Correlation between the inner edge of outer radiation belt electrons and the innermost plasmapause location

Li, Xinlin; Baker, D. N.; O’Brien, T. P.; Xie, Luhua; Zong, Qiugang

doi:10.1029/2006gl026294

Cited by 128 publications

(135 citation statements)

References 26 publications

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“…Loto'Aniu et al, 2006]. Such analyses may also shed light on the physical processes responsible for the reported correlations between the location of this inner boundary and the plasmapause [e.g., Li et al, 2006] (itself correlated with Dst see, e.g., O'Brien and Moldwin [2003]), as well as the recent reports of the apparently largely impenetrable nature of the inner edge of the outer belt Baker et al [2014].…”

Section: Summary and Discussionmentioning

confidence: 99%

Accurately specifying storm‐time ULF wave radial diffusion in the radiation belts

Dimitrakoudis

Mann

Balasis

et al. 2015

Geophysical Research Letters

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Ultralow frequency (ULF) waves can contribute to the transport, acceleration, and loss of electrons in the radiation belts through inward and outward diffusion. However, the most appropriate parameters to use to specify the ULF wave diffusion rates are unknown. Empirical representations of diffusion coefficients often use Kp; however, specifications using ULF wave power offer an improved physics‐based approach. We use 11 years of ground‐based magnetometer array measurements to statistically parameterize the ULF wave power with Kp, solar wind speed, solar wind dynamic pressure, and Dst. We find that Kp is the best single parameter to specify the statistical ULF wave power driving radial diffusion. Significantly, remarkable high energy tails exist in the ULF wave power distributions when expressed as a function of Dst. Two‐parameter ULF wave power specifications using Dst as well as Kp provide a better statistical representation of storm‐time radial diffusion than any single variable alone.

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Section: Summary and Discussionmentioning

confidence: 99%

Accurately specifying storm‐time ULF wave radial diffusion in the radiation belts

Dimitrakoudis

Mann

Balasis

et al. 2015

Geophysical Research Letters

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“…Then we consider that the events selected here give an innermost plasmapause position, not far from the plasmapause position that would be defined as the middle of the plasmasphere boundary layer. Note that in this way, we have the same plasmapause position definition as in the study of Li et al (2006). The presence of plasmaspheric plumes (Darrouzet et al, 2006(Darrouzet et al, , 2008 were further taken into account.…”

Section: Annmentioning

confidence: 99%

The relationship between plasmapause, solar wind and geomagnetic activity between 2007 and 2011

Verbanac

Pierrard

Bandić³

et al. 2015

Ann. Geophys.

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Abstract. Taking advantage of the Cluster satellite mission and especially the observations made by the instrument WHISPER to deduce the electron number density along the orbit of the satellites, we studied the relationships between the plasmapause positions (L PP ) and the following L PP indicators: (a) solar wind coupling functions B z (Z component of the interplanetary magnetic field vector, B, in GSM system), BV (related to the interplanetary electric field; B is the magnitude of the interplanetary magnetic field vector, V is solar wind velocity), and d mp /dt (which combines different physical processes responsible for the magnetospheric activity) and (b) geomagnetic indices Dst, Ap and AE. The analysis is performed separately for three magnetic local time (MLT) sectors (Sector1 -night sector (01:00-07:00 MLT); Sector2 -day sector (07:00-16:00 MLT); Sector3 -evening sector (16:00-01:00 MLT)) and for all MLTs taken together. All L PP indicators suggest the faster plasmapause response in the postmidnight sector. Delays in the plasmapause responses (hereafter time lags) are approximately 2-27 h, always increasing from Sector1 to Sector3. The obtained fits clearly resolve the MLT structures. The variability in the plasmapause is the largest for low values of L PP indicators, especially in Sector2. At low activity levels, L PP exhibits the largest values on the dayside (in Sector2) and the smallest on the postmidnight side (Sector1). Displacements towards larger values on the evening side (Sector3) and towards lower values on the dayside (Sector2) are identified for enhanced magnetic activity. Our results contribute to constraining the physical mechanisms involved in the plasmapause formation and to further study the still not well understood related issues.

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“…We explore the variations in Pc5 wave power in both time and space for two distinct types of magnetic storms that include the magnetic storms that occurred in March and April 2001, when relativistic electron flux enhancements were observed in the recovery phase and the magnetic storm in August 2001 that exhibited a prolonged decrease in relativistic electron fluxes without subsequent recovery. Furthermore, since the inner edge of the outer electron radiation zone corresponds to the plasmapause location when this gets forced inwards during periods of intense geomagnetic activity (Goldstein et al, 2005;Li et al, 2006), we investigate how the plasmapause erosion favours migration of very energetic electrons in the slot region as well as penetration of Pc5 waves to low L shells.…”

Section: Introductionmentioning

confidence: 99%

Association of radiation belt electron enhancements with earthward penetration of Pc5 ULF waves: a case study of intense 2001 magnetic storms

et al. 2015

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Abstract. Geospace magnetic storms, driven by the solar wind, are associated with increases or decreases in the fluxes of relativistic electrons in the outer radiation belt. We examine the response of relativistic electrons to four intense magnetic storms, during which the minimum of the Dst index ranged from −105 to −387 nT, and compare these with concurrent observations of ultra-low-frequency (ULF) waves from the trans-Scandinavian IMAGE magnetometer network and stations from multiple magnetometer arrays available through the worldwide SuperMAG collaboration. The latitudinal and global distribution of Pc5 wave power is examined to determine how deep into the magnetosphere these waves penetrate. We then investigate the role of Pc5 wave activity deep in the magnetosphere in enhancements of radiation belt electrons population observed in the recovery phase of the magnetic storms. We show that, during magnetic storms characterized by increased post-storm electron fluxes as compared to their pre-storm values, the earthward shift of peak and inner boundary of the outer electron radiation belt follows the Pc5 wave activity, reaching L shells as low as 3-4. In contrast, the one magnetic storm characterized by irreversible loss of electrons was related to limited Pc5 wave activity that was not intensified at low L shells. These observations demonstrate that enhanced Pc5 ULF wave activity penetrating deep into the magnetosphere during the main and recovery phase of magnetic storms can, for the cases examined, distinguish storms that resulted in increases in relativistic electron fluxes in the outer radiation belts from those that did not.

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Correlation between the inner edge of outer radiation belt electrons and the innermost plasmapause location

Cited by 128 publications

References 26 publications

Accurately specifying storm‐time ULF wave radial diffusion in the radiation belts

Accurately specifying storm‐time ULF wave radial diffusion in the radiation belts

The relationship between plasmapause, solar wind and geomagnetic activity between 2007 and 2011

Association of radiation belt electron enhancements with earthward penetration of Pc5 ULF waves: a case study of intense 2001 magnetic storms

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