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G. Randall Gladstone Steven C. Persyn John S. Eterno Brandon C. Walther David C. Slater Michael W. Davis Maarten H. Versteeg Kristian B. Persson Michael K. Young Gregory J. Dirks Anthony O. Sawka Jessica Tumlinson Henry Sykes John Beshears Cherie L. Rhoad James P. Cravens Gregory S. Winters Robert A. Klar Walter Lockhart Benjamin M. Piepgrass Thomas K. Greathouse Bradley J. Trantham Philip M. Wilcox Matthew W. Jackson Oswald H. W. Siegmund John V. Vallerga Rick Raffanti Adrian Martin J.-C. Gérard Denis C. Grodent Bertrand Bonfond Benoit Marquet François Denis 《Space Science Reviews》2017,213(1-4):447-473
The ultraviolet spectrograph instrument on the Juno mission (Juno-UVS) is a long-slit imaging spectrograph designed to observe and characterize Jupiter’s far-ultraviolet (FUV) auroral emissions. These observations will be coordinated and correlated with those from Juno’s other remote sensing instruments and used to place in situ measurements made by Juno’s particles and fields instruments into a global context, relating the local data with events occurring in more distant regions of Jupiter’s magnetosphere. Juno-UVS is based on a series of imaging FUV spectrographs currently in flight—the two Alice instruments on the Rosetta and New Horizons missions, and the Lyman Alpha Mapping Project on the Lunar Reconnaissance Orbiter mission. However, Juno-UVS has several important modifications, including (1) a scan mirror (for targeting specific auroral features), (2) extensive shielding (for mitigation of electronics and data quality degradation by energetic particles), and (3) a cross delay line microchannel plate detector (for both faster photon counting and improved spatial resolution). This paper describes the science objectives, design, and initial performance of the Juno-UVS. 相似文献
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Barraclough B.L. Dors E.E. Abeyta R.A. Alexander J.F. Ameduri F.P. Baldonado J.R. Bame S.J. Casey P.J. Dirks G. Everett D.T. Gosling J.T. Grace K.M. Guerrero D.R. Kolar J.D. Kroesche J.L. Lockhart W.L. McComas D.J. Mietz D.E. Roese J. Sanders J. Steinberg J.T. Tokar R.L. Urdiales C. Wiens R.C. 《Space Science Reviews》2003,105(3-4):627-660
The Genesis Ion Monitor (GIM) and the Genesis Electron Monitor (GEM) provide 3-dimensional plasma measurements of the solar
wind for the Genesis mission. These measurements are used onboard to determine the type of plasma that is flowing past the
spacecraft and to configure the solar wind sample collection subsystems in real-time. Both GIM and GEM employ spherical-section
electrostatic analyzers followed by channel electron multiplier (CEM) arrays for detection and angle and energy/charge analysis
of incident ions and electrons. GIM is of a new design specific to Genesis mission requirements whereas the GEM sensor is
an almost exact copy of the plasma electron sensors currently flying on the ACE and Ulysses spacecraft, albeit with new electronics
and programming. Ions are detected at forty log-spaced energy levels between ∼ 1 eV and 14 keV by eight CEM detectors, while
electrons with energies between ∼ 1 eV and 1.4 keV are measured at twenty log-spaced energy levels using seven CEMs. The spin
of the spacecraft is used to sweep the fan-shaped fields-of-view of both instruments across all areas of the sky of interest,
with ion measurements being taken forty times per spin and samples of the electron population being taken twenty four times
per spin. Complete ion and electron energy spectra are measured every ∼ 2.5 min (four spins of the spacecraft) with adequate
energy and angular resolution to determine fully 3-dimensional ion and electron distribution functions. The GIM and GEM plasma
measurements are principally used to enable the operational solar wind sample collection goals of the Genesis mission but
they also provide a potentially very useful data set for studies of solar wind phenomena, especially if combined with other
solar wind data sets from ACE, WIND, SOHO and Ulysses for multi-spacecraft investigations.
This revised version was published online in August 2006 with corrections to the Cover Date. 相似文献
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Medium energy neutral atom (MENA) imager for the IMAGE mission 总被引:1,自引:0,他引:1
Pollock C.J. Asamura K. Baldonado J. Balkey M.M. Barker P. Burch J.L. Korpela E.J. Cravens J. Dirks G. Fok M.-C. Funsten H.O. Grande M. Gruntman M. Hanley J. Jahn J.-M. Jenkins M. Lampton M. Marckwordt M. McComas D.J. Mukai T. Penegor G. Pope S. Ritzau S. Schattenburg M.L. Scime E. Skoug R. Spurgeon W. Stecklein T. Storms S. Urdiales C. Valek P. van Beek J.T.M. Weidner S.E. Wüest M. Young M.K. Zinsmeyer C. 《Space Science Reviews》2000,91(1-2):113-154
The Medium Energy Neutral Atom (MENA) imager was developed in response to the Imaging from the Magnetopause to the Aurora for Global Exploration (IMAGE) requirement to produce images of energetic neutral atoms (ENAs) in the energy range from 1 to 30 keV. These images will be used to infer characteristics of magnetospheric ion distributions. The MENA imager is a slit camera that images incident ENAs in the polar angle (based on a conventional spherical coordinate system defined by the spacecraft spin axis) and utilizes the spacecraft spin to image in azimuth. The speed of incident ENAs is determined by measuring the time-of-flight (TOF) from the entrance aperture to the detector. A carbon foil in the entrance aperture yields secondary electrons, which are imaged using a position-sensitive Start detector segment. This provides both the one-dimensional (1D) position at which the ENA passed through the aperture and a Start time for the TOF system. Impact of the incident ENA on the 1D position-sensitive Stop detector segment provides both a Stop-timing signal and the location that the ENA impacts the detector. The ENA incident polar angle is derived from the measured Stop and Start positions. Species identification (H vs. O) is based on variation in secondary electron yield with mass for a fixed ENA speed. The MENA imager is designed to produce images with 8°×4° angular resolution over a field of view 140°×360°, over an energy range from 1 keV to 30 keV. Thus, the MENA imager is well suited to conduct measurements relevant to the Earth's ring current, plasma sheet, and (at times) magnetosheath and cusp. 相似文献
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