Multi-Point Shock and Flux Rope Analysis of Multiple Interplanetary Coronal Mass Ejections Around 2010 August 1 in the Inner Heliosphere

Möstl, Christian; Farrugia, Charles J.; Kilpua, Emilia; Jian, L. K.; Liu, Ying D.; Eastwood, J. P.; Harrison, R. A.; Webb, D. F.; Temmer, Manuela; Odstrčil, D.; Davies, J. A.; Rollett, T.; Luhmann, J. G.; Nitta, N.; Mulligan, T.; Jensen, E. A.; Forsyth, R. J.; Lavraud, B.; Koning, C. A. de; Veronig, Astrid; Galvin, A. B.; Zhang, T. L.; Anderson, B. J.

doi:10.1088/0004-637x/758/1/10

Cited by 127 publications

(112 citation statements)

References 96 publications

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“…So far, the largest number of spacecraft crossings remains the event of January 1978 with five spacecraft crossings. Burlaga et al (1981) deduced a general shape for the shock and the MC axis, which are still the expected typical shapes nowadays (Möstl et al 2012;Janvier et al 2013). Berdichevsky et al (2009) reanalyzed the same event and concluded that there was a strong speed gradient in longitude with a stronger speed around the apex than on the flanks of the shock.…”

Section: Introductionmentioning

confidence: 79%

“…This provides an implicit constraint on the mean longitudinal extension of ICME shocks. Next, a limited sample of ICMEs have been analyzed by the STEREO twin spacecraft associated to other spacecraft, such as ACE, MESSENGER, VEX, or Wind (Kilpua et al 2011;Farrugia et al 2011;Möstl et al 2012). These studies provide constraints on the spatial extension and geometry of shocks in specific events.…”

Section: Introductionmentioning

confidence: 99%

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Mean shape of interplanetary shocks deduced from in situ observations and its relation with interplanetary CMEs

Janvier

Démoulin

Dasso

2014

A&A

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Context. Shocks are frequently detected by spacecraft in the interplanetary space. However, the in situ data of a shock do not provide direct information on its overall properties even when a following interplanetary coronal mass ejection (ICME) is detected. Aims. The main aim of this study is to constrain the general shape of ICME shocks with a statistical study of shock orientations. Methods. We first associated a set of shocks detected near Earth over 10 years with a sample of ICMEs over the same period. We then analyzed the correlations between shock and ICME parameters and studied the statistical distributions of the local shock normal orientation. Supposing that shocks are uniformly detected all over their surface projected on the 1 AU sphere, we compared the shock normal distribution with synthetic distributions derived from an analytical shock shape model. Inversely, we derived a direct method to compute the typical general shape of ICME shocks by integrating observed distributions of the shock normal. Results. We found very similar properties between shocks with and without an in situ detected ICME, so that most of the shocks detected at 1 AU are ICME-driven even when no ICME is detected. The statistical orientation of shock normals is compatible with a mean shape having a rotation symmetry around the Sun-apex line. The analytically modeled shape captures the main characteristics of the observed shock normal distribution. Next, by directly integrating the observed distribution, we derived the mean shock shape, which is found to be comparable for shocks with and without a detected ICME and weakly affected by the limited statistics of the observed distribution. We finally found a close correspondence between this statistical result and the leading edge of the ICME sheath that is observed with STEREO imagers. Conclusions. We have derived a mean shock shape that only depends on one free parameter. This mean shape can be used in various contexts, such as studies for high-energy particles or space weather forecasts.

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Section: Introductionmentioning

confidence: 79%

Section: Introductionmentioning

confidence: 99%

Mean shape of interplanetary shocks deduced from in situ observations and its relation with interplanetary CMEs

Janvier

Démoulin

Dasso

2014

A&A

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“…When propagating into the solar wind, sympathetic events are prone to CME-CME interaction (e.g., Lugaz et al 2008Lugaz et al , 2012Liu et al 2014b). Such interactions may significantly modify the structure of the CME-driven shock wave and the properties of the interplanetary CME (ICME), and therefore affect the potential of space weather effects (e.g., Liu et al 2012Liu et al , 2014aMöstl et al 2012). Interactions between CMEs from the same AR have often been discussed (e.g., Lugaz et al 2005bLugaz et al , 2007Lugaz et al , 2013Xiong et al 2006), but CMEs can be spatially extended and those from distant regions may also interact, adding complexity to solar wind data (e.g., Temmer et al 2012).…”

Section: Introductionmentioning

confidence: 99%

A Numerical Study of Long-Range Magnetic Impacts During Coronal Mass Ejections

Jin

Schrijver

Cheung

et al. 2016

ApJ

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With the global view and high-cadence observations from Solar Dynamics Observatory/Atmospheric Imaging Assembly and Solar TErrestrial RElations Observatory, many spatially separated solar eruptive events appear to be coupled. However, the mechanisms for "sympathetic" events are still largely unknown. In this study, we investigate the impact of an erupting flux rope on surrounding solar structures through large-scale magnetic coupling. We build a realistic environment of the solar corona on 2011 February 15 using a global magnetohydrodynamics model and initiate coronal mass ejections (CMEs) in active region 11158 by inserting Gibson-Low analytical flux ropes. We show that a CME's impact on the surrounding structures depends not only on the magnetic strength of these structures and their distance to the source region, but also on the interaction between the CME and the large-scale magnetic field. Within the CME expansion domain where the flux rope field directly interacts with the solar structures, expansion-induced reconnection often modifies the overlying field, thereby increasing the decay index. This effect may provide a primary coupling mechanism underlying the sympathetic eruptions. The magnitude of the impact is found to depend on the orientation of the erupting flux rope, with the largest impacts occurring when the flux rope is favorably oriented for reconnecting with the surrounding regions. Outside the CME expansion domain, the influence of the CME is mainly through field line compression or post-eruption relaxation. Based on our numerical experiments, we discuss a way to quantify the eruption impact, which could be useful for forecasting purposes.

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“…Such a distortion occurs over a relatively short heliocentric distance. Interactions between multiple CMEs have been revealed by in situ observations (e.g., Burlaga et al 1987;Wang et al 2003;Steed et al 2011;Möstl et al 2012), radio burst observations (e.g., Gopalswamy et al 2001;Oliveros et al 2012), white light (WL) imaging (e.g., Harrison et al 2012;Liu et al 2012;Lugaz et al 2012;Temmer et al 2012;Shen et al 2012a;Bemporad et al 2012), and numerical magnetohydrodynamic (MHD) simulations (e.g., Lugaz et al 2005;Xiong et al 2007Xiong et al , 2009; Shen et al 2012b). …”

Section: The Inner Heliospherementioning

confidence: 99%

Using Coordinated Observations in Polarized White Light and Faraday Rotation to Probe the Spatial Position and Magnetic Field of an Interplanetary Sheath

Xiong

Davies

Feng

et al. 2013

ApJ

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Coronal mass ejections (CMEs) can be continuously tracked through a large portion of the inner heliosphere by direct imaging in visible and radio wavebands. White light (WL) signatures of solar wind transients, such as CMEs, result from Thomson scattering of sunlight by free electrons and therefore depend on both viewing geometry and electron density. The Faraday rotation (FR) of radio waves from extragalactic pulsars and quasars, which arises due to the presence of such solar wind features, depends on the line-of-sight magnetic field component B and the electron density. To understand coordinated WL and FR observations of CMEs, we perform forward magnetohydrodynamic modeling of an Earth-directed shock and synthesize the signatures that would be remotely sensed at a number of widely distributed vantage points in the inner heliosphere. Removal of the background solar wind contribution reveals the shock-associated enhancements in WL and FR. While the efficiency of Thomson scattering depends on scattering angle, WL radiance I decreases with heliocentric distance r roughly according to the expression I ∝ r −3 . The sheath region downstream of the Earth-directed shock is well viewed from the L4 and L5 Lagrangian points, demonstrating the benefits of these points in terms of space weather forecasting. The spatial position of the main scattering site r sheath and the mass of plasma at that position M sheath can be inferred from the polarization of the shock-associated enhancement in WL radiance. From the FR measurements, the local B sheath at r sheath can then be estimated. Simultaneous observations in polarized WL and FR can not only be used to detect CMEs, but also to diagnose their plasma and magnetic field properties.

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Multi-Point Shock and Flux Rope Analysis of Multiple Interplanetary Coronal Mass Ejections Around 2010 August 1 in the Inner Heliosphere

Cited by 127 publications

References 96 publications

Mean shape of interplanetary shocks deduced from in situ observations and its relation with interplanetary CMEs

Mean shape of interplanetary shocks deduced from in situ observations and its relation with interplanetary CMEs

A Numerical Study of Long-Range Magnetic Impacts During Coronal Mass Ejections

Using Coordinated Observations in Polarized White Light and Faraday Rotation to Probe the Spatial Position and Magnetic Field of an Interplanetary Sheath

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