Interplanetary sources of space weather disturbances in 1997 to 2000

Дмитриев, А. В.; Crosby, Norma; Chao, J. K.

doi:10.1029/2004sw000104

Cited by 19 publications

(15 citation statements)

References 52 publications

(64 reference statements)

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“…The association of SIRs with periodic density structures is potentially significant from the standpoint of magnetospheric particle dynamics. High‐speed streams are known to be efficient drivers of radiation belt flux enhancements, and SIR‐driven storms are more effective at increasing energetic electron flux in the outer radiation belts than ICME‐driven storms (Dmitriev et al., ; Kataoka & Miyoshi, ; Miyoshi & Kataoka, , ). There is some evidence that ULF waves, particularly at the frequencies observed here, can play an important role in the energization and transport of radiation belt particles, particularly in the outer zone (Elkington et al., ; Mathie & Mann, ; O'Brien et al., ; Ozeke & Mann, ).…”

Section: Discussionmentioning

confidence: 99%

The Source, Significance, and Magnetospheric Impact of Periodic Density Structures Within Stream Interaction Regions

Kepko

Viall

2019

JGR Space Physics

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We present several examples of magnetospheric ultralow frequency pulsations associated with stream interaction regions and demonstrate that the observed magnetospheric pulsations were also present in the solar wind number density. The distance of the solar wind monitor ranged from just upstream of Earth's bow shock to 261 RE, with a propagation time delay of up to 90 min. The number density oscillations far upstream of Earth are offset from similar oscillations observed within the magnetosphere by the advection timescale, suggesting that the periodic dynamic pressure enhancements were time stationary structures, passively advecting with the ambient solar wind. The density structures are larger than Earth's magnetosphere and slowly altered the dynamic pressure enveloping Earth, leading to a quasi‐static and globally coherent “forced‐breathing” of Earth's dayside magnetospheric cavity. The impact of these periodic solar wind density structures was observed in both magnetospheric magnetic field and energetic particle data. We further show that the structures were initially smaller‐amplitude, spatially larger, structures in the upstream slow solar wind and that the higher‐speed wind compressed and amplified these preexisting structures leading to a series of quasiperiodic density structures with periods typically near 20 min. Similar periodic density structures have been observed previously at L1 and in remote images, but never in the context of solar wind shocks and discontinuities. The existence of periodic density structures within stream interaction regions may play an important role in magnetospheric particle acceleration, loss, and transport, particularly for outer zone electrons that are highly responsive to ultralow frequency wave activity.

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Section: Discussionmentioning

confidence: 99%

The Source, Significance, and Magnetospheric Impact of Periodic Density Structures Within Stream Interaction Regions

Kepko

Viall

2019

JGR Space Physics

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“…They have been investigated much less than storms driven by coronal mass ejections (CMEs) [e.g., Gonzalez et al , 1994]. Although the magnitude of CIR‐induced storms is smaller on average, they may be more geoeffective due to higher fluxes of relativistic electrons in the outer radiation belt [ Dmitriev et al , 2005; Borovsky and Denton , 2006; Kataoka and Miyoshi , 2006; Miyoshi and Kataoka , 2008] and a more severe spacecraft charging [ Borovsky and Denton , 2006].…”

Section: Introductionmentioning

confidence: 99%

Empirical modeling of a CIR‐driven magnetic storm

et al. 2010

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[1] The empirical analysis of structure and evolution of the geomagnetic field and underlying electric currents during the 8-11 March 2008 magnetospheric storm, driven by a corotating interaction region, is presented. It is based on the high-resolution geomagnetic field model TS07D (http://geomag_field.jhuapl.edu/model/) and the low-altitude mapping of field-aligned currents obtained using Iridium satellites. Compared to storms, driven by coronal mass ejections, the equatorial currents are found to be overall more dawn-dusk symmetric. Only in the early main phase a moderate hook-like westward current flowing from the Region-2 inflow area on the dawn side to the dusk/afternoon magnetopause is detected, along with an eastward current near the pre-noon magnetopause. New tail-type currents are found to dominate the storm-time magnetosphere in early main and recovery phases at the moments of strong peaks of the solar wind dynamic pressure. Similar effects, found in CME-driven storms, coincide in time with the plasma sheet density bursts. A clear distinction between the periods dominated by the partial ring current and the tail-type currents seen in the model agrees with the Iridium data that indicate a significant reduction and contraction of the field-aligned current pattern in the latter case. Overall small magnitudes of the total field-aligned currents, with rather transient enhancements, appear to be the most distinctive feature of CIR-driven storms. Comparison between the model and observations made by five THEMIS probes shows good agreement on storm timescales. Moreover, every deviation arising during a substorm reveals characteristic signatures of the tail current sheet thinning and dipolarization.

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“…The correlation between solar wind parameters and relativistic electron enhancements in the inner magnetosphere has been well studied for the geosynchronous orbit (O'Brien et al, 2001;Dmitriev et al, 2005;Miyoshi and Kataoka, 2005;Borovsky and Denton, 2006;Borovsky and Steinberg, 2006;Kataoka and Miyoshi, 2006;Kim et al, 2006). Iles et al (2002) and Vassiliadis et al (2005) studied the same correlation inside geosynchronous orbit also and found that for 3.5oLo6.5 and 4.1oLo7.5, respectively, MeV electron enhancements were well correlated with high solar wind speed.…”

Section: Superposed Epoch Analysis Of Solar Wind and Geomagnetic Paramentioning

confidence: 91%

“…Relativistic electron fluxes near geosynchronous orbit have been seen to rise on timescales of the order of 2-3 days and these rises are shown to be well correlated with high solar wind speed (O'Brien et al, 2001;Iles et al, 2002;Dmitriev et al, 2005;Kataoka and Miyoshi, 2006;Vassiliadis et al, 2005). At the geosynchronous orbit (L ¼ 6.6) radial diffusion-enhanced by ULF wave activity (Elkington et al, 1999;Mathie and Mann, 2000)-is expected to have an important effect on radiation belt electron dynamics (O'Brien et al, 2001).…”

Section: Introductionmentioning

confidence: 94%