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Key features of >30 keV electron precipitation during high speed solar wind streams: A superposed epoch analysis

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Key features of >30 keV electron precipitation during high speed solar wind streams: A superposed epoch analysis. / Kavanagh, Andrew; Honary, Farideh; Donovan, E.F.; Ulich, T.; Denton, Michael.

In: Journal of Geophysical Research, Vol. 117, A00L09, 07.06.2012, p. 1-13.

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@article{7653aacddd6b41f1b7a0b0da8b0a4191,
title = "Key features of >30 keV electron precipitation during high speed solar wind streams: A superposed epoch analysis",
abstract = "We present an epoch analysis of energetic (>30 keV) electron precipitation during 173 high speed solar wind streams (HSS) using riometer observations of cosmic noise absorption (CNA) as a proxy for the precipitation. The arrival of the co-rotating interaction region (CIR) prior to stream onset, elevates the precipitation which then peaks some 12 h after stream arrival. Precipitation continues for several days following the HSS arrival. The MLT distribution of CNA is generally consistent with the statistical pattern explained via the substorm process, though the statistical deep minimum of CNA/precipitation does change during the HSS suggesting increased precipitation in the 15–20 MLT sector. The level of precipitation is strongly controlled by the average state of the IMF BZ component on the day prior to the arrival of the stream interface. An average negative IMF BZ will produce higher CNA across all L-shells and MLT, up to 100% higher than an average positive IMF BZ.",
author = "Andrew Kavanagh and Farideh Honary and E.F. Donovan and T. Ulich and Michael Denton",
note = "{\textcopyright}2012. American Geophysical Union. All Rights Reserved.",
year = "2012",
month = jun,
day = "7",
doi = "10.1029/2011JA017320",
language = "English",
volume = "117",
pages = "1--13",
journal = "Journal of Geophysical Research",
issn = "0148-0227",
publisher = "American Geophysical Union",

}

RIS

TY - JOUR

T1 - Key features of >30 keV electron precipitation during high speed solar wind streams: A superposed epoch analysis

AU - Kavanagh, Andrew

AU - Honary, Farideh

AU - Donovan, E.F.

AU - Ulich, T.

AU - Denton, Michael

N1 - ©2012. American Geophysical Union. All Rights Reserved.

PY - 2012/6/7

Y1 - 2012/6/7

N2 - We present an epoch analysis of energetic (>30 keV) electron precipitation during 173 high speed solar wind streams (HSS) using riometer observations of cosmic noise absorption (CNA) as a proxy for the precipitation. The arrival of the co-rotating interaction region (CIR) prior to stream onset, elevates the precipitation which then peaks some 12 h after stream arrival. Precipitation continues for several days following the HSS arrival. The MLT distribution of CNA is generally consistent with the statistical pattern explained via the substorm process, though the statistical deep minimum of CNA/precipitation does change during the HSS suggesting increased precipitation in the 15–20 MLT sector. The level of precipitation is strongly controlled by the average state of the IMF BZ component on the day prior to the arrival of the stream interface. An average negative IMF BZ will produce higher CNA across all L-shells and MLT, up to 100% higher than an average positive IMF BZ.

AB - We present an epoch analysis of energetic (>30 keV) electron precipitation during 173 high speed solar wind streams (HSS) using riometer observations of cosmic noise absorption (CNA) as a proxy for the precipitation. The arrival of the co-rotating interaction region (CIR) prior to stream onset, elevates the precipitation which then peaks some 12 h after stream arrival. Precipitation continues for several days following the HSS arrival. The MLT distribution of CNA is generally consistent with the statistical pattern explained via the substorm process, though the statistical deep minimum of CNA/precipitation does change during the HSS suggesting increased precipitation in the 15–20 MLT sector. The level of precipitation is strongly controlled by the average state of the IMF BZ component on the day prior to the arrival of the stream interface. An average negative IMF BZ will produce higher CNA across all L-shells and MLT, up to 100% higher than an average positive IMF BZ.

U2 - 10.1029/2011JA017320

DO - 10.1029/2011JA017320

M3 - Journal article

VL - 117

SP - 1

EP - 13

JO - Journal of Geophysical Research

JF - Journal of Geophysical Research

SN - 0148-0227

M1 - A00L09

ER -