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The differences between storms driven by helmet streamer CIRs and storms driven by pseudostreamer CIRs

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The differences between storms driven by helmet streamer CIRs and storms driven by pseudostreamer CIRs. / Borovsky, Joseph E.; Denton, Michael.

In: Journal of Geophysical Research, Vol. 118, No. 9, 09.2013, p. 5506-5521.

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Borovsky, Joseph E. ; Denton, Michael. / The differences between storms driven by helmet streamer CIRs and storms driven by pseudostreamer CIRs. In: Journal of Geophysical Research. 2013 ; Vol. 118, No. 9. pp. 5506-5521.

Bibtex

@article{78180bd9a8b544aaad48780ac91b7d45,
title = "The differences between storms driven by helmet streamer CIRs and storms driven by pseudostreamer CIRs",
abstract = "A corotating interaction region (CIR) is formed when fast coronal hole origin solar wind overtakes slow solar wind and forms a region of compressed plasma and magnetic field. The slow wind upstream of the coronal hole fast wind can be either of helmet streamer origin or pseudostreamer origin. For a collection of 125 CIR-driven geomagnetic storms, the slow wind ahead of each CIR is examined; for those storm not containing ejecta, each CIR is categorized as a helmet streamer CIR (74 of the 125 storms) or a pseudostreamer CIR (11 of the 125 storms). Separate superposed epoch studies are performed on the two groups to discern the differences between storms driven by pseudostreamer CIRs and those driven by helmet streamer CIRs. A major difference is that pseudostreamer CIR storms tend not to have a calm before the storm, so the outer plasmasphere does not refill before storm onset, and the outer electron radiation belt does not exhibit a pre-storm decay. The superdense plasma sheet is weaker for pseudostreamer CIR storms, and the dropout of the electron radiation belt is weaker. Pseudostreamer CIR storms and helmet streamer CIR storms tend to be of the same strength as measured by the magnitude of Kp, MBI (midnight boundary index), or Dst.",
keywords = "geomagnetic storms, pseudostreamers, calm before the storm, geomagnetic storms;pseudostreamers;corotating interaction regions;calm before the storm",
author = "Borovsky, {Joseph E.} and Michael Denton",
note = "{\textcopyright}2013. American Geophysical Union. All Rights Reserved.",
year = "2013",
month = sep
doi = "10.1002/jgra.50524",
language = "English",
volume = "118",
pages = "5506--5521",
journal = "Journal of Geophysical Research",
issn = "0148-0227",
publisher = "American Geophysical Union",
number = "9",

}

RIS

TY - JOUR

T1 - The differences between storms driven by helmet streamer CIRs and storms driven by pseudostreamer CIRs

AU - Borovsky, Joseph E.

AU - Denton, Michael

N1 - ©2013. American Geophysical Union. All Rights Reserved.

PY - 2013/9

Y1 - 2013/9

N2 - A corotating interaction region (CIR) is formed when fast coronal hole origin solar wind overtakes slow solar wind and forms a region of compressed plasma and magnetic field. The slow wind upstream of the coronal hole fast wind can be either of helmet streamer origin or pseudostreamer origin. For a collection of 125 CIR-driven geomagnetic storms, the slow wind ahead of each CIR is examined; for those storm not containing ejecta, each CIR is categorized as a helmet streamer CIR (74 of the 125 storms) or a pseudostreamer CIR (11 of the 125 storms). Separate superposed epoch studies are performed on the two groups to discern the differences between storms driven by pseudostreamer CIRs and those driven by helmet streamer CIRs. A major difference is that pseudostreamer CIR storms tend not to have a calm before the storm, so the outer plasmasphere does not refill before storm onset, and the outer electron radiation belt does not exhibit a pre-storm decay. The superdense plasma sheet is weaker for pseudostreamer CIR storms, and the dropout of the electron radiation belt is weaker. Pseudostreamer CIR storms and helmet streamer CIR storms tend to be of the same strength as measured by the magnitude of Kp, MBI (midnight boundary index), or Dst.

AB - A corotating interaction region (CIR) is formed when fast coronal hole origin solar wind overtakes slow solar wind and forms a region of compressed plasma and magnetic field. The slow wind upstream of the coronal hole fast wind can be either of helmet streamer origin or pseudostreamer origin. For a collection of 125 CIR-driven geomagnetic storms, the slow wind ahead of each CIR is examined; for those storm not containing ejecta, each CIR is categorized as a helmet streamer CIR (74 of the 125 storms) or a pseudostreamer CIR (11 of the 125 storms). Separate superposed epoch studies are performed on the two groups to discern the differences between storms driven by pseudostreamer CIRs and those driven by helmet streamer CIRs. A major difference is that pseudostreamer CIR storms tend not to have a calm before the storm, so the outer plasmasphere does not refill before storm onset, and the outer electron radiation belt does not exhibit a pre-storm decay. The superdense plasma sheet is weaker for pseudostreamer CIR storms, and the dropout of the electron radiation belt is weaker. Pseudostreamer CIR storms and helmet streamer CIR storms tend to be of the same strength as measured by the magnitude of Kp, MBI (midnight boundary index), or Dst.

KW - geomagnetic storms

KW - pseudostreamers

KW - calm before the storm

KW - geomagnetic storms;pseudostreamers;corotating interaction regions;calm before the storm

U2 - 10.1002/jgra.50524

DO - 10.1002/jgra.50524

M3 - Journal article

VL - 118

SP - 5506

EP - 5521

JO - Journal of Geophysical Research

JF - Journal of Geophysical Research

SN - 0148-0227

IS - 9

ER -