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What controls the local time extent of flux transfer events?

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What controls the local time extent of flux transfer events? / Milan, S. E.; Imber, S. M.; Carter, J. A. et al.
In: Journal of Geophysical Research: Space Physics, Vol. 121, No. 2, 01.02.2016, p. 1391-1401.

Research output: Contribution to Journal/Magazine › Journal article › peer-review

Harvard

Milan, SE, Imber, SM, Carter, JA, Walach, MT & Hubert, B 2016, 'What controls the local time extent of flux transfer events?', Journal of Geophysical Research: Space Physics, vol. 121, no. 2, pp. 1391-1401. https://doi.org/10.1002/2015JA022012

APA

Milan, S. E., Imber, S. M., Carter, J. A., Walach, M. T., & Hubert, B. (2016). What controls the local time extent of flux transfer events? Journal of Geophysical Research: Space Physics, 121(2), 1391-1401. https://doi.org/10.1002/2015JA022012

Vancouver

Milan SE, Imber SM, Carter JA, Walach MT, Hubert B. What controls the local time extent of flux transfer events? Journal of Geophysical Research: Space Physics. 2016 Feb 1;121(2):1391-1401. doi: 10.1002/2015JA022012

Author

Milan, S. E. ; Imber, S. M. ; Carter, J. A. et al. / What controls the local time extent of flux transfer events?. In: Journal of Geophysical Research: Space Physics. 2016 ; Vol. 121, No. 2. pp. 1391-1401.

Bibtex

@article{d8cb255331b2459f8f1430cb39473c77,
title = "What controls the local time extent of flux transfer events?",
abstract = "Flux transfer events (FTEs) are the manifestation of bursty and/or patchy magnetic reconnection at the magnetopause. We compare two sequences of the ionospheric signatures of flux transfer events observed in global auroral imagery and coherent ionospheric radar measurements. Both sequences were observed during very similar seasonal and interplanetary magnetic field (IMF) conditions, though with differing solar wind speed. A key observation is that the signatures differed considerably in their local time extent. The two periods are 26 August 1998, when the IMF had components BZ≈-10 nT and BY≈9 nT and the solar wind speed was VX≈650 km s-1, and 31 August 2005, IMF BZ≈-7 nT, BY≈17 nT, and VX≈380 km s-1. In the first case, the reconnection rate was estimated to be near 160 kV, and the FTE signatures extended across at least 7 h of magnetic local time (MLT) of the dayside polar cap boundary. In the second, a reconnection rate close to 80 kV was estimated, and the FTEs had a MLT extent of roughly 2 h. We discuss the ramifications of these differences for solar wind-magnetosphere coupling.",
keywords = "flux transfer events, magnetic reconnection",
author = "Milan, {S. E.} and Imber, {S. M.} and Carter, {J. A.} and Walach, {M. T.} and B. Hubert",
year = "2016",
month = feb,
day = "1",
doi = "10.1002/2015JA022012",
language = "English",
volume = "121",
pages = "1391--1401",
journal = "Journal of Geophysical Research: Space Physics",
issn = "2169-9380",
publisher = "Blackwell Publishing Ltd",
number = "2",

}

RIS

TY - JOUR

T1 - What controls the local time extent of flux transfer events?

AU - Milan, S. E.

AU - Imber, S. M.

AU - Carter, J. A.

AU - Walach, M. T.

AU - Hubert, B.

PY - 2016/2/1

Y1 - 2016/2/1

N2 - Flux transfer events (FTEs) are the manifestation of bursty and/or patchy magnetic reconnection at the magnetopause. We compare two sequences of the ionospheric signatures of flux transfer events observed in global auroral imagery and coherent ionospheric radar measurements. Both sequences were observed during very similar seasonal and interplanetary magnetic field (IMF) conditions, though with differing solar wind speed. A key observation is that the signatures differed considerably in their local time extent. The two periods are 26 August 1998, when the IMF had components BZ≈-10 nT and BY≈9 nT and the solar wind speed was VX≈650 km s-1, and 31 August 2005, IMF BZ≈-7 nT, BY≈17 nT, and VX≈380 km s-1. In the first case, the reconnection rate was estimated to be near 160 kV, and the FTE signatures extended across at least 7 h of magnetic local time (MLT) of the dayside polar cap boundary. In the second, a reconnection rate close to 80 kV was estimated, and the FTEs had a MLT extent of roughly 2 h. We discuss the ramifications of these differences for solar wind-magnetosphere coupling.

AB - Flux transfer events (FTEs) are the manifestation of bursty and/or patchy magnetic reconnection at the magnetopause. We compare two sequences of the ionospheric signatures of flux transfer events observed in global auroral imagery and coherent ionospheric radar measurements. Both sequences were observed during very similar seasonal and interplanetary magnetic field (IMF) conditions, though with differing solar wind speed. A key observation is that the signatures differed considerably in their local time extent. The two periods are 26 August 1998, when the IMF had components BZ≈-10 nT and BY≈9 nT and the solar wind speed was VX≈650 km s-1, and 31 August 2005, IMF BZ≈-7 nT, BY≈17 nT, and VX≈380 km s-1. In the first case, the reconnection rate was estimated to be near 160 kV, and the FTE signatures extended across at least 7 h of magnetic local time (MLT) of the dayside polar cap boundary. In the second, a reconnection rate close to 80 kV was estimated, and the FTEs had a MLT extent of roughly 2 h. We discuss the ramifications of these differences for solar wind-magnetosphere coupling.

KW - flux transfer events

KW - magnetic reconnection

U2 - 10.1002/2015JA022012

DO - 10.1002/2015JA022012

M3 - Journal article

AN - SCOPUS:84959378225

VL - 121

SP - 1391

EP - 1401

JO - Journal of Geophysical Research: Space Physics

JF - Journal of Geophysical Research: Space Physics

SN - 2169-9380

IS - 2

ER -