Wood ].

Preliminary LAT analysis Having identi ed a new Galactic transient consis-tent with a new classical nova, Nova Scowe pre-ceded to analyze the source behaviour with the new P7REP data using the standard likelihood analysis.

Hard X-ray/soft γ-ray Characteristics of the Persistent Emission from Magnetars – Results based on multi-year INTEGRAL, RXTE and XMM Newton observations – L.

Kuiper,1 P.R. den Hartog1 and W. Hermsen1,2 1 SRON, Netherlands Instituut for Space Research. The F1 flare is characterized by a preheating stage of the compact region (with a small emission measure) to a temperature of 2•10 7 K, followed by a cooling for min, accompanied by a continuous increase in the emission measure.

The temperature value of 2•10 7 K is comparable with the temperature in the flare maximum. Then, starting from UT, the main stage of the flare's Author: Mikhail I. Savchenko, Pavel V. Vatagin, Vadim P.

Lazutkov, Dmitriy V. Skorodumov, Igor V. Kudryavtse. High−Energy Emission from Bright Gamma–Ray Bursts using Fermi Elisabetta Bissaldi Vollständiger Abdruck der von der Fakultät für Physik der Technischen Universität München zur Erlangung des akademischen Grades eines Doktors der Naturwissenschaften genehmigten Dissertation.

Vorsitzender: Univ.–Prof. Ibarra Prüfer der. A ray in the emission spectrum has a wavelength of x meters. Given that the speed of light is x m/s, what is the frequency of the ray.

- X-ray observations of two VHE γ–rays sources connected to shell-type SNRs – Shows extended (PWN-like) sources – Cannot distinguish between central source vs shell-like scenario – Modelling suggests that GLAST will provide important constraints – But these examples also show how hard it is to associate counterparts to γ–ray File Size: KB.

Abstract: Apparently diffuse X-ray emission has been known to exist along the central quarter of the Galactic Plane since the beginning of the X-ray astronomy, which is referred to as the Galactic Ridge X-ray emission (GRXE). Recent deep X-ray observations have shown that numerous X-ray point sources account for a large fraction of the GRXE in the hard band ( keV).Cited by: The key component of the Argus system is the field emission x-ray source array.

The construction of the 25 x-ray pixels is identical. The CAD drawing of one pixel is shown in Fig. The central beams of all the 25 x-ray sources intersect at a 48 û coverage 2 û step D cm S-O: cm Detector Phantom X-ray source array cm D S-D: cmFile Size: 1MB.

GALAXIES, X-RAY EMISSION. Giuseppina Fabbiano. The study of the x-ray emission of normal galaxies is a very recent part of astronomy. This work has been made possible by the sensitive x-ray imaging observations of the Einstein (HEAO 2) satellite, launched by NASA in November Before then, with the exclusion of the bright x-ray sources associated with Seyfert nuclei, only four galaxies.

An international team of researchers has performed of extended X-ray emission in the radio source known as PKS − The study, published April 11 in a paper on the arXiv pre-print. (Students should use Figure to record information contained in Figure 8.A.) 1.

Based on your experience, is a dim bulb hotter or cooler than a bright bulb. cooler. How does the temperature affect the bulb’s intensity.

The brighter the bulb, the more intense the light is and the hotter the bulb is. Hot-spot identification for HIV-1 RT–rilpivirine (figures drawn using PyMOL; DeLano, ).(a) The RT–rilpivirine structure with p66 subdomains colored and labeled and the p51 subunit colored irine is depicted at the NNRTI-binding pocket.

(b) Results of an X-ray crystallographic fragment-screening campaign on RT–rilpivirine crystals not including 4-bromopyrazole (Bauman Cited by: The first line of the data file will contain the sample name which should be stored as a string object.

The second line will contain the anode (the elemental source of the x-ray) as a 2-character symbol which should also be stored as a string object.

You will need to use this symbol to determine the wavelength of the x-ray using the table below. The electron field emission characteristics of the multipixel cathode chip were studied using the prototype setup of the x-ray source designed for the micro-RT, as shown in inset (a) of Fig.

Fig Figure2 2 shows the typical emission current (I) versus applied voltage (V) of one individual pixel in the cathode chip. The threshold field is V∕μm, which, for the purposes of this Cited by: J.S. Clark et al.: Photometric observations of the radio bright B[e]/X-ray binary CI Cam 51 Table 1.

Summary of observations giving details of telescope and detector used, photometric bands observed in and dates of observations. also lower than archival data. Associated with the fact that in the VHE and X-ray lightcurves no significant variability is seen, the observations suggest a low state of emission of the source, similar to the one of 1ES, the most distant AGN discovered so far (Aharonian et al.

The material in the disc slowly loses its angular momentum and falls into the compact star. In neutron stars and white dwarfs, additional X-rays are generated when the material hits their surfaces. X-ray emission from black holes is variable, varying in luminosity in very short timescales.

The variation in luminosity can provide information about the size of the black hole. X-ray photoelectron spectroscopy (XPS) is a surface-sensitive quantitative spectroscopic technique that measures the elemental composition at the parts per thousand range, empirical formula, chemical state and electronic state of the elements that exist within a material.

XPS is a useful measurement technique because it not only shows what elements are within a film but also what other. @article{osti_, title = {X-ray emission spectroscopy. Parts 1 and 2}, author = {Valkovic, V}, abstractNote = {In part 1 of this article x-ray production by charged particle and x-ray excitation is described.

Theory and experiments on charged-particle-induced x- ray emission are summarized. Detection of x-rays by semiconductor and other detectors are discussed. X-RAY AND LYMAN-ALPHA EMISSION FROM THE SUN AS MEASURED FROM THE NRL SR-1 SATELLITE [R.W., et al Kreplin] on *FREE* shipping on qualifying : Kreplin, R.W., et al.

cline than during the hard state rise, at a given X-ray luminosity (NIR–X-ray hysteresis), which may be due to a more powerful jet on the decline (which also likely dominated the X-ray flux; Rus-sell et al. ), or changes in the jet efficiency and/or the disc viscosity.

In this paper we use the OIR data of XTE J– during itsCited by:. 2. U-shaped Cu anticathode for the X-ray generator X-ray generator overview Figs. 1 and 2 show, respectively, a schematic view and a photograph ofthe X-raygeneratorwiththeU-shapedrotating anticathode. The X-ray generator is comprised of three sections: electron gun, beam focus system and bending magnet.Researchers study extended X-ray emission in the PKS ?

radio source 17 Aprilby Tomasz Nowakowski PKS ? Difference map between the hard.NCTM & NSES Standards. Show me related lesson plans. X-ray Emission from Atoms Inside the Atom. An atom has a nucleus, which contains particles of positive charge () and particles of neutral charge ().Surrounding the nucleus of an atom are shells of electrons, which are small negatively charged shell has a specific energy associated with it.

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