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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
    Format: text
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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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    Characteristics of the magnetospheric source of interplanetary energetic particles (1984)
    In:  Other Sources
    Details
    Publication Date: 2011-08-18
    Description: The Earth's bow shock is frequently cited as an example of an astrophysical shock where particle acceleration is observed. However, because energetic particles observed upstream of the bow shock may be accelerated within the magnetosphere, it is important to understand the properties of the magnetospheric source. A first order picture of the spatial distribution of magnetospheric particles in the magnetosheath and upstream is obtained by mapping those magnetic field lines which drape over the magnetopause through the bow shock. Subsets of these field lines that connect to potential sites of magnetic merging on the magnetopause are also traced in the event that leakage occurs preferentially where normal components of the field are present across the boundary. The results can be used to determine whether the so-called diffuse particles observed upstream are accelerated locally or within the magnetosphere.
    Keywords: SPACE RADIATION
    Type: Neilsen Eng. and Res., Inc. Appl. of A Global Solar Wind/Planetary Obstacle Interaction Computational Model 18p (SEE N84-26509 16-88)
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  • 4
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    The magnetic field of Mars: Implications from gasdynamics modeling (1984)
    In:  Other Sources
    Details
    Publication Date: 2019-06-28
    Description: On January 21, 1972 the Mars-3 spacecraft observed a variation in the magnetic field during its periapsis passage over the dayside of Mars that was suggestive of entry into a Martian magnetosphere. The original data and trajectory have been obtained to simulate the observed variation of the magnetic field using gasdynamics. In the gasdynamic model, a flow field is first generated and then this flowfield is used to carry the interplanetary magnetic field through the Martian magnetosheath. The independence of the flow field and magnetic field calculation allows rapid convergence on an IMF orientation which would result in a magnetic variation similar to that observed by Mar-3. There appears to be no need to invoke an entry into a Martian magnetosphere to explain these observations.
    Keywords: SPACE RADIATION
    Type: Neilsen Eng. and Res., Inc. Appl. of A Global Solar Wind/Planetary Obstacle Interaction Computational Model 24p (SEE N84-26509 16-88)
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  • 5
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    Whistler mode wave propagation in the solar wind near the bow shock (1981)
    In:  Other Sources
    Details
    Publication Date: 2019-06-28
    Description: The presence of whistler mode waves in, and upstream from, the bow shock has been well established by observation. Theoretical descriptions of the mode under solar wind conditions have been relatively meagre, however, and it may not be generally appreciated how readily whistler waves generated in the shock could occupy most of the region ahead of the shock most of the time. Graphic descriptions of phase and group velocities and group velocity directions for typical solar wind parameters are presented by using the cold plasma approximation over all appropriate frequencies and directions with respect to the IMF. The relations of whistler phase and group velocities to observations of a quasi-perpendicular shock crossing by ISEE are illustrated.
    Keywords: SPACE RADIATION
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  • 6
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    Particle acceleration at planetary bow shock waves (1982)
    In:  Other Sources
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    Publication Date: 2019-06-28
    Description: One property of the collisionless shocks that may be studied through a comparison of their behavior in a variety of plasma conditions at several different planets is the occurrence of MHD waves, associated with particle beams accelerated at these shocks and flowing backward to the sun. Mercury, Venus, earth and Jupiter observations of one of these wave classes show that (1) the empirical relationship between interplanetary field strength and wave frequency in the observer's rest frame is approximately true at all the planets considered, and (2) the observed frequencies are consistent with resonance with beams of ions of the same energy at each of the planets. This is, in turn, in keeping with the Sonnerup (1969) geometrical model of ion reflection at collisionless shocks. It is suggested that this ion acceleration mechanism may occur in astrophysical systems similar to the solar system, providing a source of acceleration for cosmic rays.
    Keywords: SPACE RADIATION
    Type: Nature; 295; Jan. 7
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  • 7
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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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  • 8
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    Orbital mapping of the lunar magnetic field. (1973)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: Examination of the lunar magnetic field as deduced from the orbital magnetometer data, with major emphasis on the general mapping of the lunar field over the orbit track of the Apollo 15 subsatellite. A detailed analysis of the data from a series of overflights of the Van de Graaff region at two different altitudes is also presented. This latter set of data makes it possible to determine the scale size of the region and the contrast between the remanent magnetization associated with the magnetic feature and its surroundings. The low altitude data from the Apollo 16 subsatellite, just prior to its impact into the lunar surface, are then examined. Data obtained while the moon was in the solar wind are used to construct a map which shows the lunar limb regions associated with the detection of limb compressions. This map is used to make qualitative inferences concerning the lunar remanent field in regions not covered by the contour maps.
    Keywords: SPACE SCIENCES
    Type: The Moon; 7; May-June
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  • 9
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    Power spectra of the interplanetary magnetic field near the earth (1972)
    In:  CASI
    Details
    Publication Date: 2019-06-27
    Description: Power spectra of the interplanetary magnetic field measured by near-earth satellites upstream from the earth's bow shock are free from terrestrial contamination provided the field at the satellite does not intersect the bow shock. Considerable spectral enhancement for the range of frequencies 0.01 to 1.00 Hz, due to turbulence caused by the shock, may occur if the field observed at the satellite intersects the shock. This turbulence occurs frequently in both the morning and afternoon quadrants. In the frequency band from 0.07 to 1 Hz, this noise decreases in amplitude with radial distance from the shock with an attenuation length of 4 R sub E.
    Keywords: SPACE SCIENCES
    Type: NSSDC-ID-68-014A-14-PM , NASA. Ames Res. Center Solar Wind; p 375-381
    Format: application/pdf
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  • 10
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    A study of waves in the earth's bow shock (1971)
    In:  CASI
    Details
    Publication Date: 2019-06-27
    Description: The perturbation vectors of waves up and downstream from the region of maximum compression in the bow shock were examined on OGO-5 under particularly steady solar wind conditions. The polarization of the upstream waves was RH, circular and of the downstream waves LH, elliptical in the spacecraft frame. By observing that the polarization of the waves remained unchanged as the shock motion swept the wave structure back and forth across the satellite three times in eight minutes, it was found that the waves were not stationary in the shock frame. A study of the methods of determining the shock normal indicates that the normal estimated from a shock model should be superior to one based upon magnetic coplanarity. The propagation vectors of the waves examined did not coincide with the shock model normal, the average magnetic field, or the plasma flow velocity. However, the major axis of the polarization ellipse of the downstream wave was nearly parallel to the upstream propagation vector.
    Keywords: SPACE SCIENCES
    Type: NASA-CR-127793 , PUBL-949
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