Hybrid Reconstruction to Derive 3D Height – Time Evolution for Coronal Mass Ejections

Antunes, A.; Thernisien, A.; Yahil, A.

doi:10.1007/s11207-009-9409-7

Cited by 20 publications

(18 citation statements)

References 19 publications

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“…Many workers have now devised geometrical techniques for determining 3-D information on CMEs, including forward modeling (e.g., Thernisien et al, 2006;, tie-pointing (e.g., Mierla et al, 2009), and inverse reconstruction (Antunes et al, 2009). Other triangulation efforts have also been made by (for example) de Koning et al (2009), Liewer et al (2009.…”

Section: Locations Widths Geometrymentioning

confidence: 99%

Coronal Mass Ejections: Observations

Webb

Howard

2012

Living Rev. Solar Phys.

641

534

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Solar eruptive phenomena embrace a variety of eruptions, including flares, solar energetic particles, and radio bursts. Since the vast majority of these are associated with the eruption, development, and evolution of coronal mass ejections (CMEs), we focus on CME observations in this review. CMEs are a key aspect of coronal and interplanetary dynamics. They inject large quantities of mass and magnetic flux into the heliosphere, causing major transient disturbances. CMEs can drive interplanetary shocks, a key source of solar energetic particles and are known to be the major contributor to severe space weather at the Earth. Studies over the past decade using the data sets from (among others) the SOHO, TRACE, Wind, ACE, STEREO, and SDO spacecraft, along with ground-based instruments, have improved our knowledge of the origins and development of CMEs at the Sun and how they contribute to space weather at Earth. SOHO, launched in 1995, has provided us with almost continuous coverage of the solar corona over more than a complete solar cycle, and the heliospheric imagers SMEI (2003 -2011) and the HIs (operating since early 2007) have provided us with the capability to image and track CMEs continually across the inner heliosphere. We review some key coronal properties of CMEs, their source regions and their propagation through the solar wind. The LASCO coronagraphs routinely observe CMEs launched along the Sun-Earth line as halo-like brightenings. STEREO also permits observing Earth-directed CMEs from three different viewpoints of increasing azimuthal separation, thereby enabling the estimation of their three-dimensional properties. These are important not only for space weather prediction purposes, but also for understanding the development and internal structure of CMEs since we view their source regions on the solar disk and can measure their in-situ characteristics along their axes. Included in our discussion of the recent developments in CME-related phenomena are the latest developments from the STEREO and LASCO coronagraphs and the SMEI and HI heliospheric imagers.

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Section: Locations Widths Geometrymentioning

confidence: 99%

Coronal Mass Ejections: Observations

Webb

Howard

2012

Living Rev. Solar Phys.

641

534

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“…Attempts to infer the 3-D structure have also been done by several authors (e.g. Antunes et al, 2009;Mierla et al, 2009;Moran et al, 2010;Thernisien et al, 2009;Wood et al, 2009); however, as pointed out earlier many assumptions need to be considered in order to get a unique solution. One such assumption is that CMEs expand radially and in a self-similar fashion as they propagate outwards (e.g.…”

Section: Reconstruction Techniquesmentioning

confidence: 99%

“…In essence, inverse modeling is underconstrained and forward modeling is overconstrained. Antunes et al (2009) have used a hybrid method by combining inversion with forward modeling in order to infer the 3-D structure of CMEs recorded by STEREO. The authors used the PIXON method to reconstruct this density distribution, which is based on minimizing the number of electron density volumetric elements necessary to reproduce the observations.…”

Section: Forward Modeling and Inverse Reconstructionmentioning

confidence: 99%

On the 3-D reconstruction of Coronal Mass Ejections using coronagraph data

et al. 2010

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Abstract. Coronal Mass ejections (CMEs) are enormous eruptions of magnetized plasma expelled from the Sun into the interplanetary space, over the course of hours to days. They can create major disturbances in the interplanetary medium and trigger severe magnetic storms when they collide with the Earth's magnetosphere. It is important to know their real speed, propagation direction and 3-D configuration in order to accurately predict their arrival time at the Earth. Using data from the SECCHI coronagraphs onboard the STEREO mission, which was launched in October 2006, we can infer the propagation direction and the 3-D structure of such events. In this review, we first describe different techniques that were used to model the 3-D configuration of CMEs in the coronagraph field of view (up to 15 R ).Correspondence to: M. Mierla (mmierla@gmail.com) Then, we apply these techniques to different CMEs observed by various coronagraphs. A comparison of results obtained from the application of different reconstruction algorithms is presented and discussed.

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“…The SMEI instrument records the white-light Thomson scattering of the coronal density structures, while IPS measurements are used to constrain the location of the density along the lines of sight. Finally, the Pixon technique, primarily developed for image restoration (Puetter, Gosnell, and Yahil, 2005), has been used by Antunes, Thernisien, and Yahil (2009) to reconstruct the CME event of 31 December 2007 from the STEREO/SECCHI observations. They were able to determine the kinematics of the upper and lower components of this highly distorted flux-rope event.…”

Section: Introductionmentioning

confidence: 99%

Forward Modeling of Coronal Mass Ejections Using STEREO/SECCHI Data

2009

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We describe a forward modeling method developed to study the coronal mass ejections observed with STEREO/SECCHI. We present a survey of 26 CMEs modeled with this method. We selected most of the bright events observed since November 2007 to August 2008, after when the separation was greater than 40°degrees, thus showing noticeable differences between the two views. From these stereoscopic observations and using a geometric model of a flux rope, we are able to determine the three-dimensional direction of propagation, the three-dimensional velocity and acceleration of the CME front, and in most of the cases the flux rope orientation and length. We define a merit function that allows us to partially automate the fit, as well as perform a sensitivity analysis on the model parameters. We find a precision on the longitude and latitude to be of a maximum of ±17°a nd ±4°, respectively, for a 10% decrease of the merit function but a precision on the flux rope orientation and length to be almost one order of magnitude larger, showing that these parameters are more difficult to estimate using only coronagraph data. Finally, comparison with independent measurements shows a good agreement with the direction and speed we estimated.

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Hybrid Reconstruction to Derive 3D Height – Time Evolution for Coronal Mass Ejections

Cited by 20 publications

References 19 publications

Coronal Mass Ejections: Observations

Coronal Mass Ejections: Observations

On the 3-D reconstruction of Coronal Mass Ejections using coronagraph data

Forward Modeling of Coronal Mass Ejections Using STEREO/SECCHI Data

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