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Intriligator, D. S.

Publications and source records attributed to Intriligator, D. S..

At least 37 records · Page 2
All sourcesNASA NTRSDOE OSTI
NASA NTRS1985

Plasma measurements of the Pioneer Venus Orbiter in the Venus ionosheath - Evidence for plasma heating near the ionopause

A study of the angular spread of plasma fluxes detected in the Venus ionosheath is presented. It is shown that in the inner regions of the ionosheath, where the flux intensity is severely decreased with respect to solar wind values, the width of the azimuthal distribution of the local plasma is comparable to, or even larger than, that of the stronger fluxes measured in the outer ionospheath. The observed variation of the angular width suggests the existence of a source of heating near the ionopause but is not consistent with the overall cooling that would be expected if mass loading and charge exchange collisions were solely responsible for the interaction process at that boundary. Dissipative phenomene associated with local plasma turbulence processes seem to be required to account for the broad angular distributions seen near the ionopause.

Perez-De-tejada, H.↗
NASA NTRS1984

Wave-particle interactions in the Venus wake and tail

The first descriptions of combined tail measurements from the Pioneer Venus plasma analyzer, magnetometer, and plasma wave detector are presented. The analysis concentrates on those orbits which are representative of the first tail passage. Summary plasma analyzer parameters are used to show that waves occurring at the boundary of the magnetotail can be identified as Doppler-shifted ion acoustic oscillations. High-density plasma distributions in the magnetotail region usually appear to be non-Maxwellian at the highest time resolution. These distorted distribution functions are generally accompanied by enhanced plasma wave signals and magnetic field reversals indicative of electric currents. A different time for the spacecraft entrance into the magnetotail from that previously defined is identified. It is shown that the wave activity in the Venus tail appears similar to the broadband noise identified in the earth's tail, except that at Venus the levels are usually higher.

Intriligator, D. S.↗
NASA NTRS1984

Plasma and electric field measurements of the PVO in the Venus ionosheath

A study of the plasma and electric-field measurements of the PVO in the Venus ionosheath near the terminator region is presented. A drastic decrease of the particle-flux intensity measured with the plasma instrument is encountered in the inner ionosheath before the inbound crossing of the ionopause. The outer boundary of the region of weak plasma fluxes is consistent with the presence of a rarefaction wave as reported previously from the Mariner 5 (Bridge et at., 1967), Venera (Verigin et al., 1978) and PVO (Spenner et al., 1980) plasma measurements in the Venus wake. Near that boundary there are, in addition, appreciable changes in the electric field signals detected with the PVO electric-field detectors. These observations suggest the existence of local plasma-wave activity associated with turbulent flow conditions in that region.

Perez-De-tejada, H.↗
NASA NTRS1984

Solar-terrestrial research opportunities - A look to the future

Recent and proposed research programs and their impact on the understanding of solar-terrestrial interactions, the processes driving solar activity, and the propagation of the solar wind are outlined. The magnetospheres of the earth and major planets have been mapped and their interactions with the solar wind modeled. MHD activity has been identified as the driving force for stellar surface activity, and Pioneer data are permitting a mapping of the outer areas of the heliosphere. Further studies are required to understand solar magnetic field-earth magnetosphere, ionosphere-atmosphere interactions, the effects of solar heating on earth atmosphere ozone levels, and the effects of solar transient events on the earth atmosphere. The initiation of an International Geosphere-Biosphere Program is now under study and several satellites for solar-terrestrial research are under development as cooperative efforts among the U.S., Japanese, and European agencies.

Intriligator, D. S.↗
NASA NTRS1982

Compression of the Venusian ionosphere on May 10, 1979, by the interplanetary shock generated by the solar eruption of May 8, 1979

Previous solar optical and solar wind conditions observations are summarized, and Venus ionopause data taken with the Helios 2 and Pioneer Venus Orbiter spacecraft are presented for orbits 150-161. Those orbits encountered the results of an interplanetary shock wave initiated by a solar eruption and coronal transient of May 8, 1979. A significant compression of the dayside Venus ionosphere was detected two days later. The solar observations had been made in H-alpha at 10 solar radii, at 0.3 AU, and at 0.7 AU, using plasma and magnetometer monitoring of the shock wave.

Dryer, M.↗
NASA NTRS1982

First evidence for a Europa plasma torus

The evidence from the Pioneer 10 plasma analyzer that plasma derived from Europa was present in the Jovian magnetosphere in December 1973 is summarized. Plasma detected between 1900 UT and 2100 UT on December 3, 1973, reveals a number of significant phenomena near the expected position of Europa's L shell. Mass addition to the magnetospheric plasma is indicated by a local increase in density apparently superimposed on the density gradient of Iogenic plasma. This increase in plasma density is unlike any phenomenon observed when the spacecraft is near a lunar L shell. The density shows fluctuations that make possible an estimate of the net outflow speed of magnetospheric ions per Jovian rotation. A radial flow speed in 1973 of 0.37 km/s from the Pioneer data is made, together with an estimate of 1 km/s in 1979 from Voyager 2 data, thus indicating a significant change.

Intriligator, D. S.↗
NASA NTRS1982

Plasma turbulence in the downstream ionosheath of Venus

Observations made by the Pioneer Venus Orbiter plasma analyzer and the plasma wave instrument in the Venus ionosheath are compared. Large increases in plasma wave turbulence levels appear to be connected with changing plasma distributions and interpenetrating plasma beams. Some of these plasma waves are identified as Doppler - shifted ion acoustic waves due to beam/beam interactions, but it is noted that different forms of instabilities are probably also operative. The changes in the temperature, intensity and energy of the peak in the PVO plasma distributions are similar to those observed by Venera 10 closer to the planet and appear to be evidence for rarefaction and compression in the downstream ionosheath. Some of the changes in the PVO plasma distributions may be related to the presence of a second ion population or the acceleration of protons.

Intriligator, D. S.↗
NASA NTRS1982

Orientation of planetary O/plus/ fluxes and magnetic field lines in the Venus wake

The presence of 'contaminant' heavy ions of planetary origin in the solar wind has long been the subject of intense theoretical and experimental research. Studies of their abundance, acceleration, and direction of motion are important because of their implications on the composition and dynamics of planetary and cometary plasma wakes. The plasma and magnetic field observations made with the Pioneer Venus Orbiter (PVO) at Venus have provided the opportunity to examine the conditions in which planetary ions are picked up by the solar wind. We show here that in the outer regions of the Venusian far wake the displacement of planetary O(plus) particles, characteristic of the Venus upper ionosphere, does not occur necessarily along the magnetic field lines but approximately in the direction of the shocked solar wind.

Perez-De-tejada, H.↗
NASA NTRS1982

Observations of structuring in the downstream region of a large spherical model in a laboratory simulated solar wind plasma

The effects of inserting a spherical conducting model, large in comparison with the Debye length, into a free streaming high-energy 1 kV) unmagnetized hydrogen plasma are investigated in order to measure energies and compositions directly relevant to solar wind and astrophysical plasma phenomena. Holding the incident plasma parameters constant, transverse profiles of the net Langmuir probe current are plotted at various locations downstream in the model wake and are divided into three regions (the shadow, transition, and boundary). Results attributable to the use of a high-energy plasma show that enhancements in the shadow exist at downstream locations where the Mach ratio is less than one, and turbulence exists in the transition region on the shadow edges and outside in the boundary region. In addition, a small current enhancement is found in the boundary and can be attributed to the plasma/model interaction. It is concluded that many similar features observed by spacecraft downstream from planetary bodies are relatively permanent and are due to the intrinsic nature of the interaction between the solar wind plasma and the obstacle.

Intriligator, D. S.↗
NASA NTRS1982

Observations of mass addition to the shocked solar wind of the Venusian ionosheath

The present investigation constitutes a continuation of a study conducted by Mihalov et al. (1980) concerning the heavy ion component in the plasma observations downstream from Venus, taking into account data obtained with the aid of the plasma analyzer experiment on the Pioneer Venus Orbiter (PVO). The current study is based on analyses of the first season of PVO orbits with apoapsis in the tail and provides clear evidence for the presence of heavy ions. It is found that a heavy ion component was added to the ionosheath flow for a prolonged period on June 8 and 11, 1979 while the spacecraft was downstream from the planet. The heavy ions are identified as oxygen ions O(+). Heavy ions are detected on most of the orbits in the first season or apoapsis tail passages.

Intriligator, D. S.↗
NASA NTRS1982

Plasma shocks and energetic particles in the outer solar system - Trapping and asymmetry observations from Pioneer 10 and Pioneer 11

The April 15 and 28, 1978 solar flares appear to have 0.5-20 MeV protons trapped between a pair of shocks, and the large count rate enhancement observed, along with large ranges of radial distance and longitudinal angles, imply a prolongation of trapping for a period of weeks. The apparent ability of a shock whose plasma signature is faint to confine MeV protons in the outer solar system may have significant implications for cosmic ray studies. Analytical results also imply significant azimuthal asymmetry in plasma and energetic particle behavior, at distances as far as 16 AU from the sun. Combining these observations provides evidence for unexpectedly complex interactions in the outer solar system between energetic particles and solar wind plasma.

Intriligator, D. S.↗
NASA NTRS1982

Pioneer 10/11 data analysis of the plasma analyzer experiment

The Pioneer 10 plasma analyzer detected the 10 plasma torus. Evidence was found of corotating ions which appear to be primarily S (++) and O (++) in the Pioneer 10 plasma data as the spacecraft moved inward from 6.9 to 5.4 R sub J. The Pioneer plasma analyzer was effective in obtaining information on the heavy ion populations in the Jovian magnetosphere. Interplanetary solar wind plasma shocks can trap energetic particles (cosmic rays) for weeks and out to distances of 17 AU. Energetic particles (o.5 MeV to 20 MeV) were confined between two plasma shocks from solar flares as the shocks propagated outward in the solar system.

Intriligator, D. S.↗
NASA NTRS1981

Empirical model of the interaction of the solar wind with the daytime ionosphere of Venus

Interplanetary probe data on the interaction of the solar wind with the ionosphere of Venus are examined. It is shown that the ionospheric pressure above the ionopause is approximately equal to the dynamic pressure of the solar wind, while the value of magnetic pressure at the ionopause amounts to about 2/3 of the value of external and ionospheric pressures. A first-approximation model is proposed for changes of pressure at the ionopause as a function of height and solar zenith angle. This model makes it possible to determine the 'instantaneous' profile of the ionopause for a given solar-wind pressure.

Vaisberg, O. L.↗
NASA NTRS1980

Pioneer Venus plasma observations of the solar wind-Venus interaction

Collection of data from the Ames plasma analyzer on the Pioneer Venus orbiter has permitted long-term measurements of the interaction of the solar wind with Venus. The paper presents a mapping of the ionosheath flow field, plasma measurements in the distant ionosheath and near the distant plasma cavity, and a summary of observations of jumps in the solar wind proton parameters across Venus' bow shock. Also, the apparent detection of ionospheric O(+) accelerated up to solar wind speeds downstream in Venus' ionosheath is discussed.

Mihalov, J. D.↗
NASA NTRS1980

The solar wind interaction with Venus - Pioneer Venus observations of bow shock location and structure

Pioneer Venus observations are used in carrying out a study of the location and structure of the Venus bow shock. The trace of the shock in the solar wind aberrated terminator plane is almost circular at an altitude of 1.38 Venus radii independent of interplanetary magnetic field orientation with an extrapolated subsolar height of 0.38 Venus radii. Gas dynamic relations and scaling of the terrestrial analogue are used in determining the effective impenetrable obstacle altitude from the mean shock surface with the conclusion that it lies beneath the observed height of the ionopause. The short-term variability in shock position is similar to that found at the earth; over the long-term bow shock, altitude varies by up to approximately 35% in phase with the solar cycle for reasons other than changing solar wind Mach number. In contrast to ionopause position, which is shown to be well determined by external pressure measurements, it is found that bow shock altitude is only weakly dependent on ionopause height and solar wind dynamic pressure.

Slavin, J. A.↗
NASA NTRS1980

An empirical model of the Venusian outer environment. I - The shape of the dayside solar wind-atmosphere interface. II - The shape and location of the bow shock

Solar wind plasma and magnetic field data and ionospheric data obtained from the Pioneer Venus orbiter are discussed. The variation in the magnetic field pressure within the magnetic barrier is shown to be similar to that expected for the solar wind pressure variations along an obstacle's boundary when a more realistic approximation of the shape of the ionosphere is included. Simultaneous solar wind pressure, ionospheric pressure, and magnetic barrier pressure data reveal that the ionospheric pressure below the ionopause is approximately equal to the solar wind pressure. The magnetic barrier pressure is found to be equal to approximately 2/3 to 3/4 of both the solar wind pressure and the ionospheric pressure. Estimates of the hot plasma pressure contribution to the total pressure in the magnetic barrier vary from 1/4 to 1/3. Just below the ionopause the ionospheric pressure deviations from the mean ionospheric pressure are significant, especially below approximately 400 km; they appear to be indicative of the adjustment of the ionospheric structure to changeing solar wind conditions. A first-order model of the ionopause pressure variations as a function of height and solar-zenith angle is proposed. Venera 9 and Venera 10 bow shock crossings are then analyzed for solar zenith angles in the range from approximately 25 deg to approximately 153 deg. A comparison of Venera 9 and Venera 10 bow shock crossings with those observed by the Pioneer Venus orbiter suggests that both the secular variation and the latitudinal asymmetry may be responsible for the closer shock crossings of the Venera 9 and Venera 10 spacecraft.

Vaisberg, O. L.↗