Global geomagnetic responses to the IMF &amp;lt;i&amp;gt;B&amp;lt;/i&amp;gt;&amp;lt;sub&amp;gt;z&amp;lt;/sub&amp;gt; fluctuations during the September/October 2003 high-speed stream intervals

Echer, E.; Korth, A.; Bolzan, Maurı́cio José Alves; Friedel, R. H.

doi:10.5194/angeo-35-853-2017

Cited by 8 publications

(4 citation statements)

References 80 publications

(111 reference statements)

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“…This analysis provides the frequencies where stronger energy coupling and modulation of the magnetotail by the IMF Bz variations during HILDCAAs can be observed. The periods that were found in our results agrees with what were found by other authors (Lee et al, 2006;Korth et al, 2006;Bolzan et al, 2012;Echer et al, 2017),…”

Section: Energy Transfer From Magnetotail To Auroral Region During Hisupporting

confidence: 94%

“…had found similar periods, 2.3 hours, during corotating interaction regions (CIR) driven storms. As well asEcher et al (2017) had found periods from 1.8 up to 3.1 h in a study of HSS driven geomagnetic activity events.The energy distribution in the main periods observed in the geomagnetic Bx component during HILDCAA was studied using the classification introduced by Souza et al, (2016). The energy distribution can be classified in 4 forms: Local, intermittent, Quasi-continuous and continuous.…”

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confidence: 84%

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Wavelet analysis of the magnetotail response to solar wind fluctuations during HILDCCA events

Franco¹,

Echer²,

Bolzan³

2019

Preprint

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Abstract. In this work a study of the effects of the High-Intensity Long-Duration Continuous AE activity events (HILDCAAs) in the magnetotail was conducted. The aim of this study was to search the main frequencies during HILDCAAs in the Bx component of the geomagnetic field, as well as at the main frequencies which the magnetotail responds to the solar wind during these events. In order to conduct this analysis the wavelet transform was employed in 9 HILDCAA events that occurred after the Cluster mission (2000) and coincided with the Cluster crossing through the tail of the magnetosphere from 2003 to 2007. Altogether, 25 most energetic periods was observed, which 76 % are ≤ 4 hours. The cross wavelet analysis technique was also used for the development of this study. It was applied to data of the Bz-IMF component and the Bx geomagnetic component, searching to obtain the periods in that had the highest correlation between these two series. To obtain these periods is important to identify frequencies on which the coupling of energy is stronger, as well the modulation of the magnetotail by the solar wind during HILDCAA events. The majority of correlation periods between the Bz (IMF) and Bx component of the geomagnetic field observed also were ≤ 4 hours, with 62.9 % of the periods. Thus the magnetotail responds stronger to IMF fluctuations during HILDCCAS at 2–4 hours scales, which are typical substorm periods.

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Section: Energy Transfer From Magnetotail To Auroral Region During Hisupporting

confidence: 94%

mentioning

confidence: 84%

Wavelet analysis of the magnetotail response to solar wind fluctuations during HILDCCA events

Franco¹,

Echer²,

Bolzan³

2019

Preprint

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“…DP‐2 currents correlate highly with solar wind forcing at short response delays (Etemadi et al., 1988; Lockwood et al., 1986; Nishida, 1968a, 1968b; Todd et al., 1988). These are driven responses to magnetic reconnection in the dayside magnetopause current sheet, which generates open magnetospheric field lines (Consolini & De Michelis, 2005; Echer et al., 2017; Finch et al., 2008), the voltage Φ D being the magnetic flux transfer rate from the closed to open magnetospheric field‐line topology. The open field lines generated are swept into the geomagnetic tail by the solar wind flow where they accumulate, storing energy there.…”

Section: Introductionmentioning

confidence: 99%

A Survey of 25 Years' Transpolar Voltage Data From the SuperDARN Radar Network and the Expanding‐Contracting Polar Cap Model

Lockwood

McWilliams

2021

JGR Space Physics

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This paper studies the expanding-contracting polar cap (ECPC) model of ionospheric convection excitation ) using an unprecedentedly large data set of observations of the transpolar voltage Φ PC , also known as the cross-cap potential difference. The ECPC model predicts that Φ PC at any one instant depends on the reconnection voltage in the cross-tail current sheet Φ N as well as that at the dayside magnetopause Φ D .One specific aim is to recreate two scatter plots from surveys of Φ PC that have been of great importance to our understanding of the excitation of ionospheric polar convection by the solar wind flow, but here using a much larger data set of observations. The first of these scatter plots shows the dependence of Φ PC on the northward component B Z of the interplanetary magnetic field (IMF) in the geocentric solar magnetospheric (GSM) reference frame (

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“…Forecasting the IMF and particularly its north‐south component is of most interest for interplanetary coronal mass ejections. Occasionally, however, and particularly during the declining and solar cycle minimum phases, corotating interaction regions can introduce a sufficiently strong southward component in the ambient wind to produce geoeffective disturbances (Echer et al, ).…”

Section: Assessment Of Current Model Capabilitiesmentioning

confidence: 99%

Assessing the Quality of Models of the Ambient Solar Wind

et al. 2018

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In this paper we present an assessment of the status of models of the global solar wind in the inner heliosphere. We limit our discussion to the class of models designed to provide solar wind forecasts, excluding those designed for the purpose of testing physical processes in idealized configurations. In addition, we limit our discussion to modeling of the ambient wind in the absence of coronal mass ejections. In this assessment we cover use of the models both in forecast mode and as tools for scientific research. We present a brief history of the development of these models, discussing the range of physical approximations in use. We discuss the limitations of the data inputs available to these models and its impact on their quality. We also discuss current model development trends. Empirical ModelsModeling of the solar coronal magnetic field began in earnest in the early 1960s with the advent of computers and the availability of photospheric magnetograms. The earliest models of the inner coronal field were based

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Global geomagnetic responses to the IMF <i>B</i><sub>z</sub> fluctuations during the September/October 2003 high-speed stream intervals

Cited by 8 publications

References 80 publications

Wavelet analysis of the magnetotail response to solar wind fluctuations during HILDCCA events

Wavelet analysis of the magnetotail response to solar wind fluctuations during HILDCCA events

A Survey of 25 Years' Transpolar Voltage Data From the SuperDARN Radar Network and the Expanding‐Contracting Polar Cap Model

Assessing the Quality of Models of the Ambient Solar Wind

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