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11.
Progress of Solar Wind Magnetosphere Ionosphere Link Explorer(SMILE) Mission 总被引:1,自引:1,他引:0
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SMILE (Solar wind Magnetosphere Ionosphere Link Explorer) mission is a joint ESA-CAS space science project. The working orbit is a 19 Re 5000 km HEO with 4 scientific instruments:Soft X-ray Imager(SXI), Ultra-Violet Imager (UVI), Magnetometer (MAG) and Light Ion Analyzer (LIA). SMILE aims to understand the interaction between the solar wind and the Earth's magnetosphere through the images of SXI and UVI and in-situ measurement from LIA and MAG. After the kick-off in 2016, the SMILE project went to Phase A study. The mission adoption is scheduled for November 2018, with a target launch date in 2022-2023. In this paper, the background of the mission, scientific objectives, the design and characteristics of scientific instruments and the mission outline will be introduced in details. 相似文献
12.
K.O. Mason G. Branduardi-Raymont P.M. Ogle M.J. Page E.M. Puchnarewicz N.J. Salvi 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2004,34(12):2610-2613
Long (>100 ks) observations of the bright Seyfert galaxies Mrk 766 and NGC 4051 have been obtained using XMM-Newton. The RGS 5–38 Å spectra reveal evidence of broad features. These can be modelled with relativistic emission lines coming from the immediate vicinity of a massive rotating black hole. Lines of OVIII, NVII and CVI are required to reproduce the spectrum of Mrk 766, whereas the spectrum of NGC 4051 can be modelled using a single, even broader OVIII line. Both Seyferts also exhibit broad iron line emission in the 2–8 keV range, and the data available thus far suggest that the strength of the low-energy emission lines and the strength of the iron line may be correlated. 相似文献
13.
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
14.
F.A. Jansen S.P. McKechnie P.A.J. de Korte J.A.M. Bleeker E. Gronenschild A. Peacock G. Manzo G. Branduardi-Raymont B. Kellett 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》1985,5(3):49-52
The young supernova remnant Cas A has been observed with the imaging proportional counter (PSD) of the EXOSAT observatory. High quality spatially resolved, spectral data allow for the first time the determination of the temperature structure of the remnant. Preliminary results on the distribution of temperature and emission measureover the remnant are presented. 相似文献
15.
K. O. Mason F. A. Cordova R. H. D. Corbet G. Branduardi-Raymont 《Space Science Reviews》1985,40(1-2):225-228
An x-ray observation of 2S 0921-630 has been made coincident with the time of optical eclipse of this 9-day binary. No significant reduction in X-ray flux is measured. This can be explained if the binary orbit is viewed almost exactly edge-on, so that the central X-ray emitting star is obscured by the accretion disk from direct view. The X-rays that are seen are scattered into the line of sight by material above and below the disk and the apparent size of the X-ray emission region is thus large compared to the size of the occulting star. 相似文献