「X-ray」の共起表現一覧(1語右で並び替え)4ページ目
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| radiation, but in 1962 he started researching | X-ray phenomena brought forth by electron bombardmen |
| e prisms are used in infrared spectroscopy, in | x-ray phosphors, and in scintillation counters. |
| 81, for his contribution to the development of | X-ray photoelectron spectroscopy. |
| electrons that are ejected by x-rays is called | x-ray photoelectron spectroscopy (XPS) or electron s |
| analysis (NCESS), which has a high-resolution | x-ray photoelectron spectroscopy machine to probe ne |
| s in the crystal, frequently measured by using | X-Ray Photoelectron Spectroscopy to compare the rati |
| In the CD's liner notes, the | X-ray photograph found on the cover is credited to " |
| used by a surgeon who would, with the help of | x-ray photographs, precisely remove the foreign obje |
| He pioneered the use of | x-ray photography in tuberculosis detection, and hel |
| To eliminate responses of the | X-ray photometer from Van Allen belt radiation (char |
| Unlike an | x-ray photon with a similar wavelength, which intera |
| e neutron has an additional advantage over the | x-ray photon in the study of condensed matter. |
| hether the ionization energy is provided by an | X-ray photon, an ultraviolet photon, EUV photon, or |
| ANS could measure | X-ray photons in the energy range 2 to 30 KeV, with |
| g, a common technique is to use a number of 2D | X-ray photos or MRI scans to "reconstruct" a 3D imag |
| He was appointed as Radium and | X-ray physicist to the Canadian National Research Co |
| cent and since 1988, he is a professor of soft | X-ray physics at Uppsala. |
| Normally, either | X-ray pictures are taken of the filter, or the filte |
| An all-ages and community-oriented club, the | X-Ray played a "heavyweight role in shaping Portland |
| The HRI | X-ray pointlike source location is ~4" south of Proc |
| X-ray pole figure analysis enables one to analyze an | |
| the presence of a late type star close to the | X-ray position favor the identification of the X-ray |
| Optical examination and | x-ray powder diffraction indicated the mineral to be |
| d and coworkers elucidated its structure using | X-ray powder diffractometry (XRPD) and the Rietveld |
| The | X-ray powder diffraction pattern is very distinctive |
| Microprobe analyses and | X-ray powder-diffraction studies indicate extensive |
| re spending five additional months at the Camp | X-Ray prison, where he claims to have been given tra |
| es are universally used as contrast agents for | X-ray procedures. |
| X-ray produced plasmas on the surrounding surfaces c | |
| xy, microwave radio jets, multi-million degree | X-ray producing gas and resultant radio source is kn |
| as improved measurements of the supernova, and | X-ray properties of galaxy clusters. |
| He is best known for his work studying the | X-ray properties of active galaxies, X-ray binaries, |
| TD-1A detectors: | X-ray proportional counter, MIMOSA, Utrecht Orbiting |
| uch as physiotherapy, occupational therapy and | x-ray provide essential support in the diagnosis and |
| Centaurus X-3 (4U 1118-60) is an | X-ray pulsar with a period of 4.84 seconds. |
| of GX 1+4, which was the first slowly rotating | X-ray pulsar found. |
| Long-term monitoring of | X-ray pulsar (e.g. |
| The Bursting Pulsar is the only known | X-ray pulsar that is also a Type II X-ray burster. |
| It was the first | X-ray pulsar to be discovered, and the third X-ray s |
| d his research group also discovered the first | X-ray pulsar with a rotation speed of four hundred r |
| ill capture material and temporarily become an | X-ray pulsar. |
| These energetic | X-ray pulsars are characterized by slow rotation per |
| ts for unknown reasons, so these are transient | X-ray pulsars that are observed only intermittently, |
| These accreting millisecond | X-ray pulsars are thought to be the evolutionary pro |
| Anomalous | X-ray Pulsars (AXPs) are now widely believed to be m |
| A total of thirteen accreting millisecond | X-ray pulsars have been discovered as of January 201 |
| Three of them are Intermittent millisecond | X-ray pulsars (HETE J1900.1-2455, |
| For still other types of | X-ray pulsars, the companion star is a Be star that |
| rage flux, which is often observed from binary | X-ray pulsars. |
| Detection of cyclotron features in 3 | X-ray pulsars: 4U1538-522, V0332+53, and Cep X-4. |
| revealed | X-ray pulsations at the 401 Hz neutron star spin fre |
| is about 283 seconds, and gives rise to strong | X-ray pulsations. |
| This instrument collected data on | X-ray radiation from diffuse sources in deep space. |
| n hope of discovering antimatter then in using | x-ray radiation for solid state physics and chemistr |
| ototype of a small group of stellar sources of | X-ray radiation that is about 10 times higher than e |
| Cosmic | X-ray radiation is absorbed by the Earth's atmospher |
| committee noted: "He is a world leader in the | X-ray radiation of compact objects and has formulate |
| fusion fuel in them is also imploded mainly by | X-ray radiation. |
| very of a radio pulsar 102 MHz while observing | X-ray radio source Geminga, |
| optical observation and must be studied in the | X-ray, radio, and infrared bands. |
| of the frequency of this line (usually in the | X-ray range for heavier elements), uses the same bas |
| conduct observations of galaxy clusters on the | X-ray range with the intent of finding data related |
| less energetic in the soft gamma-ray and hard | X-ray range, and repeated bursts came from the same |
| ography unit: The CBCT unit uses a cone-shaped | X-ray rather than a linear one to create three-dimen |
| tention more to his own record company, called | X-Ray Records/Rayvano Productions. |
| n this book, Niggli demonstrated that although | X-ray reflection conditions do not always uniquely d |
| Reflectivity range is the term used in | X-ray reflectometry and several other radar-related |
| radiation covering the terahertz (THz) to soft | X-ray regimes. |
| The | X-ray required a 2 hour exposure, but successfully d |
| a 45 cent stamp, along with fellow pioneers of | X-ray research Father Joseph Slattery and W.T. Filme |
| 1873 - April 27, 1954) was a pioneer in early | X-ray research, working under J. J. Thomson at the U |
| oor consists of two electron storage rings: an | X-Ray ring and a VUV (Vacuum Ultra Violet) Ring whic |
| e corresponding factor for coherent neutron or | X-ray scattering is the Debye-Waller factor; often, |
| y, analytical ultracentrifugation, Small angle | X-ray scattering (SAXS), and measurements of the dif |
| He developed the theory of | X-ray scattering by lattice vibrations of a crystal, |
| Anomalous | X-ray scattering AXRS or XRAS is a technique within |
| EM), atomic force microscopy (AFM), wide angle | X-ray scattering (WAXS), small incidence angle X-ray |
| ve-like nature of X-rays was confirmed through | X-ray scattering experiments on crystalline solids. |
| For example, | X-ray scattering and neutron scattering experiments |
| Resonant Inelastic | X-ray Scattering (RIXS) is an x-ray spectroscopy tec |
| ical and experimental nanophysics, synchrotron | x-ray scattering, supramolecular surface chemistry, |
| rogress in developing and refining the laws of | X-ray scattering, X-ray spectroscopy, the principles |
| During his graduate studies Bode was using | x-ray scattering. |
| c flow field flow fractionation or small-angle | X-ray scattering. |
| Hard | X-ray Sciences - Argonne is home to one of the world |
| , 30 parking bays, 72 immigration counters, 15 | X-ray screening areas, for less waiting times, duty- |
| x-rays or electron beam, making it useful for | x-ray screens and cathode ray tubes. |
| West Pacific LORAN-C Chain ( GRI 8930) and the | X-Ray Secondary of the East Asia LORAN-C chain ( GRI |
| Today Marcus Island LORAN-C transmitter is the | X-Ray secondary station of the North West Pacific LO |
| aminated with a scintillation screen to create | x-ray sensitive diodes. |
| were not equipped with bhangmeters (they used | X-ray sensors instead to detect an intense single pu |
| The Draco nebula (a soft | X-ray shadow) is outlined by contours and is blue-bl |
| ck Van Dyke Show episode titled "Ray Murdock's | X-Ray," which originally aired on January 23, 1963, |
| from one of them, even a small scan (possibly | x-ray) showed up with a metallic endoskeleton. |
| Camp | X-Ray, shown here under construction, was a temporar |
| ie Dixon Said" that appeared on his 1999 album | X-Ray Sierra. |
| soft X-rays by the much lower intensity of the | X-ray signal. |
| The angle between the two rings as measured by | X-ray single-crystal analysis is 78°. |
| WHITIA currently has pilot integrated digital | X-ray sites in South Africa and Guatemala at establi |
| mong the largest and brightest features in the | x-ray sky. |
| A soft | X-ray solar imaging telescope is on board the GOES-1 |
| The | X-ray source associated with Procyon A/B was observe |
| X-ray source 2A 0252+060 (1H 0253+058, XRS 02522+060 | |
| ory at 2E 2018.0+2056 and included in the soft | X-ray source list. |
| iscovery of this periodically pulsating binary | X-ray source occurred in November 1971. |
| s atmosphere, X-radiation from an astronomical | X-ray source has been discovered coming from Scorpiu |
| The | x-ray source at the core of NGC 300 is designated NG |
| An | X-ray source is in orbit around V691 Coronae Austral |
| making Sagittarius X-7 the first astronomical | X-ray source detected in Corona Australis. |
| eV gamma-ray source, and the rather weak Uhuru | X-ray source 4U 0833-45. |
| nt strong accreting, pulsing, eclipsing binary | X-ray source Vela X-1, also known as 4U 0900-40, and |
| 3U 1626-67, apparently the first astronomical | X-ray source discovered in the constellation Triangu |
| ygnus X-7 is another intense soft astronomical | X-ray source like Cygnus X-6 that is confined to the |
| is probably the first extrasolar astronomical | X-ray source observed in Canis Minor. |
| s in Circinus and Centaurus, but the causitive | X-ray source is most likely in Centaurus. |
| According to SIMBAD, the closer | X-ray source to Cyg XR-3 is EXOSAT source EXMS B1958 |
| The gamma-ray and | X-ray source GRS 1124-683, discovered by the Granat |
| s that at least one of these or a visibly dark | X-ray source originated the X-ray signals and has su |
| ROSAT detected an | X-ray source near the position of Sco X-3 at B1950.0 |
| Although it is only the third brightest | x-ray source in the constellation Cygnus, after the |
| Prior to 1970 no | X-ray source was detected in Serpens Caput. |
| is the designation for a discrete astronomical | X-ray source that has been identified in the constel |
| ulum Australe X-1 (TrA X-1) is an astronomical | X-ray source discovered in November 1974 after the X |
| BM Cam also emits X-rays and is the designated | X-ray source 1H 0501+592. |
| Uhuru did detect an | X-ray source at 2 ASE 1833-5 (GX 27+2), 2U 1833-05, |
| he average position of the currently brightest | X-ray source is RA 14h 41m 51.42±5s Dec -62° 36′ 12. |
| any of the ROSAT sources are likely to be the | X-ray source detected by the March 15, 1963, Aerobee |
| o, apparently did not search for or detect any | X-ray source in CMi. |
| 1RXS J210034.1-044442 is an | x-ray source in the constellation Aquarius. |
| X-ray source astrometry is necessary even when obser | |
| The fourth Uhuru catalog contains one | X-ray source detected early within the constellation |
| is the designation for a discrete astronomical | X-ray source that has been identified in the constel |
| the case that AT Mic is the first astronomical | X-ray source detected in the constellation Microscop |
| HEAO 1 detected an | X-ray source of NGC 4151 at 1H 1210+393, which is ou |
| on previously observed to have no astronomical | X-ray source above background. |
| HEAO 1 A1 detected no | X-ray source near Scorpius XR-4 nor Sco XR-4. |
| on SIMBAD yields only Serpens X-2 as the only | X-ray source within the box, along with two addition |
| Main article: Extrasolar | X-ray source astrometry |
| Main article: Visibly dark | X-ray source |
| 0426-10 is the designation for an astronomical | X-ray source detected by the X-ray observatory satel |
| Main article: Astronomical | X-ray source |
| oru Oda, was used to identify the first cosmic | X-ray source and thereby to launch the new field of |
| Main article: Astronomical | X-ray source catalog |
| LMC X-2 is a persistent variable | X-ray source with X-ray luminosity (Lx) ~ 0.6 to 3 x |
| Main article: Lockheed | X-ray source |
| error box for Lupus X-1, only one | X-ray source occurs within this box in the SIMBAD da |
| See also: Astrophysical | X-ray source |
| The HEAO A-1 | X-Ray Source Catalog included 842 discrete X-ray sou |
| 1989 the Japanese Ginga Team discovered a new | X-ray source that was cataloged as GS 2023+338. |
| The | X-ray source is assumed to be a neutron star as part |
| , Sgr 5) is a designation for the astronomical | X-ray source detected by the X-ray astronomy satelli |
| ers alike until XMM-Newton spotted the unusual | X-ray source while turning from one target to anothe |
| That Vega is regarded as an | X-ray source rests on one 4.8 s star-tracking observ |
| gnation for the second extrasolar astronomical | X-ray source in the constellation Sagittarius detect |
| A transient | X-ray source first discovered in 1996 by the Italian |
| A second | X-ray source detected on only one scan during the Ap |
| This | X-ray source is acknowledged in an early catalogue. |
| The | X-ray source has been designated 1SAX J1450.1-6920. |
| ignation for the fifth extrasolar astronomical | X-ray source in the constellation Scorpius detected |
| The | X-ray source parallelogram (error box) for 2U 1207+3 |
| The | X-ray source has also been detected by Ariel 5 (3A), |
| ation at 4U 1708-23 has one ROSAT visibly dark | X-ray source within 900". |
| ed as a possible visual identification for the | X-ray source Centaurus XR-2. |
| 'Extrasolar | X-ray source astrometry' becomes important with the |
| An | X-ray source designated Cepheus X-1 (or Cep X-1) was |
| hole candidate and 2000-2001 transient binary | X-ray source located in the constellation Ara. |
| gnation for the fourth extrasolar astronomical | X-ray source in the constellation Scorpius detected |
| s XR-3 (Sco XR-3) is a third such astronomical | X-ray source detected by an X-ray astronomy group at |
| 2 pm on April 2, 1997, is from an astronomical | X-ray source never seen before in the constellation |
| This | X-ray source does not appear to be associated with a |
| nal astrometry to confirm that an astronomical | X-ray source really is the same as an astronomical v |
| The earliest indications of an | X-ray source (Oph XR-1) near SN 1604, is not confirm |
| X-ray source 1H 0244+001 in Cetus has been identifie | |
| Gurzadyan, G.A., Vartanian, K.V., Solar | X-Ray Source Unassociated With Sunspots, Space Scien |
| rces GRO J1308-61 and IGR J13186-6257 (also an | X-ray source). |
| The Orion | X-ray source, λ Ori X-1, is not in any Uhuru catalog |
| Alpha Pictoris is an | X-ray source, which is unusual for an A-type star si |
| Legend: X - astronomical | X-ray source, red * - star, RSCVn - RS Canum Venatic |
| triangle - HI region, blue oval - galaxy, X - | X-ray source, red + - HII region, red diamond - IR o |
| Legend: X - | X-ray source, red + - HII region, Seyfert_2 - Seyfer |
| astronomical infrared source, X - astronomical | X-ray source, red * - star, red + - HII region, blue |
| Legend: DkNeb - dark nebula, x | -X-ray source, HMXB - high-mass X-ray binary, LMXB - |
| As an | X-ray source, NGC 4151 was apparently first so detec |
| Legend: X - | X-ray source, red * - star, Seyfert_1 - Seyfert type |
| reason for the invention, is that because the | X-ray source-point is swept electronically, not mech |
| winds from this pair makes the system a strong | X-ray source. |
| It is also a Seyfert 1 galaxy which is an | X-ray source. |
| s X-4, and that Scorpius X-4 is not a separate | X-ray source. |
| betrayed by the presence of a strong, diffuse | X-ray source. |
| e Crab Pulsar within it, is an intensive space | X-ray source. |
| AGR 1627-41 is a persistent | X-ray source. |
| Hydra A is an astronomical | X-ray source. |
| XMS B1706-232, an EXOSAT detected visibly dark | X-ray source. |
| These visually dark | X-ray sources can be radiative cosmic dust, hydrogen |
| ROSAT detected at least four | X-ray sources within 1° of the likely J2000.0 positi |
| is a designation associated with astronomical | X-ray sources in Serpens Cauda. |
| Of the first | X-ray sources discovered in each constellation (126 |
| The mean density of | X-ray sources is about one source per square degree. |
| The two stars that are | X-ray sources detected within the error box are HD 1 |
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