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311.
S.C. Gallagher W.N. Brandt G. Chartas G.P. Garmire R.M. Sambruna 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2004,34(12):2594-2598
Energetic outflows appear to occur in conjunction with active mass accretion onto supermassive black holes. These outflows are most readily observed in the 10% of quasars with broad absorption lines, where the observer’s line of sight passes through the wind. Until fairly recently, the paucity of X-ray data from these objects was notable, but now sensitive hard-band missions such as Chandra and XMM-Newton are routinely detecting broad absorption line quasars. The X-ray regime offers qualitatively new information for the understanding of these objects, and these new results must be taken into account in theoretical modeling of quasar winds. 相似文献
312.
A. N. Parmar G. Hasinger M. Arnaud X. Barcons D. Barret H. Bhringer A. Blanchard M. Cappi A. Comastri T. Courvoisier A. C. Fabian F. Fiore I. Georgantopoulos P. Grandi R. Griffiths A. Hornstrup N. Kawai K. Koyama K. Makishima G. Malaguti K. O. Mason C. Motch M. Mendez T. Ohashi F. Paerels L. Piro T. Ponman J. Schmitt S. Sciortino G. Trinchieri M. van der Klis M. Ward 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2004,34(12):2623
Europe is one of the major partners building the International Space Station (ISS) and European industry, together with ESA, is responsible for many station components including the Columbus Orbital Facility, the Automated Transport Vehicle, two connecting modules and the European Robotic Arm. Together with this impressive list of contributions there is a strong desire within the ESA Member States to benefit from this investment by utilizing the unique capabilities of the ISS to perform world-class science. XEUS is one of the astronomical applications being studied by ESA to utilize the capabilities of the ISS. XEUS will be a long-term X-ray observatory with an initial mirror area of 6 m2 at 1 keV that will be expanded to 30 m2 following a visit to the ISS. The 1 keV spatial resolution is expected to be 2–5″ half-energy-width. XEUS will consist of separate detector and mirror spacecraft (MSC) aligned by active control to provide a focal length of 50 m. A new detector spacecraft, complete with the next generation of instruments, will also be added after visiting the ISS. The limiting 0.1–2.5 keV sensitivity will then be 4 × 10−18 erg cm−2 s−1, around 200 times better than XMM-Newton, allowing XEUS to study the properties of the hot baryons and dark matter at high redshift. 相似文献
313.
Yuichiro Ezoe Tomoki Kimura Satoshi Kasahara Atsushi Yamazaki Kazuhisa Mitsuda Masaki Fujimoto Yoshizumi Miyoshi Graziella Branduardi-Raymont Kumi Ishikawa Ikuyuki Mitsuishi Tomohiro Ogawa Takuya Kakiuchi Takaya Ohashi 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2013
For the future Japanese exploration mission of the Jupiter’s magnetosphere (JMO: Jupiter Magnetospheric Orbiter), a unique instrument named JUXTA (Jupiter X-ray Telescope Array) is being developed. It aims at the first in-situ measurement of X-ray emission associated with Jupiter and its neighborhood. Recent observations with Earth-orbiting satellites have revealed various X-ray emission from the Jupiter system. X-ray sources include Jupiter’s aurorae, disk emission, inner radiation belts, the Galilean satellites and the Io plasma torus. X-ray imaging spectroscopy can be a new probe to reveal rotationally driven activities, particle acceleration and Jupiter–satellite binary system. JUXTA is composed of an ultra-light weight X-ray telescope based on micromachining technology and a radiation-hard semiconductor pixel detector. It covers 0.3–2 keV with the energy resolution of <100 eV at 0.6 keV. Because of proximity to Jupiter (∼30 Jovian radii at periapsis), the image resolution of <5 arcmin and the on-axis effective area of >3 cm2 at 0.6 keV allow extremely high photon statistics and high resolution observations. 相似文献
314.
E. Bozzo P. Romano C. Ferrigno P. Esposito V. Mangano 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2013
Supergiant fast X-ray transients are a subclass of high mass X-ray binaries displaying a peculiar and still poorly understood extreme variability in the X-ray domain. These sources undergo short sporadic outbursts (LX∼ 1036–1037 erg s−1), lasting few ks at the most, and spend a large fraction of their time in an intermediate luminosity state at about LX∼ 1033–1034 erg s−1. The sporadic and hardly predictable outbursts of supergiant fast X-ray transients were so far best discovered by large field of view (FOV) coded-mask instruments; their lower luminosity states require, instead, higher sensitivity focusing instruments to be studied in sufficient details. In this contribution, we provide a summary of the current knowledge on supergiant fast X-ray transients and explore the contribution that the new space mission concept LOFT, the Large Observatory for X-ray Timing, will be able to provide in the field of research of these objects. 相似文献
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317.
X射线数字成像系统及其应用 总被引:4,自引:0,他引:4
X射线数字成像技术具有一些引进胶片成像技术所不具备的特点,本文介绍了几种X射线数字成像系统的技术特点和主要性能指标,并就其综合性能进行了比较;介绍了两种常见的X射线数字成像系统的应用情况;对X射线数字成像技术的发展方向作了简述。 相似文献
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319.
Tobias G.W. Verhulst Stanimir M. Stankov 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2018,61(9):2245-2251
A total solar eclipse occurred on 21 August 2017, with the path of totality starting over the North Pacific Ocean, crossing North-America and ending over the Mid-Atlantic Ocean slightly North of the equator. As a result, a partial solar eclipse was observed as far away as the Western Europe. The ionospheric observatory in Dourbes, Belgium, was right on the edge of the partial eclipse and was exposed for a very short period of only few minutes just before the local sunset. High-resolution ionospheric measurements were carried out at the observatory with collocated digital ionosonde and GNSS receivers. The data analysis revealed a clear wave-like pattern in the ionosphere that can be seen arriving before the local onset of the eclipse. The paper details the analysis and provides a possible explanation of the observed phenomenon. 相似文献
320.
根据PTB和ISO 4037-1:2019要求,关于高空气比释动能系列(H系列)X射线参考辐射质的推荐数据,外推得出H-450的附加过滤为6.24 mm Cu,第一半值层(HVL1st)为(5.39~5.52)mm Cu,平均光子能量为(214.25~214.78)keV,剂量率为11.51 Gy/h(距离焦斑为1 m处,管电流为10 mA)。随后,使用PTW32005电离室作为测量器具,采用半值层法建立H-450 X射线参考辐射质,得出HVL1st为5.37 mm Cu,第二半值层(HVL2nd)为5.97 mm Cu,同质系数为0.9。最后,使用PTW30013次级标准电离室测量得出H-450 X射线参考辐射质下距离焦斑1 m,管电流为10 mA时的剂量率值为11.98 Gy/h,与理论值的相对误差为4.07 %。采用MCNP 5软件对H-450 X射线参考辐射质进行能谱模拟并计算得出其平均光子能量为200.4 keV。 相似文献