Evolution of the concept of Sudden Storm Commencements and their operative identification

Curto, J. J.; Araki, Tohru; Alberca, L. F.

doi:10.1186/bf03352059

Cited by 64 publications

(73 citation statements)

References 93 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The conditions in the solar wind that lead to enhancement of the ring current are often preceded by a solar wind shock, so the characteristic Sym-H signature of a geomagnetic storm is a positive perturbation (the storm initial phase), a rapid negative excursion lasting several hours (the storm main phase) as the ring current builds, followed by a several-day return to quiescent conditions (the storm recovery phase). The shock arrival and positive excursion of Sym-H is also known as a sudden storm commencement (e.g., Curto et al 2007). There is some evidence for feedback between the intensity of the ring current and the deflation of the magnetotail lobes during the storm recovery phase (Milan 2009;Milan et al 2009a,b).…”

Section: Magnetospheric Dynamicsmentioning

confidence: 99%

Overview of Solar Wind–Magnetosphere–Ionosphere–Atmosphere Coupling and the Generation of Magnetospheric Currents

Milan¹,

Clausen²,

Coxon³

et al. 2017

Earth's Magnetic Field

View full text Add to dashboard Cite

We review the morphology and dynamics of the electrical current systems of the terrestrial magnetosphere and ionosphere. Observations from the Active Magnetosphere and Planetary Electrodynamics Response Experiment (AMPERE) over the three years 2010 to 2012 are employed to illustrate the variability of the field-aligned currents that couple the magnetosphere and ionosphere, on timescales from minutes to years, in response to the impact of solar wind disturbances on the magnetosphere and changes in the level of solar illumination of the polar ionospheres. The variability is discussed within the context of the occurrence of magnetic reconnection between the solar wind and terrestrial magnetic fields at the magnetopause, the transport of magnetic flux within the magnetosphere, and the onset of magnetic reconnection in the magnetotail. The conditions under which the currents are expected to be weak, and hence minimally contaminate measurements of the internallyproduced magnetic field of the Earth, are briefly outlined.

show abstract

Section: Magnetospheric Dynamicsmentioning

confidence: 99%

Overview of Solar Wind–Magnetosphere–Ionosphere–Atmosphere Coupling and the Generation of Magnetospheric Currents

Milan¹,

Clausen²,

Coxon³

et al. 2017

Earth's Magnetic Field

View full text Add to dashboard Cite

show abstract

“…This means the first thing from a CME that strikes the magnetosphere is the shock. The shock compresses the magnetosphere, which produces a spiky increase in Dst, known as the storm sudden commencement (SSC) because a geomagnetic storm usually follows (Curto, Araki & Alberca 2007, and references therein). Shocks take anywhere from ∼19 hours to more than four days to reach Earth, as can be seen in Fig.…”

Section: Cme Structure and Geomagnetic Stormsmentioning

confidence: 99%

The CME link to geomagnetic storms

Gopalswamy

2009

Proc. IAU

View full text Add to dashboard Cite

Abstract. The coronal mass ejection (CME) link to geomagnetic storms stems from the southward component of the interplanetary magnetic field contained in the CME flux ropes and in the sheath between the flux rope and the CME-driven shock. A typical storm-causing CME is characterized by (i) high speed, (ii) large angular width (mostly halos and partial halos), and (iii) solar source location close to the central meridian. For CMEs originating at larger central meridian distances, the storms are mainly caused by the sheath field. Both the magnetic and energy contents of the storm-producing CMEs can be traced to the magnetic structure of active regions and the free energy stored in them.

show abstract

“…Our main priority is to detect storms that are likely to lead to notable consequences on Earth, such as GIC. In this study, we consider only storms that fulfill the following criteria [similar to those suggested by Joselyn and Tsurutani (1990) and Curto et al (2007) in their quantitative definitions of SSCs]:…”

Section: Defining Geomagnetic Storms and Stormy Conditionsmentioning

confidence: 99%

Automated detection of geomagnetic storms with heightened risk of GIC

Bailey

Leonhardt

2016

Earth Planet Sp

View full text Add to dashboard Cite

Automated detection of geomagnetic storms is of growing importance to operators of technical infrastructure (e.g., power grids, satellites), which is susceptible to damage caused by the consequences of geomagnetic storms. In this study, we compare three methods for automated geomagnetic storm detection: a method analyzing the first derivative of the geomagnetic variations, another looking at the Akaike information criterion, and a third using multi-resolution analysis of the maximal overlap discrete wavelet transform of the variations. These detection methods are used in combination with an algorithm for the detection of coronal mass ejection shock fronts in ACE solar wind data prior to the storm arrival on Earth as an additional constraint for possible storm detection. The maximal overlap discrete wavelet transform is found to be the most accurate of the detection methods. The final storm detection software, implementing analysis of both satellite solar wind and geomagnetic ground data, detects 14 of 15 more powerful geomagnetic storms over a period of 2 years.

show abstract

Evolution of the concept of Sudden Storm Commencements and their operative identification

Cited by 64 publications

References 93 publications

Overview of Solar Wind–Magnetosphere–Ionosphere–Atmosphere Coupling and the Generation of Magnetospheric Currents

Overview of Solar Wind–Magnetosphere–Ionosphere–Atmosphere Coupling and the Generation of Magnetospheric Currents

The CME link to geomagnetic storms

Automated detection of geomagnetic storms with heightened risk of GIC

Contact Info

Product

Resources

About