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  • 1
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    The particles and fields subsatellite magnetometer experiment (1972)
    In:  CASI
    Details
    Publication Date: 2005-11-30
    Description: A preliminary analysis of magnetometer data from Apollo 15 subsatellite is concluded. Remanent magnetization is a characteristic property of the moon, and the distribution is such that a complex pattern is produced. A mapping of the distribution is feasible with the present experiment. Lunar induction fields produced by transients in interplanetary magnetic field are detectable at satellite orbit. Magnetometer data will provide estimates of the latitude and longitude dependences of interior conductivity. The plasma void extends to some altitude below the satellite orbit and probably the lunar surface. Solar wind near the limbs is usually strongly disturbed.
    Keywords: SPACE SCIENCES
    Type: NASA. Manned Spaceflight Center Apollo 15 Prelim. Sci. Rept.; 9 p
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  • 2
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    Preliminary mapping of the lunar magnetic field (1972)
    In:  Other Sources
    Details
    Publication Date: 2011-08-16
    Description: Magnetic field measurements made with the Apollo 15 subsatellite established the existence of remanent magnetization over much of the Moon's surface. The major features of the structure of the measured remanent field are apparently associated with large craters, the most apparent detected to date being that in the vicinity of the Van de Graaff crater. A preliminary contour map of relative magnetic intensity was produced for a limited region of the Moon. A high resolution plot of the Van de Graaff region was constructed from vector data in an attempt to locate the source of the largest feature observed.
    Keywords: SPACE SCIENCES
    Type: Univ. Space Res. Assoc. High Pressure Phys. and Planetary Interiors; p 167-174
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  • 3
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    Solar cycle variation of interplanetary shocks, coronal mass ejections, and stream interactions observed at 0.7 AU (1995)
    In:  Other Sources
    Details
    Publication Date: 2019-04-02
    Description: A survey of the Pioneer Venus Orbiter (PVO) magnetometer and plasma data from 1979-1980, shows that the occurrence frequency of interplanetary shocks, coronal mass ejections (CMEs) and stream interactions observed at 0.7 AU exhibits a solar cycle variation. As previously found at 1 AU, the observed number of both interplanetary shocks and CMEs peaks during solar maximum (approximately 16 and approximately 27 per year, respectively) and reaches a low during solar minimum (approximately 0 and approximately 7 per year, respectively), in phase with the variation in smoothed sunspot number. The number of stream interactions observed varies in the opposite manner, having a minimum during solar maximum (approximately 15 per year) and a maximum during solar minimum (approximately 34 per year). The percentage of CMEs and stream interactions producing interplanetary shocks also varies during the solar-cycle and exhibits interesting behavior during the declining phase. While the number of CMEs observed during this phase is decreasing, the percentage of CMEs producing interplanetary shocks reaches a maximum. Also, while the number of stream interactions observed is increasing, but has not reached maximum during the declining phase, the percentage of stream interactions producing interplanety shocks is at a maximum.
    Keywords: SOLAR PHYSICS
    Type: Advances in Space Research (ISSN 0273-1177); 16; 9; p. (9)353
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  • 4
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    A bubblelike coronal mass ejection flux rope in the solar wind (1990)
    In:  Other Sources
    Details
    Publication Date: 2019-06-28
    Description: A resolution to the question of whether coronal mass ejections are loops or bubbles is proposed and applied to the geometrical analysis of a solar wind event detected at 1 AU by ISEE 1 and 3. The discontinuity orientations, the size determined by time of passage, and the magnetic cloud signature are fit into the topology of a flux rope loop distorted by expansion into a thick rope with comparable dimensions in both the ecliptic and meridional planes. The looped rope fills a bubblelike cavity, thus preserving both types of proposed coronal mass ejection geometries. Other interesting features of the data include an apparent separation by the rope core of bidirectionally streaming protons in the leading section from electrons in the trailing section, possible vortical flow within the magnetic cloud, and a well-defined filamentary structure behind the shock.
    Keywords: SOLAR PHYSICS
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  • 5
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    Interplanetary magnetic field enhancements in the solar wind Statistical properties at 1 AU (1985)
    In:  Other Sources
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    Publication Date: 2019-06-28
    Description: The present investigation is concerned with interplanetary magnetic field (IMF) enhancements which do not resemble any of the previously reported amplifications in the IMF. The magnetic field enhacements observed increase slowly at first and then more rapidly to a peak followed by a symmetrical decay. Interplanetary magnetic field enhacement observed by ISEE-3 on various dates are considered, giving attention to observations on June 5, 1979; September 8-9, 1980; February 5, 1981; and June 14-15, 1981. Interplanetary magnetic field enhancement observed with the aid of IMP-8 are also considered. A total of 45 events is found in surveying a 9-year period of magnetic field data.
    Keywords: SOLAR PHYSICS
    Type: Icarus (ISSN 0019-1035); 62; 230-243
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  • 6
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    Multiple spacecraft observations of interplanetary shocks: Characteristics of the upstream ULF turbulence (1983)
    In:  CASI
    Details
    Publication Date: 2019-06-28
    Description: All interplanetary shocks observed by ISEE-3 and either ISEE-1 or ISEE-2 or both in 1978 and 1979 are examined for evidence of upstream waves. In order to characterize the properties of these shocks it is necessary to determine accurate shock normals. An overdetermined set of equations were inverted to obtain shock normals, velocities and error estimates for all these shocks. Tests of the method indicate it is quite reliable. Using these normals the Mach number and angle were between the interplanetary magnetic field and the shock normal for each shock. The upstream waves were separated into two classes: whistler mode precursors which occur at low Mach numbers and upstream turbulence whose amplitude at Mach numbers greater than 1.5 is controlled by the angle of the field to the shock normal. The former waves are right hand circularly polarized and quite monochromatic. The latter waves are more linearly polarized and have a broadband featureless spectrum.
    Keywords: SOLAR PHYSICS
    Type: JPL Solar Wind Five; p 385-400
    Format: application/pdf
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  • 7
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    The solar wind interaction with Venus (1979)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: The Pioneer Venus orbiter reveals that Venus has a well developed bow shock like the Earth's but on that is significantly weaker than the Earth's shock. The location of the bow shock is highly variable, more so than would have been expected for an obstacle of essentially fixed size. The altitude of the ionopause is also highly variable in response to changes in the solar wind. In the ionosphere, the field is often low. However, on some orbits, very large fields are seen as low as 150 km, and on most dayside orbits, thin magnetic structures of flux ropes are observed. At night, large fields are often observed which vary from orbit to orbit. Venus has a much smaller intrinsic magnetic moment than expected from scaling the terrestrial moment.
    Keywords: SOLAR PHYSICS
    Type: ESA Magnetospheric Boundary Layers; p 231-239
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  • 8
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    A sub-Alfvenic solar wind - Interplanetary and magnetosheath observations (1982)
    In:  Other Sources
    Details
    Publication Date: 2019-06-28
    Description: During much of an approximately 5-hour period on November 22, 1979, plasma and field instruments on ISEE 3 measured a solar wind flow that was simultaneously supersonic and sub-Alfvenic (about 320 km/s) due to an abnormally low ion density (about 0.07 per cu cm). The nature of the disturbed flow adjacent to the magnetosphere is examined. This examination suggests that the earth's bow wave retained its shock-like character when the solar wind flow was sub-Alfvenic.
    Keywords: SOLAR PHYSICS
    Type: Journal of Geophysical Research; 87; Jan. 1
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  • 9
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    Association of low-frequency waves with suprathermal ions in the upstream solar wind (1979)
    In:  Other Sources
    Details
    Publication Date: 2019-06-27
    Description: Observations obtained upstream of the earth's bowshock with the LASL/MPI plasma instruments and the UCLA magnetometers on ISEE-1 and 2 have revealed a striking relationship between the presence of low-frequency fluctuations in solar wind density and field strength and the different types of distribution functions of upstream ions. Waves are absent when the ions have the beamlike distribution of the 'reflected' ions. Large-amplitude waves are present only in conjunction with the 'diffuse' ions, which are characterized by flat energy spectra and broad angular distributions. The waves are largely compressive, showing very good correlation between oscillations in magnetic field strength and plasma density.
    Keywords: SOLAR PHYSICS
    Type: Geophysical Research Letters; 6; Mar. 197
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  • 10
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    Dependence of the polar cusp on the north-south component of the interplanetary magnetic field. (1973)
    In:  Other Sources
    Details
    Publication Date: 2019-06-27
    Keywords: SPACE SCIENCES
    Type: NSSDC-ID-68-014A-13-PM , NSSDC-ID-68-014A-14-PM , NSSDC-ID-68-014A-17-PM , NSSDC-ID-68-014A-24-PM , Journal of Geophysical Research; 78; July 1
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