Stereoscopic analysis of STEREO/SECCHI data for CME trajectory determination

Liewer, P. C.; Hall, J. R.; Howard, R. A.; Jong, E. M. De; Thompson, W. T.; Thernisien, A.

doi:10.1016/j.jastp.2010.09.004

Cited by 35 publications

(36 citation statements)

References 26 publications

(15 reference statements)

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“…The different viewpoints of the STEREO spacecraft were exploited to identify the location of the radio emission, relative to the CMEs and other interplanetary structures (see Figure 3). The heliographic coordinates of the CMEs front at different times were calculated by simultaneously selecting the same structures in both STEREO-A and -B images (tie-point method, Liewer et al, 2011) with specialized routines available in the SolarSoft package suite (Freeland and Handy, 1998). …”

Section: White-light Observationsmentioning

confidence: 99%

STEREO-Wind Radio Positioning of an Unusually Slow Drifting Event

et al. 2014

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On 13 March 2010 an unusually long duration event was observed by radio spectrographs onboard the STEREO-B and Wind spacecraft. The event started at about 13:00 UT and ended at approximately 06:00 UT on 14 March. The event presents itself as slow drifting, quasi-continuous emission in a very narrow frequency interval, with an apparent frequency drift from about 625 kHz to approximately 425 kHz. Using the Leblanc, Dulk, and Bougeret (1998) interplanetary density model we determined that the drift velocities of the radio source are ≈33 km s −1 and ≈52 km s −1 for 0.2 and 0.5 times the densities of Leblanc model, respectively with a normalization density of 7.2 cm −3 at 1AU and assuming harmonic emission. A joint analysis of the radio direction finding data, coronograph white-light observations and modeling revealed that the radio sources appear to be localized in regions of interaction with relatively high density and slow solar wind speed.

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Section: White-light Observationsmentioning

confidence: 99%

STEREO-Wind Radio Positioning of an Unusually Slow Drifting Event

et al. 2014

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“…Since we have observations from two viewpoints, we can quantify this effect because we can localize the prominence in 3D space. Tiepointing is the standard technique for this purpose and has been described before (Liewer et al, 2009;Liewer et al, 2011;Thompson, Kliem, and Török, 2012). The technique relies of the correct identification of the same structure in the two images.…”

Section: D Reconstruction Of the Erupting Prominence On 28 February mentioning

confidence: 99%

Origins of Rolling, Twisting, and Non-radial Propagation of Eruptive Solar Events

Martin¹,

Panasenco²

2012

Solar Dynamics and Magnetism From the Interior to the Atmosphere

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We demonstrate that major asymmetries in erupting filaments and CMEs, namely major twists and non-radial motions are typically related to the larger-scale ambient environment around eruptive events. Our analysis of prominence eruptions observed by the STEREO, SDO and SOHO spacecraft shows that prominence spines retain, during the initial phases, the thin ribbonlike topology they had prior to the eruption. This topology allows bending, rolling, and twisting during the early phase of the eruption, but not before. The combined ascent and initial bending of the filament ribbon is non-radial in the same general direction as for the enveloping CME. However, the non-radial motion of the filament is greater than that of the CME. In considering the global magnetic environment around CMEs, as approximated by the Potential Field Source Surface (PFSS) model, we find that the non-radial propagation of both erupting filaments and associated CMEs is correlated with the presence of nearby coronal holes, which deflect the erupting plasma and embedded fields. In addition, CME and filament motions respectively are guided towards weaker field regions, namely null points existing at different heights in the overlying configuration. Due to the presence of the coronal hole, the large-scale forces acting on the CME may be asymmetric. We find that the CME propagates usually non-radially in the direction of least resistance, which is always away from the coronal hole. We demonstrate these results using both low and high latitude examples.

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“…In addition to CME imaging (e.g., Thernisien et al 2009;Liewer et al 2010;Poomvises et al 2010;Mishra et al 2015), the wide-field imagers in SECCHI have yielded important results on the structure of the solar wind itself, including observation of small-scale periodic density enhancements convected out with the solar wind (Viall et al 2010;Rouillard et al 2011). More recent analyses include measurements of the outer limits of the corona and observations of the nascent stages of a stream interaction region (SIR; Stenborg & Howard 2017).…”

Section: Introductionmentioning

confidence: 99%

The Highly Structured Outer Solar Corona

DeForest

Howard

Velli

et al. 2018

ApJ

133

111

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We report on the observation of fine-scale structure in the outer corona at solar maximum, using deep-exposure campaign data from the Solar Terrestrial Relations Observatory-A (STEREO-A)/COR2 coronagraph coupled with postprocessing to further reduce noise and thereby improve effective spatial resolution. The processed images reveal radial structure with high density contrast at all observable scales down to the optical limit of the instrument, giving the corona a "woodgrain" appearance. Inferred density varies by an order of magnitude on spatial scales of 50 Mm and follows an f −1 spatial spectrum. The variations belie the notion of a smooth outer corona. They are inconsistent with a well-defined "Alfvén surface," indicating instead a more nuanced "Alfvén zone"-a broad trans-Alfvénic region rather than a simple boundary. Intermittent compact structures are also present at all observable scales, forming a size spectrum with the familiar "Sheeley blobs" at the large-scale end. We use these structures to track overall flow and acceleration, finding that it is highly inhomogeneous and accelerates gradually out to the limit of the COR2 field of view. Lagged autocorrelation of the corona has an enigmatic dip around 10 R e , perhaps pointing to new phenomena near this altitude. These results point toward a highly complex outer corona with far more structure and local dynamics than has been apparent. We discuss the impact of these results on solar and solar-wind physics and what future studies and measurements are necessary to build upon them.

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Stereoscopic analysis of STEREO/SECCHI data for CME trajectory determination

Cited by 35 publications

References 26 publications

STEREO-Wind Radio Positioning of an Unusually Slow Drifting Event

STEREO-Wind Radio Positioning of an Unusually Slow Drifting Event

Origins of Rolling, Twisting, and Non-radial Propagation of Eruptive Solar Events

The Highly Structured Outer Solar Corona

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