排序方式: 共有7条查询结果,搜索用时 4 毫秒
1
1.
Klumpar D.M. Möbius E. Kistler L.M. Popecki M. Hertzberg E. Crocker K. Granoff M. Tang Li Carlson C.W. McFadden J. Klecker B. Eberl F. Künneth E. Kästle H. Ertl M. Peterson W.K. Shelly E.G. Hovestadt D. 《Space Science Reviews》2001,98(1-2):197-219
The Time-of-flight Energy Angle Mass Spectrograph (TEAMS) is being flown on the FAST Small Explorer mission to measure the 3-dimensional distribution function of the major ion species present in the lower magnetosphere. The instrument is similar to time-of-flight plasma analyzer systems that have been designed and planned for flight as CODIF (COmposition and DIstribution Function analyzer) on the four European Space Agency Cluster-II spacecraft and, as ESIC (Equator-S Ion Composition instrument) on Equator-S. This instrument allows the 3-dimensional distribution functions of individual ion species to be determined within
spin period (2.5 s). Two-dimensional distributions are measured in 80 ms. These capabilities are crucial for the study of selective energization processes in the auroral regions of the magnetosphere. The design, operational characteristics, and test and calibration results for this instrument are presented. The sensor consists of a toroidal top-hat electrostatic analyzer with instantaneous acceptance of ions over 360° in polar angle. After post-acceleration of the incoming ions by up to 25 kV, a time-of-flight mass spectrograph discriminates the individual species. It has been demonstrated through calibration that the instrument can easily separate H+, He2+, He+, O+ and, for energies after post-acceleration of > 20 keV, even O2
+ molecules. On-board mass discrimination and the internal accumulation of several distinct data quantities combined with the spacecraft's flexible telemetry formatting allow for instrument data rates from 7.8 kb s–1 to 315 kb s–1 to be telemetered to ground through the FAST centralized Instrument Data Processor. 相似文献
2.
The Plasma and Suprathermal Ion Composition (PLASTIC) Investigation on the STEREO Observatories 总被引:1,自引:0,他引:1
A. B. Galvin L. M. Kistler M. A. Popecki C. J. Farrugia K. D. C. Simunac L. Ellis E. Möbius M. A. Lee M. Boehm J. Carroll A. Crawshaw M. Conti P. Demaine S. Ellis J. A. Gaidos J. Googins M. Granoff A. Gustafson D. Heirtzler B. King U. Knauss J. Levasseur S. Longworth K. Singer S. Turco P. Vachon M. Vosbury M. Widholm L. M. Blush R. Karrer P. Bochsler H. Daoudi A. Etter J. Fischer J. Jost A. Opitz M. Sigrist P. Wurz B. Klecker M. Ertl E. Seidenschwang R. F. Wimmer-Schweingruber M. Koeten B. Thompson D. Steinfeld 《Space Science Reviews》2008,136(1-4):437-486
The Plasma and Suprathermal Ion Composition (PLASTIC) investigation provides the in situ solar wind and low energy heliospheric ion measurements for the NASA Solar Terrestrial Relations Observatory Mission, which consists of two spacecraft (STEREO-A, STEREO-B). PLASTIC-A and PLASTIC-B are identical. Each PLASTIC is a time-of-flight/energy mass spectrometer designed to determine the elemental composition, ionic charge states, and bulk flow parameters of major solar wind ions in the mass range from hydrogen to iron. PLASTIC has nearly complete angular coverage in the ecliptic plane and an energy range from ~0.3 to 80 keV/e, from which the distribution functions of suprathermal ions, including those ions created in pick-up and local shock acceleration processes, are also provided. 相似文献
3.
THE CLUSTER ION SPECTROMETRY (CIS) EXPERIMENT 总被引:5,自引:0,他引:5
H. RÈME J. M. Bosqued J. A. Sauvaud A. Cros J. Dandouras C. Aoustin J. Bouyssou Th. Camus J. Cuvilo C. Martz J. L. MÉDALE H. Perrier D. Romefort J. Rouzaud C. D'Uston E. MÖBIUS K. Crocker M. Granoff L. M. Kistler M. Popecki D. Hovestadt B. Klecker G. Paschmann M. Scholer C. W. Carlson D. W. Curtis R. P. Lin J. P. Mcfadden V. Formisano E. Amata M. B. Bavassano-CATTANEO P. Baldetti G. Belluci R. Bruno G. Chionchio A. Di Lellis E. G. Shelley A. G. Ghielmetti W. Lennartsson A. Korth H. Rosenbauer R. Lundin S. Olsen G. K. Parks M. Mccarthy H. Balsiger 《Space Science Reviews》1997,79(1-2):303-350
The Cluster Ion Spectrometry (CIS) experiment is a comprehensive ionic plasma spectrometry package on-board the four Cluster spacecraft capable of obtaining full three-dimensional ion distributions with good time resolution (one spacecraft spin) with mass per charge composition determination. The requirements to cover the scientific objectives cannot be met with a single instrument. The CIS package therefore consists of two different instruments, a Hot Ion Analyser (HIA) and a time-of-flight ion COmposition and DIstribution Function analyser (CODIF), plus a sophisticated dual-processor-based instrument-control and Data-Processing System (DPS), which permits extensive on-board data-processing. Both analysers use symmetric optics resulting in continuous, uniform, and well-characterised phase space coverage. CODIF measures the distributions of the major ions (H+, He+, He++, and O+) with energies from ~0 to 40 keV/e with medium (22.5°) angular resolution and two different sensitivities. HIA does not offer mass resolution but, also having two different sensitivities, increases the dynamic range, and has an angular resolution capability (5.6° × 5.6°) adequate for ion-beam and solar-wind measurements. 相似文献
4.
Möbius E. Kistler L.M. Popecki M.A. Crocker K.N. Granoff M. Turco S. Anderson A. Demain P. Distelbrink J. Dors I. Dunphy P. Ellis S. Gaidos J. Googins J. Hayes R. Humphrey G. Kästle H. Lavasseur J. Lund E.J. Miller R. Sartori E. Shappirio M. Taylor S. Vachon P. Vosbury M. Ye V. Hovestadt D. Klecker B. Arbinger H. Künneth E. Pfeffermann E. Seidenschwang E. Gliem F. Reiche K.-U. Stöckner K. Wiewesiek W. Harasim A. Schimpfle J. Battell S. Cravens J. Murphy G. 《Space Science Reviews》1998,86(1-4):449-495
The Solar Energetic Particle Ionic Charge Analyzer (SEPICA) is the main instrument on the Advanced Composition Explorer (ACE)
to determine the ionic charge states of solar and interplanetary energetic particles in the energy range from ≈0.2 MeV nucl−1
to ≈5 MeV charge−1. The charge state of energetic ions contains key information to unravel source temperatures, acceleration,
fractionation and transport processes for these particle populations. SEPICA will have the ability to resolve individual charge
states and have a substantially larger geometric factor than its predecessor ULEZEQ on ISEE-1 and -3, on which SEPICA is based.
To achieve these two requirements at the same time, SEPICA is composed of one high-charge resolution sensor section and two
low- charge resolution, but large geometric factor sections. The charge resolution is achieved by the focusing of the incoming
ions, through a multi-slit mechanical collimator, deflection in an electrostatic analyzer with a voltage up to 30 kV, and
measurement of the impact position in the detector system. To determine the nuclear charge (element) and energy of the incoming
ions, the combination of thin-window flow-through proportional counters with isobutane as counter gas and ion-implanted solid
state detectors provide for 3 independent ΔE (energy loss) versus E (residual energy) telescopes. The multi-wire proportional
counter simultaneously determines the energy loss ΔE and the impact position of the ions. Suppression of background from penetrating
cosmic radiation is provided by an anti-coincidence system with a CsI scintillator and Si-photodiodes. The data are compressed
and formatted in a data processing unit (S3DPU) that also handles the commanding and various automatted functions of the instrument.
The S3DPU is shared with the Solar Wind Ion Charge Spectrometer (SWICS) and the Solar Wind Ion Mass Spectrometer (SWIMS) and
thus provides the same services for three of the ACE instruments. It has evolved out of a long family of data processing units
for particle spectrometers.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
5.
The ionic charge distributions of solar energetic particles (SEP) as observed in interplanetary space provide fundamental
information about the origin of these particles, and the acceleration and propagation processes at the Sun and in interplanetary
space. In this paper we review the measurements of ionic charge states of energetic particles in interplanetary space and
discuss their implication for our understanding of SEP sources, and acceleration and propagation processes. 相似文献
6.
B. Klecker H. Kunow H. V. Cane S. Dalla B. Heber K. Kecskemety K.-L. Klein J. Kota H. Kucharek D. Lario M. A. Lee M. A. Popecki A. Posner J. Rodriguez-Pacheco T. Sanderson G. M. Simnett E. C. Roelof 《Space Science Reviews》2006,123(1-3):217-250
The characteristics of solar energetic particles (SEP) as observed in interplanetary space provide fundamental information about the origin of these particles, and the acceleration and propagation processes at the Sun and in interplanetary space. Furthermore, energetic particles provide information on the development and structure of coronal mass ejections as they propagate from the solar corona into the interplanetary medium. In this paper we review the measurements of energetic particles in interplanetary space and discuss their implication for our understanding of the sources, and of acceleration and propagation processes. 相似文献
7.
The ionic charge of solar energetic particles (SEP) as observed in interplanetary space is an important parameter for the
diagnostic of the plasma conditions at the source region and provides fundamental information about the acceleration and propagation
processes at the Sun and in interplanetary space. In this paper we review the new measurements of ionic charge states with
advanced instrumentation onboard the SAMPEX, SOHO, and ACE spacecraft that provide for the first time ionic charge measurements
over the wide energy range of ∼0.01 to 70 MeV/nuc (for Fe), and for many individual SEP events. These new measurements show
a strong energy dependence of the mean ionic charge of heavy ions, most pronounced for iron, indicating that the previous
interpretation of the mean ionic charge being solely related to the ambient plasma temperature was too simplistic. This energy
dependence, in combination with models on acceleration, charge stripping, and solar and interplanetary propagation, provides
constraints for the temperature, density, and acceleration time scales in the acceleration region. The comparison of the measurements
with model calculations shows that for impulsive events with a large increase of Q
Fe(E) at energies ≤1 MeV/nuc the acceleration occurs low in the corona, typically at altitudes ≤0.2 R
S
. 相似文献
1