Solar wind modulation of the auroral zone geomagnetic activity when the interplanetary magnetic field has a strong northward component

Hruška, A.; Hruska, J.

doi:10.1029/ja094ia05p05479

Cited by 4 publications

(2 citation statements)

References 8 publications

(3 reference statements)

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“…These results are in accordance with the models suggesting the strong electron acceleration in the magnetosphere in 1-2 days after the SSC (Hruska and Hruska, 1989;Blake et al, 2001). At this time there is a main process of acceleration of low-energy electron (previously injected during the substorm) up to high energy (several MeV) in the magnetosphere.…”

Section: Interplanetary and Geomagnetic Disturbances Related To The Esupporting

confidence: 93%

Long-term (50 years) measurements of cosmic ray fluxes in the atmosphere

Stozhkov

Svirzhevsky

Bazilevskaya

et al. 2009

Advances in Space Research

116

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Section: Interplanetary and Geomagnetic Disturbances Related To The Esupporting

confidence: 93%

Long-term (50 years) measurements of cosmic ray fluxes in the atmosphere

Stozhkov

Svirzhevsky

Bazilevskaya

et al. 2009

Advances in Space Research

116

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“…This is explained by known temporal relationships between these two solar wind parameters. In particular, empirical [ Hruska and Hruska , 1989] and theoretical [ Pizzo , 1983] studies show that strong enhancements in IMF magnitude tend to precede significant increases in solar wind speed near corotating interaction regions (CIRs) by a day or so. The same Pizzo study, as well as empirical studies as far back as the study of Gosling et al [1972], also showed that sharp increases in density occur at the leading edge of CIRs.…”

Section: Single‐input Radiation Belt Linear Predictions (Revisited)mentioning

confidence: 99%

Radiation belt electrons respond to multiple solar wind inputs

2007

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[1] The multivariate statistical basis that underlies both single-and multi-input linear prediction filter analyses is reviewed, providing context necessary to understand the full capabilities and limitations of such models. A brief reanalysis of single-input filters is conducted primarily as a contrast to subsequent analysis of multi-input linear filters, which (1) guarantee similar or better prediction capabilities than single-input linear filters and (2) reduce bias in estimated filter coefficients that is inherent to underspecified linear models when ordinary least squares algorithms are employed. The former is clearly valuable from a practical standpoint, but the latter helps build confidence in any physical interpretations of both the filter coefficients, which often emulate stable low-order dynamical response functions quite well, as well as prediction error statistics that can be used to provide a lower bound on the fractional or percent variance of radiation belt electron flux that can be attributed to each different solar wind input. We find that the solar wind bulk speed tends to be the primary driver of electron flux enhancements at magnetic L shells larger than 4, with little or no relation to flux decreases. Changes in the solar wind's magnetic field strength tend to temporarily reduce electron fluxes between L = 4 and L = 8, while enhancing it between L = 3 and L = 4. In contrast to predictions generated by single-input linear filters, multi-input filters show that solar wind plasma density only contributes weakly to electron flux variability, although it does so consistently across nearly all L shells. Finally, we studied two distinct 4-year intervals within the most recent solar cycle and found that smaller, more time-stationary prediction errors are generated by multi-input linear filters. We therefore conclude that multi-input filters more accurately reflect real dynamic relationships than any single-input linear filter alone.

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Coronal mass ejections, magnetic clouds, and relativistic magnetospheric electron events: ISTP

Baker¹,

Pulkkinen²,

Li³

et al. 1998

J. Geophys. Res.

153

126

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Abstract. The role of high-speed solar wind streams in driving relativistic electron acceleration within the Earth's magnetosphere during solar activity minimum conditions has been well documented. The rising phase of the new solar activity cycle (cycle 23) commenced in 1996, and there have recently been a number of coronal mass ejections (CMEs) and related "magnetic clouds" at 1 AU. As these CME/cloud systems interact with the Earth's magnetosphere, some events produce substantial enhancements in the magnetospheric energetic particle population while others do not. This paper compares and contrasts relativistic electron signatures observed by the POLAR, SAMPEX, Highly Elliptical Orbit, and geostationary orbit spacecraft during two magnetic cloud events: May 27-29, 1996, and January 10-11, 1997. Sequences were observed in each case in which the interplanetary magnetic field was first strongly southward and then rotated northward. In both cases, there were large solar wind density enhancements toward the end of the cloud passage at 1 AU. Strong energetic electron acceleration was observed in the January event, but not in the May event. The relative geoeffectiveness for these two cases is assessed, and it is concluded that large induced electric fields (9B/9t) caused in situ acceleration of electrons throughout the outer radiation zone during the January 1997 event.

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Solar wind modulation of the auroral zone geomagnetic activity when the interplanetary magnetic field has a strong northward component

Cited by 4 publications

References 8 publications

Long-term (50 years) measurements of cosmic ray fluxes in the atmosphere

Long-term (50 years) measurements of cosmic ray fluxes in the atmosphere

Radiation belt electrons respond to multiple solar wind inputs

Coronal mass ejections, magnetic clouds, and relativistic magnetospheric electron events: ISTP

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