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  • 1
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    The efficiency of 'viscous interaction' between the solar wind and the magnetosphere during intense northward IMF events (1995)
    In:  Other Sources
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    Publication Date: 2011-08-24
    Description: We examined 11 cases when the interplanetary magnetic field (IMF) was intensely northward (greater than 10 nT) for long durations of time (greater than 3 hours), to quantitatively determine an uppler limit on the efficiency of solar wind energy injection into the magnetosphere. We have specifically selected these large B(sub N) events to minimize the effects of magnetic reconnection. Many of these cases occurred during intervals of high-speed streams associated with coronal mass ejections when viscous interaction effects might be at a maximum. It is found that the typical efficiency of solar wind energy injection into the magnetosphere is 1.0 x 10(exp -3) to 4.0 x 10(exp -3), 100 to 30 times less efficient than during periods of intense southward IMFs. Other energy sinks not included in these numbers are discussed. Estimates of their magnitudes are provided.
    Keywords: GEOPHYSICS
    Type: Geophysical Research Letters (ISSN 0094-8276); 22; 6; p. 663-666
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  • 2
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    The causes of geomagnetic storms during solar maximum (1994)
    In:  Other Sources
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    Publication Date: 2011-08-24
    Description: One of the oldest mysteries in geomagnetism is the linkage between solar and geomagnetic activity. In investigating the causes of geomagnetic storms occurring during solar maximum, the following topics are discussed: solar phenomena; types of solar wind; magnetic reconnection and magnetic storms; an interplanetary example; and future space physics missions.
    Keywords: GEOPHYSICS
    Type: EOS (ISSN 0096-3941); 75; 5; p. 49, 51-53
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  • 3
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    Periodic variation in the geomagnetic activity - A study based on the Ap index (1993)
    In:  Other Sources
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    Publication Date: 2011-08-24
    Description: The monthly and daily samples of the Ap index for the interval from 1932 through 1982 were studied using the power spectrum technique. Results obtained for Bartel's period (about 27 days), the semiannual period, the dual-peak solar cycle distribution of geomagnetic storms, and certain other medium-scale periodicities are examined in detail. In addition, results on the cumulative occurrence number of storms per decade as a function of the Ap and Dst indices for the storm are presented.
    Keywords: GEOPHYSICS
    Type: Journal of Geophysical Research (ISSN 0148-0227); 98; A6; p. 9215-9231.
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  • 4
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    Comment on 'Geomagnetic activity associated with earth passage of interplanetary shock disturbances and coronal mass ejections' by J. T. Gosling, D. J. McComas, J. L. Philips, and S. J. Bame (1993)
    In:  Other Sources
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    Publication Date: 2011-08-24
    Description: It is contended that statistical data do not support the claim of Gosling et al. (1991) to the effect that the initial speed of a solar wind driver gas close to the sun appears to be the most crucial factor in determining if an earthward direct event will be effective in exciting a large geomagnetic disturbance. It is argued that the time intervals are much too large to observe the storm-time B sub Z dependence. Gosling et al. reply that this comment is based on a serious misunderstanding of their conclusions.
    Keywords: GEOPHYSICS
    Type: Journal of Geophysical Research (ISSN 0148-0227); 98; A2; p. 1507, 1508; Reply
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  • 5
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    Great magnetic storms (1992)
    In:  Other Sources
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    Publication Date: 2011-08-24
    Description: The five largest magnetic storms that occurred between 1971 to 1986 are studied to determine their solar and interplanetary causes. All of the events are found to be associated with high speed solar wind streams led by collisionless shocks. The high speed streams are clearly related to identifiable solar flares. It is found that: (1) it is the extreme values of the southward interplanetary magnetic fields rather than solar wind speeds that are the primary causes of great magnetic storms, (2) shocked and draped sheath fields preceding the driver gas (magnetic cloud) are at least as effective in causing the onset of great magnetic storms (3 of 5 events) as the strong fields within the driver gas itself, and (3) precursor southward fields ahead of the high speed streams allow the shock compression mechanism (item 2) to be particularly geoeffective.
    Keywords: GEOPHYSICS
    Type: Geophysical Research Letters (ISSN 0094-8276); 19; 73-76
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  • 6
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    Comment on 'A new method of forecasting geomagnetic activity and proton showers' by A. Hewish and P.J. Duffet-Smith (1988)
    In:  Other Sources
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    Publication Date: 2011-08-19
    Keywords: GEOPHYSICS
    Type: Planetary and Space Science (ISSN 0032-0633); 36; 205
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  • 7
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    Statistical properties of magnetic field fluctuations in the distant plasmasheet (1987)
    In:  Other Sources
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    Publication Date: 2011-08-19
    Description: Short (less than 1 min) and long time (greater than 5 min) variations of the plasmasheet magnetic field have been examined during all intervals when ISEE-3 was at distances x less than -200 earth radii. It is determined that short period magnetic turbulence increases by a factor of about 3 with increasing geomagnetic activity, as indicated by AE. In contrast, long period field variations with North-then-South signatures at plasmasheet entry occur about 2.5 times more frequently than South-then-North signatures. This result, combined with other previous ISEE-3 results, is in agreement with the interpretation that the North-South plasmasheet features are plasmoids propagating tailward. However, a statistical examination of the geomagnetic activity relationship indicates that there does not appear to be any substorm dependence on these North-South events.
    Keywords: GEOPHYSICS
    Type: Planetary and Space Science (ISSN 0032-0633); 35; 289-293
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  • 8
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    Distant (200-238 earth radii) magnetotail lobe characteristics during quiet solar wind conditions (1987)
    In:  Other Sources
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    Publication Date: 2011-08-19
    Description: Simultaneous ISEE-3 magnetic field and IMP-8 magnetic field and plasma data have been used to investigate the distant tail lobe average properties under quiet solar wind conditions. Under solar wind pressures of not greater than 5 x 10 to the -10th dynes/sq cm, an average tail lobe strength of 7.1 + or - 1.2 nT, and an average plasma beta of 0.3, are found. Results suggest that under quiet solar wind conditions the distant tail lobes are relatively free from plasma and are usually dominated by the magnetic field pressure.
    Keywords: GEOPHYSICS
    Type: Planetary and Space Science (ISSN 0032-0633); 35; 285-288
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  • 9
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    Criteria of interplanetary parameters causing intense magnetic storms (Dst of less than -100 nT) (1987)
    In:  Other Sources
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    Publication Date: 2011-08-19
    Description: An analysis of ISEE-3 field and plasma data shows that 10 intense magnetic storms that occurred in 1979 were caused by long-duration, large-amplitude (13-30 nT) and negative (less than -10 nT) IMF Bz events associated with interplanetary duskward-electric fields of greater than 5 mV/m. The results suggest that these criteria may be used as predictors of intense storms. A study of opposite polarity (northward) Bz events with the same criteria shows that their occurrence is similar both in number and in their relationship to interplanetary disturbances. The amplitudes of the storms were not found to vary with shock strengths.
    Keywords: GEOPHYSICS
    Type: Planetary and Space Science (ISSN 0032-0633); 35; 1101-110
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  • 10
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    The cause of high-intensity long-duration continuous AE activity (HILDCAAS) - Interplanetary Alfven wave trains (1987)
    In:  Other Sources
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    Publication Date: 2011-08-19
    Description: It is shown that high intensity (AE of greater than 1,000 nT), long duration (T of greater than 2d) continuous auroral activity events are caused by outward (from the sun) propagating interplanetary Alfven wave trains. The Alfven waves are often (but not always) detected several days after major interplanetary events, such as shocks and solar wind density enhancements. Presumably, magnetic reconnection between the southward components of the Alfven wave magnetic fields and magnetospheric fields is the mechanism for transfer of solar wind energy to the magnetosphere.
    Keywords: GEOPHYSICS
    Type: Planetary and Space Science (ISSN 0032-0633); 35; 405-412
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