Engineering topics

Elphic, R. C.

Publications and source records attributed to Elphic, R. C..

At least 55 records · Page 3

NASA NTRS1994

Maximizing the Scientific Return of Low Cost Planetary Missions Using Solar Electric Propulsion(abstract)

After many years of development, solar electric propulsion is now a practical low cost alternative for many planetary missions. In response to the recent Discovery AO, we and a number of colleagues have examined the scientific return from a missioon to map the Moon and then rendezvous with a small body. In planning this mission, we found that solar electric propulsion was quite affordable under the Discovery guidelines, that many targets could be reached more rapidly with solar electric propulsion than chemical propulsion, that a large number of planetary bodies were accessible with modest propulsion systems, and that such missions were quite adaptable, with generous launch windows which minimized mission risks. Moreover, solar electric propulsion is ideally suited for large payloads requiring a large amount of power.

solar electric propulsion low cost missions ion th↗

NASA NTRS1993

Electron generation of electrostatic waves in the plasma sheet boundary layer

Broadband electrostatic noise (BEN) has been shown to occur in conjunction with ion beams; extensive investigations of possible ion beam-related instabilities that could generate the observed wave spectra have been conducted. It has also been demonstrated that unstable electron distribution functions are sometimes measured in the plasma sheet boundary layer. We present simultaneous observations of ion and electron distribution functions and electric field wave spectra measured by ISEE 1 and ISEE 2 in the Earth's magnetotail. As the spacecraft moved from the tail lobe toward the plasma sheet, the fast indication of boundary layer plasma was seen in the electron distributions, followed some minutes later by the detection of boundary layer ions. The onset of large-amplitude electrostatic waves at frequencies up to the electron plasma frequency was coincident with the onset of the boundary layer electrons, suggesting that broadband electrostatic waves may often be generated by unstable electron distributions in the plasma sheet boundary layer, particularly the higher frequency portion of the wave spectrum. The observed changes in the electron distribution functions indicate that the plasma was not heated locally by the waves.

Onsager, T. G.↗

NASA NTRS1993

Well-resolved observations by ISEE 2 of ion dispersion in the magnetospheric cusp

During a prolonged period of southward IMF on October 30, 1978, the ISEE 2 spacecraft observed an unusually prolonged and distinct region of ion energy-time dispersion in the dayside dawn magnetosphere. Observed plasma features included the (1) presence of magnetosheath electrons and initial absence of magnetosheath ions and (2) subsequent arrival and energy-time dispersion of magnetosheath ions as the spacecraft transited outbound from 6.03 to 7.66 Earth radii. We use ISEE 2 ion measurements to illustrate these dispersive time-of-flight effects and to support our interpretation of a location in the north magnetospheric cusp. Ion energy dispersion persists for about 35 min and includes well-resolved sequences of magnetosheath and magnetospheric ion distributions. We focus primarily on observations and time-of-flight analysis of ions from the magnetosheath, which are observed simultaneously entering and exiting the cusp at different energies. We discuss the observational support and shortcomings of various ion injection locations and durations and conclude that quasi-steady merging at the dayside magnetopause, with ion dispersion caused by spacecraft motion away from the last closed field line, is the most likely scenario.

Phillips, J. L.↗

NASA NTRS1993

Solar wind-induced secondary ions and their relation to lunar surface composition

Based on previous laboratory experiments simulating solar wind sputtering of lunar surface materials, it appears that solar wind ions sputter secondary ions in sufficient numbers to be measured from low-altitude lunar orbit. Solar wind protons are hundreds of times less efficient than those used in standard secondary ion mass spectrometry; nevertheless secondary ions of Na, Mg, Al, Si, K, Ca, Mn, Ti and Fe were observed sputtered from sample simulants of mare and highland soils. These secondary ion fluxes depend both on concentration in the soil and on probability of ionization; yields of easily ionized elements such as K and Na are relatively much greater than those for the more electronegative elements and compounds. The principal geochemical indicator elements Na, Mg, Al, Si, K, Ca, Ti, Mn and Fe are nevertheless detectable. However, it has not been shown that the observed secondary ions vary strictly one-to-one with their concentrations in the geochemically distinct soil simulants used here. While we have a first order understanding of secondary ion sputtering, it is not clear that the observed ion yields can be linked with great accuracy to the simulant's composition. The simulants were analyzed by electron microprobe to establish their detailed composition. The observed secondary ion fluxes can then be compared with the microprobe results. For example Ti(+) fluxes from the three simulants correspond to the true composition with accuracies of better than 10 percent for the high-Ti basalt, and about 20 percent for the low-Ti simulant. The highlands simulant produced a statistically insignificant Ti(+) count rate. Here we discuss the results of further SIMS experiments using the ASU/Center for Solid State Science facility. With careful isolation and preparation of samples, we avoid the problems of the previous experiments. In particular, we will make use of ground-up sample to mimic the sputtering behavior of regolith, and will avoid charging by placing the soil on a conducting indium substrate. We report the results of a blind test of the SIMS technique using a sample of unknown composition.

Elphic, R. C.↗

NASA NTRS1992

A two satellite study of nightside flux transfer events in the plasma sheet

The short-term (about 1 min) events during two consecutive substorms on March 23 1979 have been studied using high time resolution measurements of magnetic and electric fields and of the kiloelectronvolt electron flux at X about -21 R(e). Data obtained make it possible to describe the localized magnetic structures transported or propagated within the plasma sheet and to identify these events as plasma sheet nightside magnetic flux transfer events (NFTEs). The best examples of the NFTEs found so far are all observed in a thin portion of plasma sheet where the contraction of the reconnected field lines dominates over the oppositely directed pressure gradient force. Systematic differences in the magnetic variations observed at ISEE-1 and 2 indicate current concentration at the outer plasma sheet boundary during the passage of a NFTE.

Sergeev, V. A.↗

NASA NTRS1992

An ion mass spectrometer for measuring isotopic adundances and loss rates of O, C and H in Mars' upper atmosphere

The history of Mars' climate is clearly intimately linked to the evolution of its store of volatiles, particularly H2O, and CO2. The global CO2-H2O system is complex, with a number of production, loss, exchange, and buffering mechanisms operating between the atmosphere and the surface. For example, loss of these volatiles takes place through solar wind interaction with the upper atmosphere/ionosphere, ionospheric chemistry, and thermal escape. The atmospheric water inventory is, in turn, influenced by the exchange with polar water ice deposits and high latitude ground-ice. Atmospheric CO2, on the other hand, can be lost through adsorption in the regolith and in the formation of carbonates. Finally, oxygen is exchanged between atmospheric CO2 and H2O.

Elphic, R. C.↗

NASA NTRS1992

Lunar and Asteroid Composition Using a Remote Secondary Ion Mass Spectrometer

Laboratory experiments simulating solar wind sputtering of lunar surface materials have shown that solar wind protons sputter secondary ions in sufficient numbers to be measured from low-altitude lunar orbit. Secondary ions of Na, Mg, Al, Si, K, Ca, Mn, Ti, and Fe have been observed sputtered from sample simulants of mare and highland soils. While solar wind ions are hundreds of times less efficient than those used in standard secondary ion mass spectrometry, secondary ion fluxes expected at the Moon under normal solar wind conditions range from approximately 10 to greater than 10(exp 4) ions cm(sup -2)s(sup -1), depending on species. These secondary ion fluxes depend both on concentration in the soil and on probability of ionization; yields of easily ionized elements such as K and Na are relatively much greater than those for the more electronegative elements and compounds. Once these ions leave the surface, they are subject to acceleration by local electric and magnetic fields. For typical solar wind conditions, secondary ions can be accelerated to an orbital observing location. The same is true for atmospheric atoms and molecules that are photoionized by solar EUV. The instrument to detect, identify, and map secondary ions sputtered from the lunar surface and photoions arising from the tenuous atmosphere is discussed.

Elphic, R. C.↗

NASA NTRS1991

Observations of reconnection of interplanetary and lobe magnetic field lines at the high-latitude magnetopause

Results are presented of ISEE 2 observations of plasma accelerations obtained at the high-latitude (lobe) magnetopause at a time when the local magnetosheath and magnetospheric magnetic fields were nearly oppositely directed and the flow speed in the magnetosheath, V(s), was nearly equal to the local Alfven speed, V(A). The observations provide direct evidence for the rereconnection of the open field lines of the tail lobes with the IMF, when the magnetic field shear is large. It is pointed out, however, that, since V(s) was almost equal to V(A), it is unlikely that the rereconnection is associated with the strong sunward convection in the polar cap.

Gosling, J. T.↗

NASA NTRS1991

ISEE 1 observations of electrostatic ion cyclotron waves in association with ion beams on auroral field lines from about 2.5 to 4.5 R(E)

Quasi-monochromatic waves at about the hydrogen cyclotron frequency were observed as the ISEE 1 satellite traversed auroral field lines at radial distances of about 2.5-4.5 R(E) near midnight on June 19, 1981. Waves and both lower and higher frequencies were observed at higher altitudes, and possible electrostatic helium cyclotron and oxygen cyclotron waves occurred at lower altitudes. Upflowing hydrogen and oxygen beams and field-aligned currents occurred simultaneously. The features of the waves are most consistent with the current-driven mode. In addition, numerical studies of the linear dispersion relation, using parameters based on the observations, show that both the parallel and oblique two-stream modes and the ion-beam-driven modes were stable while oblique current-driven modes were unstable. The O(+) and H(+) distributions provide evidence for interactions with local electrostatic ion cyclotron waves and for the H(+)-O(+) two-stream instability at altitudes below the satellite.

Catell, C. A.↗

NASA NTRS1990

Field-aligned current signatures in the near-tail region. II - Coupling between the region 1 and the region 2 systems

The development of the substorm-associated current signature in the near magnetotail region is investigated on the basis of ground magnetometer, satellite magnetic field, and energetic particle data collected during the March 28, 1979 substorm event. It is shown that the development of the region 1 and the region 2 systems during substorms should be viewed in terms of the formation of a new current system in the near-tail system, rather than merely an enhancement in the current intensity of preexisting systems. Experimental data suggest that the region 2 system is as important as the region 1 system and must be taken into account. The development of the region 2 system and the three-dimensional current closure are discussed.

Ohtani, S.↗

NASA NTRS1990

Flux transfer events at the magnetopause and in the ionosphere

Observations of the flux transfer events (FTEs) made by the ISEE 2 spacecraft at the dayside magnetopause and simultaneous EISCAT observations of ionospheric flow bursts and Ny Alesund observations of dayside auroral breakup events near the ISEE field line footpoints are presented. The simultaneous observations took place on December 1, 1986. EISCAT radar recorded ionospheric flow bursts of up to 1 km/s and the peak of each burst followed an FTE observation at ISEE by a few minutes. Bursts were comprised of a westward and then poleward flow and each burst was recorded to have lasted ten or fifteen minutes. Dayside auroral breakup forms were observed by the all sky camera at Ny Alesund during or shortly after the flow bursts and moving westward and then poleward. It is noted that this is the first observation of a direct link between FTEs at the magnetopause and flowbursts and associated dayside auroral forms.

Elphic, R. C.↗

NASA NTRS1990

Cold ion beams in the low latitude boundary layer during accelerated flow events

Measurements made with the Fast Plasma Experiment on ISEE 1 and 2 reveal that accelerated beams of cold (1-30 eV for H/+/) ions are present sporadically on reconnected field lines within the low latitude boundary layer (LLBI). H(+) normally is the major constituent of these beams, but He(+) and O(+) are also occasionally detected in variable concentrations. Because of the low temperatures and the compositional makeup of these beams, the ionosphere must ultimately be the source of these ions. Observed beam speeds (between 120 and 250 km/s) are always less than that of the magnetosheath ions which penetrate into the LLBL on reconnected field lines, but both ion populations share the same E x B convective drift. Analysis reveals that reflection at the magnetopause cannot be the mechanism accelerating these ions. A more likely possibility is that the ions are accelerated primarily by the large transverse drift of recently reconnected field lines.

Gosling, J. T.↗

NASA NTRS1990

ISEE observations of low frequency waves and ion distribution function evolution in the plasma sheet boundary layer

This paper describes ISEE plasma and magnetic fluctuation observations during two crossings of the plasma sheet boundary layer (PSBL) in the earth's magnetotail. Distribution function observations show that the counterstreaming ion components undergo pitch-angle scattering and evolve into a shell distribution in velocity space. This evolution is correlated with the development of low frequency, low amplitude magnetic fluctuations. However, the measured wave amplitudes are insufficient to accomplish the observed degree of ion pitch-angle scatttering locally; the near-earth distributions may be the result of processes occurring much farther down the magnetotail. Results show a clear correlation between the ion component beta and the relative streaming speed of the two components, suggesting that electromagnetic ion/ion instabilities do play an important role in the scattering of PSBL ions.

Elphic, R. C.↗

NASA NTRS1990

Observations of the density profile in the magnetosheath near the stagnation streamline

An enhancement in the plasma density occurs in more than half of the ISEE-1 and 2 magnetosheath passes near the stagnation streamline just in front of the magnetopause. On average, this structure is about 0.4 R(e) thick and clearly separated from the magnetopause. The average density enhancement is about 44 percent above the ambient magnetosheath density. The anticorrelation of the magnetic field and density is that expected for the MHD slow mode. Strong fluctuations in the density within the structure are usually accompanied by fluctuations in velocity.

Song, P.↗

NASA NTRS1990

On the structure of the tail magnetic field

The configuration of the magnetic field in the Earth's geomagnetic tail is studied. The results in the lobe region and in the plasma sheet boundary layer region are compared. A systematic enhancement of the By component of the field is detected in the plasma sheet boundary layer with respect to the lobe; this enhancement leads to a lower rate of flaring of the magnetic field lines in the lobe with respect to the plasma sheet boundary layer. This observation is a signature of field aligned currents at the boundary. The direction of such field aligned currents agrees with the nightside region two current system.

Candidi, M.↗

NASA NTRS1990

Plasma flow reversals at the dayside magnetopause and the origin of asymmetric polar cap convection

Events observed in a fast plasma experiment, where the y-component of the plasma flow within the low latitude boundary layer and magnetopause current layer was oppositely directed to that in the adjacent magnetosheath, are examined. The observations are shown to be qualitatively and quantitatively consistent with previous observations of accelerated flows at the magnetopause and with models of magnetic reconnection, with reconnection occurring at low latitudes near the GSE XY plane, independently of the magnitude or the sign of the y-component ot the local magnetosheath magnetic field. Local magnetic shears at the magnetopause for these events (in 60-180 deg range) and the fact that these events occur at low latitudes do not support the antiparallel merging hypothesis. The observations of B(y)-dependent flow reversals demonstrate how the asymmetric polar cap convection and related phenomena, such as the Svalgaard-Mansurov effect, originate in magnetic reconnection at the dayside magnetopause.

Gosling, J. T.↗

NASA NTRS1990

Structure and properties of the subsolar magnetopause for northward IMF - ISEE observations

This paper describes the structure and the magnetic-field, electric-field, and plasma properties of the ISEE-1 magnetopause crossing on November 5, 1978, which occurred near the subsolar point when the IMF was strongly northward. It was found that the magnetopause was composed of three layers: (1) a sheath transition layer, in which there is a gradual density decrease without a change in temperature and which occurs totally within the magnetosheath plasma; (2) an outer boundary layer, which is dominated by magnetosheath particles; (3) and an inner boundary layer dominated by magnetospheric particles. No significnt heating or cooling was seen across the magnetopause during this crossing. The plasma within each of the layers was quite uniform, and their boundaries were sharp, suggesting that there was very little diffusion present.

Song, P.↗

NASA NTRS1990

Reconnection versus Kelvin-Helmholtz instability in magnetospheric energy transfer - ISEE observations

Examination of multiple magnetopause crossings observed with the magnetometers on ISEE 1 and 2 makes it possible to determine the amplitude of the oscillation of surface waves on the magnetopause with periods greater than about 2 min and its dependence on latitude, local time, and the direction of the IMF. The magnetopause is more oscillatory for southward IMF than for northward IMF. When the IMF is southward, the amplitude of the oscillation increases with increasing angle from the subsolar point, which suggests that reconnection-related phenomena can generate surface waves on the magnetopause. When the IMF is northward, the oscillation does not grow with distance from the subsolar point, which is contrary to the expected growth of the Kelvin-Helmholtz (K-H) instability. It is also found that solar-wind pressure fluctuations may cause all of the observed boundary oscillations for northward IMF.

Song, PU↗