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  • 1
    Online Resource
    Online Resource
    Magnetospheric plasma pressures in the midnight meridian: Observations from 2.5 to 35 R E
    American Geophysical Union (AGU) ; 1989
    In:  Journal of Geophysical Research Vol. 94, No. A5 ( 1989), p. 5264-
    Details
    In: Journal of Geophysical Research, American Geophysical Union (AGU), Vol. 94, No. A5 ( 1989), p. 5264-
    Type of Medium: Online Resource
    ISSN: 0148-0227
    URL: Article
    DOI: 10.1029/JA094iA05p05264
    Language: English
    Publisher: American Geophysical Union (AGU)
    Publication Date: 1989
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  • 2
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    Online Resource
    Utilizing the polar cap index to explore strong driving of polar cap dynamics : STRONG DRIVING OF POLAR CAP DYNAMICS
    American Geophysical Union (AGU) ; 2012
    In:  Journal of Geophysical Research: Space Physics Vol. 117, No. A7 ( 2012-07), p. n/a-n/a
    Details
    In: Journal of Geophysical Research: Space Physics, American Geophysical Union (AGU), Vol. 117, No. A7 ( 2012-07), p. n/a-n/a
    Type of Medium: Online Resource
    ISSN: 0148-0227
    URL: Article
    DOI: 10.1029/2011JA017087
    Language: English
    Publisher: American Geophysical Union (AGU)
    Publication Date: 2012
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  • 3
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    Simulating the effect of centrifugal forces in Jupiter's magnetosphere
    American Geophysical Union (AGU) ; 2014
    In:  Journal of Geophysical Research: Space Physics Vol. 119, No. 3 ( 2014-03), p. 1925-1950
    Details
    In: Journal of Geophysical Research: Space Physics, American Geophysical Union (AGU), Vol. 119, No. 3 ( 2014-03), p. 1925-1950
    Abstract: The centrifugal force accelerates particles during outward flux tube expansion Nonadiabatic flux tube expansion occurs at Jupiter between noon and dusk LT These effects can explain why Jupiter's plasma sheet thickens from 12 to 18 LT
    Type of Medium: Online Resource
    ISSN: 2169-9380 , 2169-9402
    URL: Issue
    URL: Article
    DOI: 10.1002/jgra.v119.3
    DOI: 10.1002/2013JA019381
    Language: English
    Publisher: American Geophysical Union (AGU)
    Publication Date: 2014
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  • 4
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    Magnetosphere‐ionosphere mapping at Jupiter: Quantifying the effects of using different internal field models
    American Geophysical Union (AGU) ; 2015
    In:  Journal of Geophysical Research: Space Physics Vol. 120, No. 4 ( 2015-04), p. 2584-2599
    Details
    In: Journal of Geophysical Research: Space Physics, American Geophysical Union (AGU), Vol. 120, No. 4 ( 2015-04), p. 2584-2599
    Abstract: There are three widely used internal Jovian magnetic field models We compare auroral mapping results using different field models Mapping results can be shifted by several degrees or tens of Jovian radii
    Type of Medium: Online Resource
    ISSN: 2169-9380 , 2169-9402
    URL: Issue
    URL: Article
    DOI: 10.1002/jgra.v120.4
    DOI: 10.1002/2014JA020729
    Language: English
    Publisher: American Geophysical Union (AGU)
    Publication Date: 2015
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  • 5
    Online Resource
    Online Resource
    Model field flux conservation and the beard magnetotail model: Two corrections
    American Geophysical Union (AGU) ; 1983
    In:  Journal of Geophysical Research: Space Physics Vol. 88, No. A7 ( 1983-07), p. 5784-5784
    Details
    In: Journal of Geophysical Research: Space Physics, American Geophysical Union (AGU), Vol. 88, No. A7 ( 1983-07), p. 5784-5784
    Type of Medium: Online Resource
    ISSN: 0148-0227
    URL: Article
    DOI: 10.1029/JA088iA07p05784
    Language: English
    Publisher: American Geophysical Union (AGU)
    Publication Date: 1983
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  • 6
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    Anomalous aspects of magnetosheath flow and of the shape and oscillations of the magnetopause during an interval of strongly northward interplanetary magnetic field
    American Geophysical Union (AGU) ; 1993
    In:  Journal of Geophysical Research: Space Physics Vol. 98, No. A4 ( 1993-04), p. 5727-5742
    Details
    In: Journal of Geophysical Research: Space Physics, American Geophysical Union (AGU), Vol. 98, No. A4 ( 1993-04), p. 5727-5742
    Abstract: On February 15, 1978, the orientation of the interplanetary magnetic field (IMF) remained steadily northward for more than 12 hours. The ISEE 1 and 2 spacecraft were located near apogee on the dawnside flank of the magnetotail. IMP 8 was almost symmetrically located in the magnetosheath on the dusk flank and IMP 7 was upstream in the solar wind. Using plasma and magnetic field data, we show that (1) the magnetosheath flow speed on the flanks of the magnetotail steadily exceeded the solar wind speed by 20%, (2) surface waves of ∼5‐min period and very nonsinusoidal waveform were persistently present on the dawn magnetopause and waves of similar period were present in the dusk magnetosheath, and (3) the magnetotail ceased to flare at an antisunward distance of 15 R E . We propose that the acceleration of the magnetosheath flow is achieved by magnetic tension in the draped field configuration for northward IMF and that the reduction of tail flaring is consistent with a decreased amount of open magnetic flux and a larger standoff distance of the subsolar magnetopause. Results of a three‐dimensional magnetohydrodynamic simulation support this phenomenological model.
    Type of Medium: Online Resource
    ISSN: 0148-0227
    URL: Article
    DOI: 10.1029/92JA02263
    Language: English
    Publisher: American Geophysical Union (AGU)
    Publication Date: 1993
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  • 7
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    Io and its plasma environment
    American Geophysical Union (AGU) ; 1980
    In:  Journal of Geophysical Research: Space Physics Vol. 85, No. A11 ( 1980-11), p. 5959-5968
    Details
    In: Journal of Geophysical Research: Space Physics, American Geophysical Union (AGU), Vol. 85, No. A11 ( 1980-11), p. 5959-5968
    Abstract: We describe and examine the interaction of Io with its plasma torus and the Jovian magnetic field in the context of several currently popular models. We address three specific matters. First, we discuss features implied by sub‐Alfvenic flow which must be common to all models. Next, we examine the magnetic signature observed near Io by the Goddard Space Flight Center Voyager 1 magnetometer and point out that the preliminary estimate of 5 × 10 6 A current may be an overestimate. We obtain good fits with alternative current distributions which yield currents as small as 7 × 10 5 A through Io. The best fits are obtained for an Alfven Mach number ( M A ) of 0.15, but good fits are also found for 0.1 〈 M A 〈 0.25. Lastly, we point out the crucial role of charged particle data for probing the near Io interaction. We use published data from the low energy charged particle (LECP) detector to suggest that Io has an intrinsic magnetic field of magnitude comparable with earlier estimates. We make predictions which can test this picture as further data become available.
    Type of Medium: Online Resource
    ISSN: 0148-0227
    URL: Article
    DOI: 10.1029/JA085iA11p05959
    Language: English
    Publisher: American Geophysical Union (AGU)
    Publication Date: 1980
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  • 8
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    Online Resource
    In situ observations of the “preexisting auroral arc” by THEMIS all sky imagers and the FAST spacecraft : THE PREEXISTING AURORAL ARC
    American Geophysical Union (AGU) ; 2012
    In:  Journal of Geophysical Research: Space Physics Vol. 117, No. A5 ( 2012-05), p. n/a-n/a
    Details
    In: Journal of Geophysical Research: Space Physics, American Geophysical Union (AGU), Vol. 117, No. A5 ( 2012-05), p. n/a-n/a
    Type of Medium: Online Resource
    ISSN: 0148-0227
    URL: Article
    DOI: 10.1029/2011JA017128
    Language: English
    Publisher: American Geophysical Union (AGU)
    Publication Date: 2012
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  • 9
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    A global magnetohydrodynamic simulation of the Jovian magnetosphere
    American Geophysical Union (AGU) ; 1998
    In:  Journal of Geophysical Research: Space Physics Vol. 103, No. A1 ( 1998-01), p. 225-235
    Details
    In: Journal of Geophysical Research: Space Physics, American Geophysical Union (AGU), Vol. 103, No. A1 ( 1998-01), p. 225-235
    Abstract: We have developed a three‐dimensional global magnetohydrodynamic simulation of the interaction between the solar wind and a rapidly rotating magnetosphere and applied it to Jupiter. For fixed solar wind dynamic pressure the rotating model Jovian magnetosphere extends farther toward the Sun and has greater extent in the east–west direction than a model without rotation but is little different in the north south direction. There is a pronounced dawn‐dusk asymmetry with the dawn magnetopause displaced farther from Jupiter. The middle Jovian magnetosphere contains a thin plasma sheet dominated by rotating plasmas. On the day side this plasma sheet thickens near the magnetopause. Near the dawnside magnetopause where rotating Jovian convection is opposed to the solar wind induced flow, a pressure ridge forms where the magnetospheric flow slows and forms a stagnation region. In the magnetotail the rotating flow is diverted tailward. For x 〈 −100 R J x‐type and o‐type neutral lines form. When the solar wind pressure was decreased, the boundaries moved away from Jupiter and the dayside field lines became stretched into a more tail‐like configuration. A flow vortex formed in the evening middle magnetosphere.
    Type of Medium: Online Resource
    ISSN: 0148-0227
    URL: Article
    DOI: 10.1029/97JA02247
    Language: English
    Publisher: American Geophysical Union (AGU)
    Publication Date: 1998
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  • 10
    Online Resource
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    Imaging the effect of dipole tilt on magnetotail boundaries
    American Geophysical Union (AGU) ; 1994
    In:  Journal of Geophysical Research: Space Physics Vol. 99, No. A4 ( 1994-04), p. 6079-6092
    Details
    In: Journal of Geophysical Research: Space Physics, American Geophysical Union (AGU), Vol. 99, No. A4 ( 1994-04), p. 6079-6092
    Abstract: Eight years of IMP 8, four years of ISEE 2, and one year of IMP 7 magnetometer data have been combined to produce an "image" of the average magnetic field for a YZ cross section (aberrated GSM) of the magnetotail at a downtail distance of 25 R E . The shape of the neutral sheet and magnetopause boundaries can be observed directly from the images. A fitting function that qualitatively matches the observed boundary shape can then be chosen. This approach improves on previous fits to possibly unsuitable functional forms specified independently of the data. In addition, as a refinement of previous studies, we have corrected for varying solar wind dynamic pressure and the effects of tail flaring. We find the magnetopause is displaced above the XY plane with increasing dipole tilt. The neutral sheet is found to curve slightly more than the model of Fairfield (1980) during times of large dipole tilt and near the flanks appears to differ substantially from the neutral sheet shape given by the analytic model of Voigt [1984], the more recent neutral sheet model of Dandouras (1988) based on the Voigt model, and the semi‐empirical model of Tsyganenko (1989).
    Type of Medium: Online Resource
    ISSN: 0148-0227
    URL: Article
    DOI: 10.1029/93JA01924
    Language: English
    Publisher: American Geophysical Union (AGU)
    Publication Date: 1994
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