Three-dimensional reconstruction of heliospheric structure using iterative tomography: A review

Jackson, B. V.; Hick, P. P.; Buffington, A.; Bisi, M. M.; Clover, J. M.; Tokumaru, M.; Kojima, M.; Fujiki, K.

doi:10.1016/j.jastp.2010.10.007

Cited by 60 publications

(54 citation statements)

References 103 publications

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“…Workers have, however, been working with these difficulties for 50 years and a number of techniques have evolved to extract reliable CME measurements using IPS. Recent papers involving such measurements include Jones et al (2007), Bisi et al (2008), Jackson et al (2010b), Tappin and Howard (2010), and Manoharan (2010).…”

Section: Interplanetary Scintillation (Ips) Observationsmentioning

confidence: 99%

“…SMEI was used for CME tracking (Tappin et al, 2004;Webb et al, 2006;Howard et al, 2006Howard et al, , 2007, space weather forecasting Webb et al, 2009;Howard and Tappin, 2010), and 3-D reconstruction Jackson et al, 2010b). SMEI observations have been compared with coronagraph and in-situ spacecraft measurements (Tappin et al, 2004;Tappin, 2006;Howard et al, 2006Howard et al, , 2007Howard and Simnett, 2008;Webb et al, 2009) and compared with IPS observations (Jackson et al, 2008b;Bisi et al, 2008).…”

Section: Heliospheric Imagersmentioning

confidence: 99%

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Coronal Mass Ejections: Observations

Webb

Howard

2012

Living Rev. Solar Phys.

670

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: Interplanetary Scintillation (Ips) Observationsmentioning

confidence: 99%

Section: Heliospheric Imagersmentioning

confidence: 99%

Coronal Mass Ejections: Observations

Webb

Howard

2012

Living Rev. Solar Phys.

670

534

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“…The scintillations carry information about the speeds of small scale structures moving away from the Sun in the solar wind. There are several different tomographic methods that can be used to extract the three-dimensional structure from the scintillation data (e.g., see the reviews by Kojima et al 2007;Jackson et al 2011). However, near-Sun maps from these data must be created carefully, since the minimum distance of the source-receiver lines of sight for these measurements are typically at ∼20 R from the Sun (depending on frequency).…”

Section: Introductionmentioning

confidence: 99%

THE EVOLUTION OF PLASMA PARAMETERS ON A CORONAL SOURCE SURFACE AT 2.3R_☉DURING SOLAR MINIMUM

Strachan¹,

Panasyuk²,

Kohl³

et al. 2011

ApJ

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We analyze data from the Solar and Heliospheric Observatory to produce global maps of coronal outflow velocities and densities in the regions where the solar wind is undergoing acceleration. The maps use UV and white light coronal data obtained from the Ultraviolet Coronagraph Spectrometer and the Large Angle Spectroscopic Coronagraph, respectively, and a Doppler dimming analysis to determine the mean outflow velocities. The outflow velocities are defined on a sphere at 2.3 R from Sun-center and are organized by Carrington Rotations during the solar minimum period at the start of solar cycle 23. We use the outflow velocity and density maps to show that while the solar minimum corona is relatively stable during its early stages, the shrinkage of the north polar hole in the later stages leads to changes in both the global areal expansion of the coronal hole and the derived internal flux tube expansion factors of the solar wind. The polar hole areal expansion factor and the flux tube expansion factors (between the coronal base and 2.3 R ) start out as super-radial but then they become more nearly radial as the corona progresses away from solar minimum. The results also support the idea that the largest flux tube expansion factors are located near the coronal hole/streamer interface, at least during the deepest part of the solar minimum period.

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“…10 Elongation-time (ε-t ) plots for a single point moving in the equatorial plane, traveling with a speed of 1000 km/s, measured relative to an observer at the Earth looking at the Sun (Howard and Simnett 2008). Curves show changes in the ε-t plot as the longitude of the trajectory moves from near the Sun-Earth line (0 • ) to the solar limb (90 • ) , and reviewed in Jackson et al 2011b). This technique applies the known basic physics of the heliosphere and Computer Aided Tomography (CAT) techniques to heliospheric brightness viewed remotely.…”

Section: Three-dimensional Reconstruction Of Cmes and Resultsmentioning

confidence: 99%

“…Other SMEI work with CMEs includes comparison with interplanetary scintillation (IPS) radio data (e.g., Tokumaru et al 2007;Jackson et al 2007aJackson et al , 2007bJackson et al , 2011b, comparison with in-situ data (e.g., Jackson et al , 2011cWebb et al 2009bWebb et al , 2013, and space weather forecasting (Sect. 5.1).…”

Section: Coronal Mass Ejectionsmentioning

confidence: 99%

The Solar Mass Ejection Imager and Its Heliospheric Imaging Legacy

et al. 2013

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The Solar Mass Ejection Imager (SMEI) was the first of a new class of heliospheric and astronomical white-light imager. A heliospheric imager operates in a fashion similar to coronagraphs, in that it observes solar photospheric white light that has been Thomson scattered by free electrons in the solar wind plasma. coronagraphs, this imager differs in that it observes at much larger angles from the Sun. This in turn requires a much higher sensitivity and wider dynamic range for the measured intensity. SMEI was launched on the Coriolis spacecraft in January 2003 and was deactivated in September 2011, thus operating almost continuously for nearly nine years. Its primary objective was the observation of interplanetary transients, typically coronal mass ejections (CMEs), and tracking them continuously throughout the inner heliosphere. Towards this goal it was immediately effective, observing and tracking several CMEs in the first month of mission operations, with some 400 detections to follow. Along with this primary science objective, SMEI also contributed to many and varied scientific fields, including studies of corotating interaction regions (CIRs), the high-altitude aurora, zodiacal light, Gegenschein, comet tail disconnections and motions, and variable stars. It was also able to detect and track Earth-orbiting satellites and space debris. Along with its scientific advancements, SMEI also demonstrated a significantly improved accuracy of space weather prediction, thereby establishing the feasibility and usefulness of operational heliospheric imagers. In this paper we review the scientific and operational achievements of SMEI, discuss lessons learned, and present our view of potential next steps in future heliospheric imaging.

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Three-dimensional reconstruction of heliospheric structure using iterative tomography: A review

Cited by 60 publications

References 103 publications

Coronal Mass Ejections: Observations

Coronal Mass Ejections: Observations

THE EVOLUTION OF PLASMA PARAMETERS ON A CORONAL SOURCE SURFACE AT 2.3R_☉DURING SOLAR MINIMUM

The Solar Mass Ejection Imager and Its Heliospheric Imaging Legacy

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Three-dimensional reconstruction of heliospheric structure using iterative tomography: A review

Cited by 60 publications

References 103 publications

Coronal Mass Ejections: Observations

Coronal Mass Ejections: Observations

THE EVOLUTION OF PLASMA PARAMETERS ON A CORONAL SOURCE SURFACE AT 2.3R☉DURING SOLAR MINIMUM

The Solar Mass Ejection Imager and Its Heliospheric Imaging Legacy

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Product

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THE EVOLUTION OF PLASMA PARAMETERS ON A CORONAL SOURCE SURFACE AT 2.3R_☉DURING SOLAR MINIMUM