A simplified model for timing the arrival of solar flare‐initiated shocks

Smart, D. F.; Shea, M. A.

doi:10.1029/ja090ia01p00183

Cited by 121 publications

(82 citation statements)

References 37 publications

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“…, Gosling 1993b). This transformation in understanding was reflected in the evolution of modeling efforts from flare-driven shocks (also called blast waves) to CMEs (Wu et al 1981;Wei 1982;Smart and Shea 1985;Smith and Dryer 1990;Wei and Dryer 1991;Gosling and Riley 1996;Vandas et al 1996, e.g., and references therein; see also reviews by Pizzo 1985 andDryer et al 1988).…”

Section: Structure Of Cmes To Icmesmentioning

confidence: 99%

The Physical Processes of CME/ICME Evolution

et al. 2017

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As observed in Thomson-scattered white light, coronal mass ejections (CMEs) are manifest as large-scale expulsions of plasma magnetically driven from the corona in the most energetic eruptions from the Sun. It remains a tantalizing mystery as to how these erupting magnetic fields evolve to form the complex structures we observe in the solar wind at Earth. Here, we strive to provide a fresh perspective on the post-eruption and interplanetary evolution of CMEs, focusing on the physical processes that define the many complex interactions of the ejected plasma with its surroundings as it departs the corona and propagates through the heliosphere. We summarize the ways CMEs and their interplanetary CMEs (ICMEs) are rotated, reconfigured, deformed, deflected, decelerated and disguised during their journey through the solar wind. This study then leads to consideration of how structures originating in coronal eruptions can be connected to their far removed interplanetary counterparts. Given that ICMEs are the drivers of most geomagnetic storms (and the sole driver of extreme storms), this work provides a guide to the processes that must be considered in making space weather forecasts from remote observations of the corona.

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Section: Structure Of Cmes To Icmesmentioning

confidence: 99%

The Physical Processes of CME/ICME Evolution

et al. 2017

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“…Assuming that the shock speed follows a longitudinal dependence as Smart & Shea 1985) we obtain the least-square fit indicated by the solid curves in Figure 14(a). The purple line is obtained assuming that the shock at STEREO-A had the same origin, whereas the gray line does not consider the observation from STEREO-A.…”

Section: Evidence For An Extended Interplanetary Shockmentioning

confidence: 99%

Longitudinal Properties of a Widespread Solar Energetic Particle Event on 2014 February 25: Evolution of the Associated Cme Shock

Lario

Kwon

Vourlidas

et al. 2016

ApJ

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We investigate the solar phenomena associated with the origin of the solar energetic particle (SEP) event observed on 2014 February 25 by a number of spacecraft distributed in the inner heliosphere over a broad range of heliolongitudes. These include spacecraft located near Earth; the twin Solar TErrestrial RElations Observatory spacecraft, STEREO-A and STEREO-B, located at ∼1 au from the Sun 153°west and 160°east of Earth, respectively; the MErcury Surface Space ENvironment GEochemistry and Ranging mission (at 0.40 au and 31°w est of Earth); and the Juno spacecraft (at 2.11 au and 48°east of Earth). Although the footpoints of the field lines nominally connecting the Sun with STEREO-A, STEREO-B and near-Earth spacecraft were quite distant from each other, an intense high-energy SEP event with Fe-rich prompt components was observed at these three locations. The extent of the extreme-ultraviolet wave associated with the solar eruption generating the SEP event was very limited in longitude. However, the white-light shock accompanying the associated coronal mass ejection extended over a broad range of longitudes. As the shock propagated into interplanetary space it extended over at least ∼190°i n longitude. The release of the SEPs observed at different longitudes occurred when the portion of the shock magnetically connected to each spacecraft was already at relatively high altitudes (2 R e above the solar surface). The expansion of the shock in the extended corona, as opposite to near the solar surface, determined the SEP injection and SEP intensity-time profiles at different longitudes.

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“…Gopalswamy et al 2000;Michałek et al 2004;Vršnak & Žic 2007), analytical propagation models (e.g. Smart & Shea 1985;Vršnak & Gopalswamy 2002;Cantó et al 2005;Vršnak & Žic 2007;Borgazzi et al 2009;), or numerical MHD simulations (e.g. González-Esparza et al 2003;Manchester et al 2004;Odstrcil et al 2004;Smith et al 2009;Taktakishvili et al 2009).…”

Section: Introductionmentioning

confidence: 99%

The role of aerodynamic drag in propagation of interplanetary coronal mass ejections

Vršnak

Žic

Falkenberg

et al. 2010

A&A

122

115

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Context. The propagation of interplanetary coronal mass ejections (ICMEs) and the forecast of their arrival on Earth is one of the central issues of space weather studies. Aims. We investigate to which degree various ICME parameters (mass, size, take-off speed) and the ambient solar-wind parameters (density and velocity) affect the ICME Sun-Earth transit time. Methods. We study solutions of a drag-based equation of motion by systematically varying the input parameters. The analysis is focused on ICME transit times and 1 AU velocities. Results. The model results reveal that wide ICMEs of low masses adjust to the solar-wind speed already close to the sun, so the transit time is determined primarily by the solar-wind speed. The shortest transit times and accordingly the highest 1 AU velocities are related to narrow and massive ICMEs (i.e. high-density eruptions) propagating in high-speed solar wind streams. We apply the model to the Sun-Earth event associated with the CME of 25 July 2004 and compare the results with the outcome of the numerical MHD modeling.

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A simplified model for timing the arrival of solar flare‐initiated shocks

Cited by 121 publications

References 37 publications

The Physical Processes of CME/ICME Evolution

The Physical Processes of CME/ICME Evolution

Longitudinal Properties of a Widespread Solar Energetic Particle Event on 2014 February 25: Evolution of the Associated Cme Shock

The role of aerodynamic drag in propagation of interplanetary coronal mass ejections

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