Space- and ground-based investigations of solar wind–magnetosphere–ionosphere coupling

Milan, S. E.; Wild, J. A.; Grocott, Adrian; Draper, N. C.

doi:10.1016/j.asr.2005.08.009

Cited by 14 publications

(21 citation statements)

References 35 publications

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“…However, data from the NORSTAR MSP at the Gillam observation site in Canada (Figure 42), which measures auroral emission at several wavelengths over a narrow longitude range but a wide range of latitude, are available from ∼ 03:30 UT and show the equatorward edge of the nightside aurora moving to lower latitudes. This is consistent with the expansion of the ionospheric polar cap caused by enhanced reconnection at the dayside magnetosphere producing more open magnetic flux (Milan et al, 2006). This is interesting because the predominantly northward-directed IMF in the ICME sheath would not usually be expected to produce such significant open magnetic flux.…”

Section: Multi-spacecraft Measurements and Ground-based Observations supporting

confidence: 69%

From the Sun to the Earth: The 13 May 2005 Coronal Mass Ejection

et al. 2010

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We report the results of a multi-instrument, multi-technique, coordinated study of the solar eruptive event of 13 May 2005. We discuss the resultant Earth-directed (halo) coronal mass ejection (CME), and the effects on the terrestrial space environment and upper Earth atmosphere. The interplanetary CME (ICME) impacted the Earth's magnetosphere and caused the most-intense geomagnetic storm of 2005 with a Disturbed Storm Time (Dst) index reaching −263 nT at its peak. The terrestrial environment responded to the storm on a global scale. We have combined observations and measurements from coronal and interplanetary remote-sensing instruments, interplanetary and near-Earth in-situ measurements, remote-sensing observations and in-situ measurements of the terrestrial magnetosphere and ionosphere, along with coronal and heliospheric modelling. These analyses are used to trace the origin, development, propagation, terrestrial impact, and subsequent consequences of this event to obtain the most comprehensive view of a geo-effective solar eruption to date. This particular event is also part of a NASA-sponsored Living With a Star (LWS) study and an on-going US NSF-sponsored Solar, Heliospheric, and INterplanetary Environment (SHINE) community investigation.

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Section: Multi-spacecraft Measurements and Ground-based Observations supporting

confidence: 69%

From the Sun to the Earth: The 13 May 2005 Coronal Mass Ejection

et al. 2010

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“…The solar wind density and IMF B z are plotted due to their role in as a possible trigger for a substorm onset. And E sw is shown since it the major solar wind/IMF component for dayside reconnection (Milan, 2004;Milan et al, 2006). Note that when E sw is positive there is dayside reconnection since B z is negative.…”

Section: Isolated Substormmentioning

confidence: 99%

Aurora and open magnetic flux during isolated substorms, sawteeth, and SMC events

et al. 2007

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Abstract. Using Polar UVI LBHl and IMAGE FUV WIC data, we have compared the auroral signatures and polar cap open flux for isolated substorms, sawteeth oscillations, and steady magnetospheric convection (SMC) events. First, a case study of each event type is performed, comparing auroral signatures and open magnetic fluxes to one another. The latitude location of the auroral oval is similar during isolated substorms and SMC events. The auroral intensity during SMC events is similar to that observed during the expansion phase of an isolated substorm. Examination of an individual sawtooth shows that the auroral intensity is much greater than the SMC or isolated substorm events and the auroral oval is displaced equatorward making a larger polar cap. The temporal variations observed during the individual sawtooth are similar to that observed during the isolated substorm, and while the change in polar cap flux measured during the sawtooth is larger, the percent change in flux is similar to that measured during the isolated substorm. These results are confirmed by a statistical analysis of events within these three classes. The results show that the auroral oval measured during individual sawteeth contains a polar cap with, on average, 150% more magnetic flux than the oval measured during isolated substorms or during SMC events. However, both isolated substorms and sawteeth show a 30% decrease in polar cap magnetic flux during the dipolarization (expansion) phase.

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“…If the reconnection rate is proportional to B z (e.g. Milan et al, 2006) then D (and consequently N ) is expected to fall to ∼70 kV.…”

Section: Open Flux Reconnection Rates and Transpolar Voltagementioning

confidence: 99%

“…Changes in F P C can be used to infer the dayside and nightside reconnection rates, D and N , respectively, as discussed by Milan et al (2003Milan et al ( , 2006:…”

Section: Open Flux Reconnection Rates and Transpolar Voltagementioning

confidence: 99%

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Flux closure during a substorm observed by Cluster, Double Star, IMAGE FUV, SuperDARN, and Greenland magnetometers

et al. 2006

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Abstract. We examine magnetic flux closure during an extended substorm interval on 29 August 2004 involving a two-stage onset and subsequent re-intensifications. Cluster and Double Star provide observations of magnetotail dynamics, while the corresponding auroral evolution, convection response, and substorm current wedge development are monitored by IMAGE FUV, SuperDARN, and the Greenland magnetometer chain, respectively. The first stage of onset is associated with the reconnection of closed flux in the plasma sheet; this is accompanied by a short-lived auroral intensification, a modest substorm current wedge magnetic bay, but no significant ionospheric convection enhancement. The second stage follows the progression of reconnection to the open field lines of the lobes; accompanied by prolonged auroral bulge and westward-travelling surge development, enhanced magnetic bays and convection. We find that the tail dynamics are highly influenced by ongoing dayside creation of open flux, leading to flux pile-up in the near-tail and a step-wise down-tail motion of the tail reconnection site. In all, 5 dipolarizations are observed, each associated with the closure of ∼0.1 GWb of flux. Very simple calculations indicate that the X-line should progress down-tail at a speed of 20 km s −1 , or 6 R E between each dipolarization.

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Space- and ground-based investigations of solar wind–magnetosphere–ionosphere coupling

Cited by 14 publications

References 35 publications

From the Sun to the Earth: The 13 May 2005 Coronal Mass Ejection

From the Sun to the Earth: The 13 May 2005 Coronal Mass Ejection

Aurora and open magnetic flux during isolated substorms, sawteeth, and SMC events

Flux closure during a substorm observed by Cluster, Double Star, IMAGE FUV, SuperDARN, and Greenland magnetometers

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