排序方式: 共有39条查询结果,搜索用时 312 毫秒
31.
B. H. Mauk J. B. Blake D. N. Baker J. H. Clemmons G. D. Reeves H. E. Spence S. E. Jaskulek C. E. Schlemm L. E. Brown S. A. Cooper J. V. Craft J. F. Fennell R. S. Gurnee C. M. Hammock J. R. Hayes P. A. Hill G. C. Ho J. C. Hutcheson A. D. Jacques S. Kerem D. G. Mitchell K. S. Nelson N. P. Paschalidis E. Rossano M. R. Stokes J. H. Westlake 《Space Science Reviews》2016,199(1-4):471-514
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H. E. Spence A. W. Case M. J. Golightly T. Heine B. A. Larsen J. B. Blake P. Caranza W. R. Crain J. George M. Lalic A. Lin M. D. Looper J. E. Mazur D. Salvaggio J. C. Kasper T. J. Stubbs M. Doucette P. Ford R. Foster R. Goeke D. Gordon B. Klatt J. O’Connor M. Smith T. Onsager C. Zeitlin L. W. Townsend Y. Charara 《Space Science Reviews》2010,150(1-4):243-284
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The charged-particle telescope (CPT) onboard the Clementine spacecraft measured the fluxes of energetic protons emitted in solar energetic particle events. Protons in the energy range from 10 to 80 MeV were of greatest interest for radiation effects such as total dose and single event upsets. Energetic electrons were also of interest for spacecraft charging and their contribution to total dose. The lower-energy CPT electron channels (25-500 keV) were mainly of geophysical interest. While orbiting the moon, the CPT observed the wake created by the moon when it blocked the flow of energetic particles in the magnetotail region. The CPT provided opportunities to observe energetic electron bursts during magnetic storms and magnetospheric substorms. CPT data are particularly useful in multispacecraft studies of interplanetary disturbances and their interaction with the magnetosphere. The proton channels on the CPT provided data on solar energetic protons and storm-time protons associated with the passage of an interplanetary shock at 0903 UT on Feb. 21, 1994. Results are compared with those from GOES-7, SAMPEX, and GEOTAIL. 相似文献
35.
The problems of engineering professionalism, working conditions, and ethics have long been a subject of much controversy but little well-written material. In this paper, the author attempts to analyze some of the more troublesome of these problems, and offers a few solutions of his own device. Although written in a semi-humorous vein, the subject material deals directly with professional/ethical problems faced by the contemporary engineer working for an employer. 相似文献
36.
The Two Wide-angle Imaging Neutral-atom Spectrometers (TWINS) NASA Mission-of-Opportunity 总被引:3,自引:0,他引:3
D. J. McComas F. Allegrini J. Baldonado B. Blake P. C. Brandt J. Burch J. Clemmons W. Crain D. Delapp R. DeMajistre D. Everett H. Fahr L. Friesen H. Funsten J. Goldstein M. Gruntman R. Harbaugh R. Harper H. Henkel C. Holmlund G. Lay D. Mabry D. Mitchell U. Nass C. Pollock S. Pope M. Reno S. Ritzau E. Roelof E. Scime M. Sivjee R. Skoug T. S. Sotirelis M. Thomsen C. Urdiales P. Valek K. Viherkanto S. Weidner T. Ylikorpi M. Young J. Zoennchen 《Space Science Reviews》2009,142(1-4):157-231
Two Wide-angle Imaging Neutral-atom Spectrometers (TWINS) is a NASA Explorer Mission-of-Opportunity to stereoscopically image the Earth’s magnetosphere for the first time. TWINS extends our understanding of magnetospheric structure and processes by providing simultaneous Energetic Neutral Atom (ENA) imaging from two widely separated locations. TWINS observes ENAs from 1–100 keV with high angular (~4°×4°) and time (~1-minute) resolution. The TWINS Ly-α monitor measures the geocoronal hydrogen density to aid in ENA analysis while environmental sensors provide contemporaneous measurements of the local charged particle environments. By imaging ENAs with identical instruments from two widely spaced, high-altitude, high-inclination spacecraft, TWINS enables three-dimensional visualization of the large-scale structures and dynamics within the magnetosphere for the first time. This “instrument paper” documents the TWINS design, construction, calibration, and initial results. Finally, the appendix of this paper describes and documents the Southwest Research Institute (SwRI) instrument calibration facility; this facility was used for all TWINS instrument-level calibrations. 相似文献
37.
J. B. Blake 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》1989,9(12):125
Blake and Freisen painted out that if the anomalous cosmic rays are only singly charged they can penetrate deeply into the Earth's magnetosphere well below the cutoff for stripped ions. Ions which reach low altitude can be stripped by the residual atmosphere and become stably trapped. An experiment has been developed which will be able to detect the intensities of such stably trapped heavy ions as a function of magnetospheric position. In anticipation of the flight of this experiment, the fluxes and spectra of the trapped heavy ions have been calculated based upon the anomalous component observed in the IPM. 相似文献
38.
J. B. Blake J. F. Fennell L. M. Friesen B. M. Johnson W. A. Kolasinski D. J. Mabry J. V. Osborn S. H. Penzin E. R. Schnauss H. E. Spence D. N. Baker R. Belian T. A. Fritz W. Ford B. Laubscher R. Stiglich R. A. Baraze M. F. Hilsenrath W. L. Imhof J. R. Kilner J. Mobilia D. H. Voss A. Korth M. Güll K. Fisher M. Grande D. Hall 《Space Science Reviews》1995,71(1-4):531-562
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B. Heber E. Keppler R.G. Marsden C. Tranquille B. Blake M. Fränz 《Space Science Reviews》2001,97(1-4):363-366
Moraal and Steenberg (1999), showed that the peak energy in the anomalous cosmic ray spectra is independent of the radial
distance up to a few AU away from the termination shock but dependent on the solar wind speed, the radius of the termination
shock and the scattering strength. In this paper we will discuss the variation of the cosmic ray oxygen energy spectrum as
measured by the Ulysses EPAC and the COSPIN/LET on board Ulysses. We found that the peak energy decreased from ∼5 MeV nucl−1, when Ulysses was at high northern heliographic latitudes embedded in the fast solar wind to ∼3.5 MeV n−1, in the streamer belt. The shift towards lower energy might also be caused by changing modulation although Voyager measurements
indicate no variation of the ACR Oxygen spectrum at ∼60 AU.
This revised version was published online in August 2006 with corrections to the Cover Date. 相似文献