3 edition of Analysis of energetic proton and electron data in Neptune"s magnetosphere found in the catalog.
Analysis of energetic proton and electron data in Neptune"s magnetosphere
1994 by California Institute of Tecnology, Division of Physics, Mathematics, and Astronomy Space Radiation Laboratory, National Aeronautics and Space Administration, National Technical Information Service, distributor in Pasadena, CA, [Washington, DC, Springfield, Va .
Written in English
|Statement||submitted by Edward C. Stone.|
|Series||NASA contractor report -- NASA CR-195707.|
|Contributions||United States. National Aeronautics and Space Administration.|
|The Physical Object|
When an energetic neutron collides with a proton (i.e., a hydrogen nucleus), there is a high probability that the neutron will exchange substantial momentum with the proton. Since human beings are largely composed of hydrogen-rich compounds such as proteins, fat, and especially water, neutrons passing through the human body have a substantial. Chen, Jiasheng and Theodore A. Fritz, CEP as a Source of Upstream Energetic Ions, In NATO Science Series Book: Multiscale Processes In The Earth’s Magnetosphere: From Interball To Cluster, Edited by: Jean-Andre Sauvaud and Zdenek Nemecek, Proceeding of the conference: Magnetospheric Response to Solar Activity, September , , Charles. Martin, G. I. Pugacheva, W. N. Spjeldvik and T. Kohno: "Dynamics of the Low Altitude Energetic Proton Fluxes Beneath the Main Terrestrial Radiation Belts", Journal of . Global ENA Imaging and In Situ Observations of Substorm Dipolarization on 10 August Abstract This paper presents the first combined use of data from Magnetospheric Multiscale (MMS), Two Wide-angle Imaging Neutral-atom Spectrometers (TWINS), and Van Allen Probes (RBSP) to study the 10 August magnetic dipolarization.
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This grant was for the analysis and interpretation of data obtained by the cosmic ray system (CRS) on Voyager 2 in the magnetosphere of Neptune. The research goals included the following: characterize the distribution and intensity of trapped electrons and protons; relate them to theoretical models of particle transport; study the particle absorption signatures of Neptune's moons Author: Edward C.
Stone. Analysis of energetic proton and electron data in Neptune's magnetosphere: final report for National Aeronautics and Space Administration, January 1, - Decem Author: Edward Stone ; United States. Analysis of energetic proton and electron data in Neptune's magnetosphere.
By Edward C. Stone. Abstract. This grant was for the analysis and interpretation of data obtained by the cosmic ray system (CRS) on Voyager 2 in the magnetosphere of Neptune. The research goals included the following: characterize the distribution and intensity of Author: Edward C.
Stone. "Analysis of Energetic Proton and Electron Data in Neptune's Magnetosphere" This grant was for the analysis and interpretation of data obtained by the cosmic ray system (CRS) on Voyager 2 in the magnetosphere of Neptune. The research goals included the following: characterize the distribution and intensity of trapped electrons.
The Cosmic Ray Subsystem aboard Voyager 2 measured large fluxes of trapped energetic protons and electrons in the inner magnetosphere of Neptune during the flyby; the protons above MeV observed by the Low Energy Telescopes are analyzed in this : Mark Dixon Looper.
Energetic Charged Particles in the Magnetosphere of Neptune | Science. The Voyager 2 cosmic ray system (CRS) measured significant fluxes of energetic [≥1 megaelectron volt (MeV)] trapped electrons.
The absence at Neptune ofclear, BS-associated protonandelectron enhance-ments is also ani unusual aspectofplanetary magnetosphere encounters by Voyager. Further, therewasonlyamodestincrease in the proton intensities at the magnetopause (MP) and a marginal electron intensity in-crease, both of which are unique in the.
2 Data Sources and Analysis Methods. The baseline observations for this study come from the Energetic Proton, Electron and Alpha Detector (EPEAD) on board the GOES‐15 spacecraft (GOES N Series Data Book, ; Hanser, ; Rodriguez et al., ). This satellite was launched on 4 March and was subsequently declared operational on 6.
The highly energetic electron environment in the inner magnetosphere (geosynchronous orbit and inward) has received a lot of interest recently, as it becomes increasingly evident that existing stat.
electron data collected by IMP 8 over a period of nearly 4 years. These data provide strong evidence that the high energy component of upstream electrons is closely related to the magnetopause electron layer.
DATA AND ANALYSIS Data for this analysis were collected between day and day by the California Institute of Technology. Voyager 2 observations of electrostatic electron and ion harmonic waves in Neptune's magnetosphere are addressed.
A model of electron Bernstein modes generated by a loss cone distribution of. The proton/electron telescope (PET) on SAMPEX (Solar, Anomalous, and Magnetospheric Particle Explorer) is designed to provide measurements of energetic electrons and light nuclei from solar. The electron spectra are based on fluxes derived from several different detectors /2/ and each point on a spectrum represents the integral flux above the corresponding energy.
The proton spectra are differential measurements from similar telescopes with different viewing directions for a single 30 minute time period. Energetic Electron Transport in the Inner Magnetosphere During Geomagnetic Storms and Substorms: Final Research Report 15 February Prepared by D.
McKENZIE and P. ANDERSON Space Science Applications Laboratory Laboratory Operations Prepared for NASA-GSFC Greenbelt, MD 1 Contract No. NAG51 Engineering and Technology Group. Energetic Particle. Energetic particles precipitating into the Earth’s atmosphere come from different sources: solar energetic protons, high-energy protons of energies up to a few hundreds of MeV from large eruptions on the surface of the sun, in solar flares and solar coronal mass ejections; From: The Dynamic Loss of Earth's Radiation Belts.
The proton intensity in the low latitude ‘rim’ of the polar region appears to track the interplanetary flux of solar protons more readily than does the polar intensity. The rim straddles the energetic electron trapping boundary, and the rim intensity is frequently greater than the polar plateau flux.
The Voyager 2 cosmic ray system (CRS) measured significant fluxes of energetic [>/=1 megaelectron volt (MeV)] trapped electrons and protons in the magnetosphere of Neptune.
The intensities are maximum near a magnetic L shell of 7, decreasing closer to the planet because of absorption by satellites and rings. The variation of the flux of energetic electrons in the magnetosphere has been proven to be strongly related to the solar wind speed.
Observations of GEO orbit show that the flux of low-energy electrons is not only modulated by the solar wind speed, but, if a time delay is added, is also positively correlated to the flux of high-energy electrons. Figure 2 Association between energetic electron bursts and the signatures of magnetic islands.
a,d, Differential energy ﬂuxes (in units of cm−2 keV−1 s−1 at 4s resolution) of electrons with energies of 35–94keV in three energy channels recorded by Cluster. Energetic electron bursts are seen in all three energy channels. b,e, The z.
Data from Explorer 45 (S/sup 3/- A) instruments have revealed characteristics of magnetospheric storm or substorm time energetic particle enhancements in the inner magnetosphere (L.
A review of the existing data on Neptune and a search of the NASA Planetary Data System (PDS) were completed to obtain the most current descriptions of the Neptunian high-energy particle environment.
These data were fit in terms of the O8 B-L coordinates to develop the electron and proton. Earth's magnetic field creates a 'bubble' around Earth that helps protect our planet from some of the more harmful effects of energetic particles streaming out from the sun in the solar wind.
Some of the earliest hints of this interaction go back to the s with the work of Richard Carrington, and in the early s with the work of Kristian Birkeland and Carl Stormer.
comparable to proton characteristic lengths we use multi-point magnetic field and density data (derived from spacecraft potential) from the Cluster spacecraft when they were in undisturbed intervals of slow and fast solar wind.
Using the spacecraft potential allows much higher time resolution than is typically. A study of the precipitation of protons ( 35 MeV) and electrons ( - MeV) in the northern auroral zone based on the observations of EXOS-C satellite during reveals that the global peak flux profile follows the global minimum magnetic field profile with a full-width-at-half-maximum (FWFM) of approx 7 deg for the proton zone and approx 5 deg for the electron zone.
Energy spectra of protons and sulphur The prime focus of the work is on the analysis and interpretation of the electron pitch angle distribution.
A discussion is presented on how adiabatic processes The analysis of the energetic particle data and magnetic ﬁeld data obtained with the Energetic Particles Detector and with the. Neptune is the eighth and farthest-known planet from the Sun in the Solar the Solar System, it is the fourth-largest planet by diameter, the third-most-massive planet, and the densest giant e is 17 times the mass of Earth, slightly more massive than its near-twin e is denser and physically smaller than Uranus because its greater mass causes more.
Particle acceleration and loss in the million electron Volt (MeV) energy range (and above) is the least understood aspect of radiation belt science. In order to measure cleanly and separately both the energetic electron and energetic proton components, there is a.
INSTaU•m• ANn DATA ANALYSIS. The Voyager cosmic ray system includes two high-energy telescopes, four low-energy telescopes and one electron telescope (TET). Each was optimized for sensitivity to the low fluxes of interplanetary cosmic rays. For a complete description see Stone et al.
The interplanetary data are analyzed by requiting. Energization of the Inner Magnetosphere by Solar Wind Pressure Pulses W.
William Liu Energetic Trapped Proton and Electron Flux Variations at Low Altitudes Measured Onboard CORONAS-F Satellite DuringAugust-December, Their Connection with the Particle Flux Variations in Geostationary Orbit Sergey N.
Kuznetsov and Irina N. Myagkova Magnetospheric Substorms and the Sources of Inner Magnetosphere Particle Acceleration E. Antonova Energization of the Inner Magnetosphere by Solar Wind Pressure Pulses W. William Liu Energetic Trapped Proton and Electron Flux Variations at Low Altitudes Measured Onboard.
magnetosphere, provide a survey of the energetic electron density and temperature distribution in the magnetotail be-tween McIlwain L-values ofL=6 and L= Analysis reveals the characteristics of the density-temperature distri-bution of energetic electrons and its variation as a function of solar wind speed and the Kp index.
The density. The RBSP Energetic particle, Composition, and Thermal plasma (RBSP-ECT) Suite. The RBSP-ECT SOC can be found here. The RBSP-ECT suite consists of three instruments designed to measure plasma and energetic particles in the radiation belts and inner magnetosphere. They are: the Helium Oxygen Proton Electron (HOPE) plasma spectrometer.
Intercalibration of magnetospheric energetic electron data Intercalibration of magnetospheric energetic electron data Friedel, R. W.; Bourdarie, S.; Cayton, T.
Introduction The natural energetic electron environment in the Earth's radiation belts is of general importance as dynamic variations in this environment can impact space hardware and. Waterfall’s CPI Theory views solar plasma as an electron wave-field transporting protons from the Sun to Earth’s auroral oval.
When it reaches the ionosphere, the electron releases its proton cargo and is free. The free electron either alone or in conjunction with other electrons joins with elementary particles found within the ionosphere. Hill, M.E., "Methods of Analysis for Voyager LECP Data," Scholarly paper required by the Dept.
of Physics, Univ. of Maryland, for the M.S. degree and for. Energetic neutral atom (ENA) imaging, often described as "seeing with atoms", is a technology used to create global images of otherwise invisible phenomena in the magnetospheres of planets and throughout the heliosphere, even to its outer constitutes the far-flung edge of the solar system.
The solar wind consists of ripped-apart atoms (called plasma) flying out of the Sun. Chenette, D.L., and E.
Stone, "The Mimas Ghost Revisited: An Analysis of the Electron Flux and Electron Microsignatures Observed in the Vicinity of Mimas at. related analysis of Pioneer 11 charged particle and gamma ray data acquired near the rings.
He has been Principal Investigator on several ongoing NASA research projects relating to analysis of Galileo Orbiter energetic particle data and to modeling of moon-magnetosphere interactions for the Galilean moons in the Jupiter system.
population of the magnetotail energetic‐electron population: in case (b) the question is then what is the source population of the outer electron radiation belt.  Three outstanding questions about these energetic‐ electron populations in the Earth’s magnetosphere are the following.
(1) What is the source population of the outer. In Earth’s magnetosphere, an extreme example of impulsive acceleration occurred Mawhen a high-speed interplanetary shock launched by a CME compressed the boundary of the magnetosphere well inside the orbit of geosynchronous spacecraft.
8 The event produced >MeV electron and proton radiation belts within a normally benign. Dichter, B. K., and F. A. Hanser (), Development and Use of Data Analysis Procedures for the CRRES Payloads AFGL/Dosimeter and AGRL/Fluxmeter and Application of the Data Analysis Results to Improve the Static and Dynamic Models of the Earth’s Radiation Belts, PL-TR, Phillips Laboratory, AFMC, Hanscom AFB, MA.Purchase COSPAR: Space Research - 1st Edition.
Print Book & E-Book. ISBN Table 1 shows the proton energy ranges at which each electron channel is subject to contamination by protons (CP) with an energy range of – keV for E1 channel.
The E2 electron channel is sensitive to protons over the energy range of – keV; and the E3 channel is affected by protons in the range of – keV (Evans and Greer ).