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  • 1
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    Magnetic holes in the solar wind (1977)
    In:  Other Sources
    Details
    Publication Date: 2011-08-17
    Description: An analysis of high-resolution magnetic field measurements from the Goddard Space Flight Center magnetometer on Explorer 43 showed that low magnetic field intensities (less than 1 gamma) in the solar wind at 1 AU occur as distinct depressions, or 'holes', in otherwise nearly average conditions. These magnetic holes are new kinetic scale phenomena, having a characteristic dimension of the order of 20,000 km. They occurred at a rate of 1.5/d in the 18-day interval (March 18 to April 6, 1971) that was considered. Most magnetic holes are characterized by both a depression in /B/ and a change in the magnetic field direction, and some of these are possibly the result of magnetic merging. However, in other cases the direction, does not change; such holes are not due to merging but might be a diamagnetic effect due to localized plasma inhomogeneities.
    Keywords: SOLAR PHYSICS
    Type: Journal of Geophysical Research; 82; May 1
    Format: text
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  • 2
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    On the polarization state of hydromagnetic fluctuations in the solar wind (1981)
    In:  Other Sources
    Details
    Publication Date: 2011-08-18
    Description: From presently available observations one can infer that the Alfvenic turbulence measured in the solar wind, predominantly on trailing edges of high-speed streams, is a mixture of modes with two different polarizations, namely, Alfvenic modes and modes which are the incompressible limit of slow magnetosonic waves. Using Helios 2 magnetic data and a variance analysis, parallel (to the mean field) and perpendicular components of the fluctuations are separated, and the possible correlation between such components which would be predicted as a consequence of the incompressible character of the turbulence is studied. Correlations between eigenvalues of the variance matrix are also investigated and discussed.
    Keywords: SOLAR PHYSICS
    Type: Journal of Geophysical Research; 86; Mar. 1
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  • 3
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    Statistical properties of MHD fluctuations associated with high-speed streams from Helios-2 observations (1982)
    In:  Other Sources
    Details
    Publication Date: 2011-08-18
    Description: (Previously announced in STAR as N82-18117)
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 78; June 198
    Format: text
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  • 4
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    Magnetic dips in the solar wind (1979)
    In:  Other Sources
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    Publication Date: 2011-08-17
    Description: Using magnetic data from the Helios-1 fluxgate magnetometer, with a 0.2 s resolution, we have investigated the structure of several interplanetary discontinuities involving magnetic dips and rotations of the magnetic field vector. A minimum variance analysis illustrates the behaviour of the magnetic field through the transition. Using this analysis, quite different structures have been isolated and, in particular, narrow transitions resembling almost one dimensional reconnected neutral sheets. For the thinner cases (scale lengths of the magnetic rotation of the order or smaller than 1000 km), we find that the observed structures can be the nonlinear effect of a resistive tearing mode instability having developed on an originally one dimensional neutral sheet at the solar corona.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics; 62; May 1979
    Format: text
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  • 5
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    On the alignment of plasma anisotropies and the magnetic field direction in the solar wind (1977)
    In:  Other Sources
    Details
    Publication Date: 2011-08-17
    Description: One year's Imp 6 solar wind plasma and magnetic field data are examined to determine whether anisotropies in particle velocity distributions are aligned with the measured interplanetary magnetic field vector. Alignment of components in the analysis plane was generally found to be excellent whenever plasma parameter magnitudes were larger than determination uncertainties, although some spread exists (typical rms approximately equal to 10 deg). By assuming cylindrical symmetry about the simultaneously measured magnetic field vector during the 1-year interval under study, three-dimensional values of selected solar wind plasma thermal parameters were constructed from the two-dimensional plasma measurements, and the statistical properties of their distributions have been tabulated.
    Keywords: SOLAR PHYSICS
    Type: Journal of Geophysical Research; 82; Dec. 1
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  • 6
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    Magnetic fields and flows between 1 and 0.3 AU during the primary mission of Helios 1 (1978)
    In:  Other Sources
    Details
    Publication Date: 2011-08-17
    Description: Magnetic phenomena and coronal holes observed by Helios 1 during nearly four rotations of the sun are discussed. It is estimated that the magnetic field intensity of open field lines in some of the coronal holes (which changed in shape and latitude from one rotation to the next) was of the order of 10-20 G during the studied period, December 1974 to March 1975. Magnetic field polarity, cold magnetic enhancements, and longitudinal widths of the stream are described. It is concluded that between the sun and 0.3 AU there was a diverging stream surrounded by a thin boundary layer in which there was large velocity shear. There is evidence for compression of the magnetic field in the western boundary layer.
    Keywords: SOLAR PHYSICS
    Type: Journal of Geophysical Research; 83; Nov. 1
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  • 7
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    The large-scale magnetic field in the solar wind (1976)
    In:  CASI
    Details
    Publication Date: 2016-05-14
    Description: A literature review is presented of theoretical models of the interaction of the solar wind and interplanetary magnetic fields. Observations of interplanetary magnetic fields by the IMP and OSO spacecraft are discussed. The causes for cosmic ray variations (Forbush decreases) by the solar wind are examined. The model of Parker is emphasized. This model shows the three dimensional magnetic field lines of the solar wind to have the form of spirals wrapped on cones. It is concluded that an out-of-the-ecliptic solar probe mission would allow the testing and verification of the various theoretical models examined. Diagrams of the various models are shown.
    Keywords: SOLAR PHYSICS
    Type: Proc. of the Symp. on the Study of the Sun and Interplanetary Medium in Three Dimensions; p 143-165
    Format: application/pdf
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  • 8
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    On the polarization state of hydromagnetic fluctuations in the solar wind (1980)
    In:  CASI
    Details
    Publication Date: 2019-06-28
    Description: From presently available observations it can be inferred that the Alfvenic turbulence measured in the solar wind, predominantly on trailing edges of high speed streams, is a mixture of modes with two different polarizations, namely, Alfvenic modes and modes which are the incompressible limit of slow magnetosonic waves. Using Helios 2 magnetic data and a variance analysis, parallel (to the mean field) and perpendicular components of the fluctuations are separated and the possible correlation between such components is studied. Correlations between eigenvalues of the variance matrix are also investigated and discussed.
    Keywords: SOLAR PHYSICS
    Type: NASA-TM-82282 , LPS-80-9
    Format: application/pdf
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  • 9
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    Magnetic field hourly averages from the Rome-GSFC experiment aboard Helios 1 and Helio 2 (1987)
    In:  CASI
    Details
    Publication Date: 2019-06-28
    Description: Plots of all the hourly averages computed from the solar magnetic field measurements obtained during the mission are given separately for Helios 1 and Helios 2. The magnitude and the direction of the averaged field are plotted versus the number of solar rotations as seen from Helios, counted from launch.
    Keywords: SOLAR PHYSICS
    Type: NASA-TM-89782 , NAS 1.15:89782 , IFSI-87-1
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  • 10
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    The large-scale magnetic field in the solar wind (1975)
    In:  CASI
    Details
    Publication Date: 2019-06-27
    Description: A large-scale, three dimensional magnetic field in the interplanetary medium with an expected classical spiral pattern to zeroth order is discussed. Systematic and random deviations which are expected are treated. The sector structure which should be evident at high latitudes is examined. Interplanetary streams are discussed as determining the patterns of magnetic field intensity. It was proposed that the large-scale spiral field can induce a meridional flow which might alter the field geometry somewhat. The nonuniformities caused by streams will probably significantly influence the motion of solar and galactic particles. It was concluded that knowledge of the 3-dimensional field and its dynamical effects can be obtained by in situ measurements by a probe which goes over the sun's poles. Diagrams of the magnetic fields are given.
    Keywords: SOLAR PHYSICS
    Type: NASA-TM-X-70983 , X-692-75-242
    Format: application/pdf
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