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At least 883 records · Page 49

Core plasma in the magnetosphere

The paper presents a review of new findings related to core plasma (which includes ions and electrons with energies less than 50 eV) identified in studies of magnetosphere during 1983-1986. These findings include the cleft ion fountain; the plasmaspheric heavy ion torus; core molecular ions; high core-plasma densities in the plasma-sheet boundary layer; intense transverse heating of core plasmas in the equatorial regions; the supersonic polar wind (H/+/ and He/+/); toroidal or ring heavy-ion distribution functions in the auroral region; conic-to-field-aligned ion signatures of inverted-V auroral events; and the large-scale electron density structure of the magnetosphere. The progress made on modeling core plasma includes simulation of thermal helium heating at the equator; kinetic models of the plasma transport from localized ionospheric regions; time-dependent hydrodynamic models of the polar wind and plasmasphere-ionosphere coupling; and kinetic models of plasmasphere refilling.

Horwitz, J. L.↗

The magnetospheres of Jupiter, Saturn, and Uranus

The results published by U.S. scientists during 1983-1986 from studies related to the magnetospheres of Jupiter, Saturn, and Uranus are discussed. Consideration is given to the magnetic fields of these planets, charged particle environments, the interactions between the planetary rings and planetary satellites, the solar wind interactions, radio emissions, and auroras. Special attention is given to observations of (1) a small flux of energetic electrons and protons in the otherwise radiation-free environment in the magnetosphere under the rings of Saturn (interpreted as interactions of Galactic cosmic rays with the rings), (2) spokes, and (3) Saturn ring erosion.

Connerney, J. E. P.↗

The magnetosphere of Saturn

Pioneer 11 and Voyager 1 and 2 magnetic field measurements over the entire flyby of Saturn's magnetic field have been analyzed by fitting a magnetospheric dipole field (i.e., a dipole field plus the field due to currents in the magnetopause), higher moments of the internal field aligned with the dipole along the rotation axis, and the field due to an equatorial sheet current to the magnetic measurements. A dipole moment of 21,431 nT R(s) exp 3, a quadrupole moment of 2403 nT R(s) exp 4, an octopole moment of 2173 nT R(s) exp 5, and an equatorial sheet current of half thickness 2.0 R(s) from about 5 R(s) to the solar edge of the magnetopause, fit the measurements over the entire magnetosphere with an rms deviation of 3.2 nT where R(s) is the planet radius, 66,330 km. The primary feature of the present analysis is the explicit inclusion of the calculated magnetopause current field, which reduces the overall rms deviation over the entire flyby from sigma values of 4.7 and 5.9 nT, using previous models, to 3.2 nT using the present.

Beard, David B.↗

An extended study of the low-latitude boundary layer on the dawn and dusk flanks of the magnetosphere

The characteristics and structure of the low-latitude boundary layer (LLBL) have been studied for 66 ISEE 1 passes through the LLBL region. The dawn and dusk LLBL are on closed magnetic field lines for northward magnetosheath and/or IMF (M/IMF), and are on both closed and open field lines for southward M/IMF. For southward M/IMF, the regions of open LLBL field lines lie adjacent to the magnetopause and outside the closed LLBL. The LLBL is thicker (thinner) for northward (southward) M/IMF. With distance away from the subsolar magnetosphere, the LLBL becomes thicker for northward M/IMF and more variable in thickness for southward M/IMF. No dependence of LLBL thickness or electric field on geomagnetic activity is seen in these data. The LLBL electric field is a few millivolts per meter with a apparent upper limit of about 10 mV/m. The field captures magnetospherically drifting particles and propels them tailward.

Mitchell, D. G.↗

Radial force balance within Jupiter's dayside magnetosphere

A local field stress technique, developed previously in a study of the Saturnian magnetosphere, is introduced to the problem of determining the radial force balance characteristics of Jupiter's magnetosphere. The near-equatorial, radial magnetic force densities are estimated using the data obtained by Voyager 1 principally on the dayside (inbound) portion of its trajectory. Using the low-energy charged particle data (greater than about 30 keV) and other published data, ways in which the field forces might be balanced are explored. Inside 22 Jupiter radii, the magnetic radial forces match, in both magnitude and radial variation, the hot particle pressure gradient forces, assuming a mix of H(+) and O(n+) ions. Outside 22 Jupiter radii, a previously reported force balance problem is confirmed qualitatively, and two possible solutions are suggested.

Mauk, B. H.↗

Magnetosphere, exosphere, and surface of Mercury

It is presently suggested in light of the atomic Na exosphere discovered for Mercury that this planet, like the Jupiter moon Io, is capable of maintaining a heavy ion magnetosphere. Na(+) ions from the exosphere are in this scenario accelerated to keV energies en route to making substantial contributions to the mass and energy budgets of the magnetosphere. Since Mercury's Na supply to the exosphere is primarily internal, it would appear that Mercury is losing its semivolatiles and that this process will proceed by way of photosputtering, which maintains an adequate Na-ejection rate from the planet's surface.

Cheng, A. F.↗

A boundary layer model for magnetospheric substorms

An alternative framework for understanding magnetospheric substorm activity is presented. It is argued that observations of magnetic field and plasma flow variations in the magnetotail can be explained in terms of the passage of the plasma sheet boundary layer over the satellite detecting the tail signatures. It is shown that field-aligned currents and particle acceleration processes on magnetic field lines threading the ionospheric Harang discontinuity lead to the distinctive particle and field signatures observed in the magnetotail during substorms. It is demonstrated that edge effects of field-aligned currents associated with the westward traveling surge can lead to the negative B(z) perturbations observed in the tail that are presently attributed to observations made on the anti-earthward side of a near-earth neutral line. Finally, it is shown that the model can provide a physical explanation of both the driven system and the loading-unloading system whose combined effects provide the observed substorm perturbation pattern in the magnetosphere and ionosphere.

Rostoker, Gordon↗

Comment on 'Magnetospheric origin of energetic (E greater than or equal to 50 keV) ions upstream of the bow shock: The October 31, 1977, event' by G. C. Anagnostopoulos, E. T. Sarris, and S. M. Krimigis

Observational data on the effects of the solar burst event of October 31, 1977 on the earth bow shock are reassessed in a critical examination of the hypothesis of Anagnostopoulos et al. (1986), that energetic ions detected upstream of the shock originated in the magnetosphere and then leaked into the upstream region. The upstream and magnetospheric observations are compared, and consideration is given to the proton energy spectrum, anisotropies, and connection time. It is found that the event in question can best be explained in terms of Fermi shock acceleration. In a reply by Anagnostopoulos et al., additional data on this and similar events are presented in extensive graphs and analyzed. It is argued that there are many observed phenomena which cannot be explained by Fermi acceleration but are consistent with upstream leakage.

Ellison, Donald C.↗

Plasma instabilities in the terrestrial magnetosphere - A review of recent theoretical research

This paper reviews recent theoretical research on plasma instabilities in the terrestrial magnetosphere. This paper is organized with respect to particle free energies: electron-ion currents, electron beams, ion beams, electron anisotropies and ion anisotropies are successively considered. For each free energy, the associated instability properties are summarized, and their applications to magnetospheric physics are briefly described. Theory and simulations which have established close correlations with observations are emphasized.

Gary, S. Peter↗

Survey of electrons in the Uranian magnetosphere - Voyager 2 observations

Results of an analysis of the Voyager 2 plasma-science-experiment electron measurements made during the Uranus encounter are presented. The energy coverage is in the range of 10 to 5950 eV. The large day-night asymmetry together with the spin axis alignment with the solar direction and the large tilt of the planetary magnetic dipole suggest that solar-wind-driven time-dependent magnetospheric convection will be an important transport mechanism within the Uranian magnetosphere. The steady state convection time of the plasma is estimated to be between 1 and 3 days.

Sittler, Edward C., Jr.↗

The hot plasma and radiation environment of the Uranian magnetosphere

A detailed account is given of the results of the Voyager 2 low-energy charged particle investigation of the Uranian magnetosphere. Data show that the encounter of the inbound bow shock was immediately preceded by intense upstream proton events characterized by bulk streaming pointing approximately tangentially to the magnetospheric boundaries. Observations are presented which suggest that substorm processes analogous to those occurring within the earth's magnetotail are occurring within the Uranian magnetotail.

Mauk, B. H.↗

Self-excitation of auroral arcs in a three-dimensionally coupled magnetosphere-ionosphere system

This paper presents the first full three-dimensional dynamic simulation of auroral arc formation. The magnetospheric and ionospheric dynamics are represented by one-fluid magnetohydrodynamic equations and two-fluid weakly ionized plasma equations, respectively. The feedback coupling between magnetospheric Alfven waves and ionospheric density waves results in a spontaneous generation of longitudinally elongated striations of field-aligned currents and ionospheric electron densities, which compare very well with many features of quiet auroral arcs.

Watanabe, Kunihiko↗

Remarks on the MHD problem of generic magnetospheres and magnetotails

An understanding of the plasma physics problem of MHD flow around a magnetized sphere or cylinder in different Reynolds number regimes is shown to be crucial to magnetospheric and magnetotail studies. A significant amount of knowledge can be acquired from experimental and computational hydrodynamic precedents. It is believed that highly symmetric laminar models of the magnetosphere and magnetotail are unlikely in view of the high Reynolds numbers involved.

Montgomery, D.↗

A magnetospheric simulation at the Space Station

It is proposed that a strong magnet (terrella) be flown at or near the Space Station to create an artificial magnetosphere in a laboratory setting. The relative flow of the ionosphere past the terrella will constitute a plasma wind that will interact with the magnetic field of the terrella to produce a localized magnetosphere. This object could then be extensively studied using diagnostic probes attached to the Space Station or with free flyers. The space and storage requirements would be minimal, since the experiment would be conducted outside the Space Station. The total equipment would consist of several terrella (with varying surface conductivities), approximately 3 small magnetometer/plasma diagnostic packages, and several gas canisters for upstream seeding. Power requirements would be approximately 60 watts. Several track mounted tethers, each approximately or 200 m long in length, with track parallel to the orbital motion and 100 m long, are also needed. Astronaut time needed would be minimal in the tethered configuration (approximately 4 man hours/week). A free flying configuration, while not needing the tether track, would require much more human interaction.

Lopez, R. E.↗

Relativistic magnetospheric electrons: Lower ionospheric conductivity and long-term atmospheric variability

Long term observations of relativistic electrons in the earth's outer magnetosphere show a strong solar cycle dependence with a prominent intensity maximum during the approach to solar minimum. This population therefore closely corresponds to the presence of high speed solar wind streams emanating from solar coronal holes. Using a numerical code, the precipitating electron energy deposition in the earth's upper and middle atmosphere were calculated. Observed events (typically persisting several days) would have maximum effect in the 40 to 60 km altitude range with peak energy depositions greater than 110 keV/cu cm-s. It is suggested that this electron population could play an important long term role in modulating lower D region ionization and middle atmospheric ozone chemistry. Methods are described of observing middle atmospheric and lower ionospheric effects of the electrons including balloon, riometer, and space-based ozone sensor systems. A particularly promising approach may involve the monitoring of global Schumann resonance modes which are sensitive to global changes in the properties of the earth-ionosphere cavity. Present work indicates that Schumann resonance properties are moderately correlated with the flux of precipitating relativistic electrons thus offering the possibility of continuously monitoring this aspect of magnetosphere-atmosphere coupling.

Baker, D. N.↗

Stationary auroral current oscillations resulting from the magnetospheric generator

The origin of the steady state spatial current oscillations in the auroral field-aligned currents, which was detected in the measurements by the two Dynamics Explorer (DE) satellites DE 1 and DE 2, is explained in the framework of a simple steady state model of the magnetosphere-ionosphere current system. The model has only three parameters, including the magnetic-field-aligned conductivity, the ionospheric height-integrated Pedersen conductivity, and the conductivity of a generator or dynamo at the magnetospheric equator. Good agreement between this model and the measurements from the DE satellites was obtained.

Weimer, D. R.↗

Simultaneous energetic particle observations at geostationary orbit and in the upstream solar wind - Evidence for leakage during the magnetospheric compression event of November 1, 1984

The issue of accelertion and transport of particles in the upstream solar wind was investigated using the energetic ion and electron observations obtained simultaneously by three fortuitously positioned geostationary spececraft during a strong magnetospheric compression event of November 1, 1984. This compression event brought the subsolar magnetopause inward of the synchronous orbit. Data obtained indicate that, in the November 1 event, the process of magnetospheric ion escape was a very likely source for energetic particles both in the magnetosheath and the upstream solar wind.

Baker, D. N.↗

A predicted Triton plasma torus in Neptune's magnetosphere

The possibility of the formation of a plasma torus generated by the satellite Triton in the magnetosphere of Neptune is investigated. A set of coupled differential equations is solved that describe the evolution of material sputtered from the surface of atmosphere of Triton in the conditions likely to exist in an assumed Neptunian magnetosphere for various combinations of nitrogen and methane that may exist on Triton. The model assumes a mechanism for transport that gives upper limits for predicted torus concentrations. It is concluded that a successful detection of plasma by the Voyager Plasma Science instrument may be possible and could be an important source of information about the composition of Triton's surface and atmosphere.

Delitsky, Mona L.↗