X-ray emission - translation to αραβικά
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  1. Λεξικά
  2. Αγγλο-αραβικό λεξικό
  3. X-ray emission

X-ray emission - translation to αραβικά

NON-DESTRUCTIVE ELEMENTAL ANALYSIS TECHNIQUE
Proton-induced x-ray emission; Particle induced X-ray emission; MicroPIXE; PIXE; Proton Induced X-ray Emission; Particle-induced X-ray Emission; Particle-Induced X-ray Emission

X-ray emission         
  • [[XMM-Newton]] spectrum from superheated iron atoms at the inner edge of the accretion disk orbiting the neutron star in Serpens X-1. The line is usually a symmetrical peak, but it exhibits the classic features of distortion due to relativistic effects. The extremely fast motion of the iron-rich gas causes the line to spread out. The entire line has been shifted to longer wavelengths (left, red) because of the neutron star's powerful gravity. The line is brighter toward shorter wavelengths (right, blue) because Einstein's special theory of relativity predicts that a high-speed source beamed toward Earth will appear brighter than the same source moving away from Earth.
  • Chandra]] images show PSR J1846-0258 in Kes 75 in October 2000 (left) and June 2006 (right). The pulsar brightened in X-rays after giving off powerful outbursts earlier in 2006.
  • Chandra]] image shows the supernova Kes 75 with the young, normal pulsar, neutron star PSR J1846-0258 in the center of the blue area at the top.
  • A [[near-infrared]] image of NGC 4151.
  • Two supermassive black holes spiraling towards merger near the center of [[NGC 1128]], some 25,000 light years away from each other.
  • Dec]] −52° 12' 21". Observation date: 30 August 1999. Instrument: ACIS. Aka: Cl 1409+524
  • A view of 4C 71.07 from observations by the Burst and Transient Source Experiment. This helped convince scientists that they were studying data from the quasar and not some other source in the neighborhood.
  • Chandra X-ray Observatory image of the galaxy cluster [[Abell 2142]].
  • Chandra image of two galaxies (Arp 270) in the early stage of a merger in the constellation [[Leo Minor]]. In the image, red represents low, green intermediate, and blue high-energy (temperature) X-rays. Image is 4 arcmin on a side. RA 10h 49 m 52.5s Dec +32° 59' 6". Observation date: 28 April 2001. Instrument: ACIS.
  • X-ray photo by [[Chandra X-ray Observatory]] of the [[Bullet Cluster]]. Exposure time was 140 hours. The scale is shown in mega[[parsec]]s. [[Redshift]] (''z'') = 0.3, meaning its light has wavelengths stretched by a factor of 1.3.
  • Dec]] −33° 42' 58.80" in Sculptor. Color code: Ultraviolet (blue), Optical (green), X-ray (purple), Infrared (red).
  • Cassiopeia A: a false color image composited of data from three sources. Red is infrared data from the [[Spitzer Space Telescope]], orange is visible data from the [[Hubble Space Telescope]], and blue and green are data from the [[Chandra X-ray Observatory]].
  • Dec]] +41° 30' 37.00" in [[Perseus]]. Observation dates: 13 pointings between 8 August 2002 and 20 October 2004. Color code: Energy (Red 0.3–1.2 keV, Green 1.2-2 keV, Blue 2–7 keV). Instrument: ACIS.
  • This shows a [[ROSAT]] false-color image in X-rays between 500 eV and 1.1 keV of the Chamaeleon I dark cloud. The contours are 100 μm emission from dust measured by the IRAS satellite.
  • Chandra observation of TWA 5B.
  • Chandra image of [[Cygnus X-1]], which was the first strong black hole candidate to be discovered.
  • Swift]] imaged it on 28 January 2009. This image merges data acquired by Swift's Ultraviolet/Optical Telescope (blue and green) and X-Ray Telescope (red). At the time of the observation, the comet was 99.5 million miles from Earth and 115.3 million miles from the Sun.
  • ly]] across in infrared light, as seen by the [[Spitzer Space Telescope]]. The magnetar itself is not visible at this wavelength, but it has been seen in X-ray light.
  • Classified as a [[peculiar star]], [[Eta Carinae]] exhibits a superstar at its center as seen in this image from [[Chandra]]. The new X-ray observation shows three distinct structures: an outer, horseshoe-shaped ring about 2 light years in diameter, a hot inner core about 3 light-months in diameter, and a hot central source less than 1 light-month in diameter which may contain the superstar that drives the whole show. The outer ring provides evidence of another large explosion that occurred over 1,000 years ago.
  • abbr=on}}. Observation dates: 10 pointings between 16 December 2003 – 13 April 2004. Instrument: HRC.
  • Polar]] satellite. The area of brightest X-ray emission is red. Such X-rays are not dangerous because they are absorbed by lower parts of the Earth's [[atmosphere]].
  • This light curve of Her X-1 shows long term and medium term variability. Each pair of vertical lines delineate the eclipse of the compact object behind its companion star. In this case, the companion is a 2 Solar-mass star with a radius of nearly four times that of the Sun. This eclipse shows us the orbital period of the system, 1.7 days.
  • Hydra]]. Observation date: 30 October 1999. Instrument: ACIS.
  • Jupiter shows intense X-ray emission associated with auroras in its polar regions (Chandra observatory X-ray image on the left). The accompanying schematic illustrates how Jupiter's unusually frequent and spectacular auroral activity is produced. Jupiter's strong, rapidly rotating magnetic field (light blue lines) generates strong electric fields in the space around the planet. Charged particles (white dots), trapped in Jupiter's magnetic field, are continually being accelerated (gold particles) down into the atmosphere above the polar regions, so auroras are almost always active on Jupiter. Observation period: 17 hrs, 24–26 February 2003.
  • Chandra mosaic of the X-ray sources in the [[Lockman Hole]]. Color code: Energy (red 0.4-2keV, green 2-8keV, blue 4-8keV). Image is about 50 arcmin per side.
  • Chandra image of LP 944-20 before flare and during flare.
  • Andromeda]]'s galactic center appears to harbor an X-ray source characteristic of a black hole of a million or more solar masses. Seen above, the false-color X-ray picture shows a number of X-ray sources, likely X-ray binary stars, within Andromeda's central region as yellowish dots. The blue source located right at the galaxy's center is coincident with the position of the suspected massive black hole. While the X-rays are produced as material falls into the black hole and heats up, estimates from the X-ray data show Andromeda's central source to be very cold – only about million degrees, compared to the tens of millions of degrees indicated for Andromeda's X-ray binaries.
  • Chandra]] image of M 82.
  • lightspeed]].
  • Dec]] +74° 14' 51.00" in [[Camelopardus]]. Observation date: 30 November 2003.
  • Map of the column density of Galactic neutral hydrogen in the same projection as the 0.25 keV SXRB. Note the general negative correlation between the 0.25 keV diffuse X-ray background and the neutral hydrogen column density shown here.
  • Orion]]. Soft X-rays are emitted by hot gas (T ~ 2–3 MK) in the interior of the superbubble. This bright object forms the background for the "shadow" of a filament of gas and dust. The filament is shown by the overlaid contours, which represent 100 micrometre emission from dust at a temperature of about 30 K as measured by [[IRAS]]. Here the filament absorbs soft X-rays between 100 and 300 eV, indicating that the hot gas is located behind the filament. This filament may be part of a shell of neutral gas that surrounds the hot bubble. Its interior is energized by UV light and stellar winds from hot stars in the Orion OB1 association. These stars energize a superbubble about 1200 lys across which is observed in the optical (Hα) and X-ray portions of the spectrum.
  • ultraviolet]] light (released 5 January 2016).
  • ULX ray source]]</div>
  • The Chandra X-ray image is of the quasar PKS 1127-145, a highly luminous source of X-rays and visible light about 10&nbsp;billion light years from Earth. An enormous X-ray jet extends at least a million light years from the quasar. Image is 60 arcsec on a side. RA 11h 30&nbsp;m 7.10s Dec −14° 49' 27" in Crater. Observation date: 28 May 2000. Instrument: ACIS.
  • This Chandra X-ray image of Radio Galaxy Pictor A shows a spectacular jet emanating from the center of the galaxy (left) and extends across 360 thousand lyr toward a brilliant hot spot. Image is 4.2 arcmin across. RA 05h 19&nbsp;m 49.70s Dec −45° 46' 45" in Pictor. Instrument: ACIS.
  • Dec]] −42° 41' 41.40" in Puppis. Observation date: 4 September 2005. Color code: Energy (Red 0.4–0.7 keV; Green 0.7–1.2 keV; Blue 1.2–10 keV). Instrument: ACIS.
  • In visible light, 4C 71.07 is less than impressive, just a distant speck of light. It is in radio and in X-rays – and now, gamma rays – that this object really shines. 4C 71.07 is its designation in the Fourth Cambridge Survey of radio sources. Its redshift of z=2.17, puts it about 11&nbsp;billion years away in a 12 to 15-billion year-old universe (using z=1 as 5&nbsp;billion light years).
  • Orion]]. On the left is Orion as seen in X-rays only. Betelgeuse is easily seen above the three stars of Orion's belt on the right. The X-ray colors represent the temperature of the X-ray emission from each star: hot stars are blue-white and cooler stars are yellow-red. The brightest object in the optical image is the full moon, which is also in the X-ray image. The X-ray image was actually obtained by the [[ROSAT]] satellite during the All-Sky Survey phase in 1990–1991.
  • Supernova 2005ke, which was detected in 2005, is a Type Ia supernova, an important "standard candle" explosion used by astronomers to measure distances in the universe. Shown here is the event in optical, ultraviolet and X-ray wavelengths. This is the first X-ray image of a Type Ia, and it has provided observational evidence that Type Ia are the explosion of a white dwarf orbiting a red giant star.
  • Chandra X-ray (left) and Hubble optical (right) images of Saturn on 14 April 2003. Observation period: 20 hrs, 14–15 April 2003. Color code: red (0.4 – 0.6 keV), green (0.6 – 0.8 keV), blue (0.8 – 1.0 keV).
  • SNR]] Sagittarius A East, the spiral structure Sagittarius A West, and a very bright compact radio source at the center of the spiral, [[Sagittarius A*]].
  • [[Stephan's Quintet]], a compact group of galaxies discovered about 130 years ago and located about 280 million light years from Earth, provides a rare opportunity to observe a galaxy group in the process of evolving from an X-ray faint system dominated by spiral galaxies to a more developed system dominated by elliptical galaxies and bright X-ray emission. Being able to witness the dramatic effect of collisions in causing this evolution is important for increasing our understanding of the origins of the hot, X-ray bright halos of gas in groups of galaxies.
  • The corona of the Sun as seen in the X-ray region of the [[electromagnetic spectrum]] on 8 May 1992 by the soft X-ray telescope on board the [[Yohkoh]] solar observatory spacecraft.
  • This is a false-color, 3-layer composite from the [[TRACE]] observatory: the blue, green, and red channels show the 17.1 nm, 19.5 nm, and 28.4 nm, respectively. These TRACE filters are most sensitive to emission from 1, 1.5, and 2 million degree plasma, thus showing the entire corona and detail of coronal loops in the lower solar atmosphere.
  • remnant]] as seen by the [[Chandra X-ray Observatory]]
ASTRONOMICAL OBJECT EMITTING X-RAYS
X-ray astrophysical sources; Astronomical X-ray source; Celestial X-ray source; Astronomical X-ray sources; Diffuse X-ray background; TWA 5B (Star); X-ray emission
انبعاث الاشعة السينية
x ray crystallography         
  • Model of the arrangement of water molecules in ice, revealing the [[hydrogen bond]]s (1) that hold the solid together.
  • The incoming beam (coming from upper left) causes each scatterer to re-radiate a small portion of its intensity as a spherical wave. If scatterers are arranged symmetrically with a separation ''d'', these spherical waves will be in sync (add constructively) only in directions where their path-length difference 2''d'' sin θ equals an integer multiple of the [[wavelength]] λ. In that case, part of the incoming beam is deflected by an angle 2θ, producing a ''reflection'' spot in the [[diffraction pattern]].
  • Three methods of preparing crystals, A: Hanging drop. B: Sitting drop. C: Microdialysis
  • tetrahedrally]] and held together by single [[covalent bond]]s, making it strong in all directions. By contrast, graphite is composed of stacked sheets. Within the sheet, the bonding is covalent and has hexagonal symmetry, but there are no covalent bonds between the sheets, making graphite easy to cleave into flakes.
  • access-date=2018-11-28}}</ref> The electron density is obtained from experimental data, and the ligand is modeled into this electron density.
  • Structure of a protein alpha helix, with stick-figures for the covalent bonding within electron density for the crystal structure at ultra-high-resolution (0.91&nbsp;Å). The density contours are in gray, the helix backbone in white, sidechains in cyan, O atoms in red, N atoms in blue, and hydrogen bonds as green dotted lines.<ref>From PDB file 2NRL, residues 17–32.</ref>
  • Animation showing the five motions possible with a four-circle kappa goniometer. The rotations about each of the four angles φ, κ, ω and 2θ leave the crystal within the X-ray beam, but change the crystal orientation. The detector (red box) can be slid closer or further away from the crystal, allowing higher resolution data to be taken (if closer) or better discernment of the Bragg peaks (if further away).
  • backbone]] from its N-terminus to its C-terminus.
  • Rocknest]]", October 17, 2012).<ref name="NASA-20121030" />
  • A protein crystal seen under a [[microscope]]. Crystals used in X-ray crystallography may be smaller than a millimeter across.
  • An X-ray diffraction pattern of a crystallized enzyme. The pattern of spots (''reflections'') and the relative strength of each spot (''intensities'') can be used to determine the structure of the enzyme.
  • Workflow for solving the structure of a molecule by X-ray crystallography.
TECHNIQUE USED FOR DETERMINING THE ATOMIC OR MOLECULAR STRUCTURE OF A CRYSTAL, IN WHICH THE ORDERED ATOMS CAUSE A BEAM OF INCIDENT X-RAYS TO DIFFRACT INTO SPECIFIC DIRECTIONS
X-ray structure; X-Ray Crystallography; X-Ray Diffraction Pattern; X ray diffraction; X-ray diffraction analysis; Crystallography, x-ray; Protein Crystallography; Protein crystallography; Xray crystallography; Xray Crystallography; X-ray Crystallography; X-ray crystalography; Crystallographic resolution; Laue diffraction; X-ray diffraction; History of X-ray crystallography; X ray crystallography; X-ray single-crystal analysis; X-ray crystal structure; Single-crystal X-ray crystallography; X-ray crystallographer; Laue method; X-ray diffraction crystallography; Single-crystal X-ray diffraction; X-ray structural analysis
‎ مَبْحَثُ تَصْويرِ البِلَّوراتِ بالأَشِعَّةِ السِّينِيَّة‎
x-ray diffraction         
  • Spectrum of various inelastic scattering processes that can be probed with inelastic X-ray scattering (IXS).
FAMILY OF NON-DESTRUCTIVE ANALYTICAL TECHNIQUES
X-ray scattering; X-Ray Diffraction; Resonant anomalous X-ray scattering; X-ray diffuse scattering; X-Ray diffraction; X-ray Diffraction; Inelastic X-ray scattering
انْعِراجُ الأشِعَّةِ السينِيَّة

Ορισμός

X-ray crystallography
¦ noun the study of crystals and their structure by means of the diffraction of X-rays by the regularly spaced atoms of crystalline materials.
Εμφάνιση περισσότερων ορισμών

Βικιπαίδεια

Particle-induced X-ray emission

Particle-induced X-ray emission or proton-induced X-ray emission (PIXE) is a technique used for determining the elemental composition of a material or a sample. When a material is exposed to an ion beam, atomic interactions occur that give off EM radiation of wavelengths in the x-ray part of the electromagnetic spectrum specific to an element. PIXE is a powerful yet non-destructive elemental analysis technique now used routinely by geologists, archaeologists, art conservators and others to help answer questions of provenance, dating and authenticity.

The technique was first proposed in 1970 by Sven Johansson of Lund University, Sweden, and developed over the next few years with his colleagues Roland Akselsson and Thomas B Johansson.

Recent extensions of PIXE using tightly focused beams (down to 1 μm) gives the additional capability of microscopic analysis. This technique, called microPIXE, can be used to determine the distribution of trace elements in a wide range of samples. A related technique, particle-induced gamma-ray emission (PIGE) can be used to detect some light elements.

https://en.wikipedia.org/wiki/Particle-induced X-ray emission
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