Faraday Rotation Response to Coronal Mass Ejection Structure

Jensen, E. A.; Hick, P. P.; Bisi, M. M.; Jackson, B. V.; Clover, J. M.; Mulligan, T.

doi:10.1007/s11207-010-9543-2

Cited by 27 publications

(27 citation statements)

References 19 publications

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“…In these analyses, various portions of the CME response were measured (the shock sheath, the erupting prominence material), and compared with equivalent portions of the CME in coronagraph observations. In the analysis of the 28 October 2003 CME, showed that the prominence material of the CME is elongated in the direction of the Earth, and approximates the loop-like magnetic field structure measured in-situ at Earth for this event (Jensen et al 2010;Jackson et al 2011a). The SMEI reconstructions agreed well with in situ density measurements at Earth and STEREO (e.g., Jackson et al , 2010bJackson et al , 2012.…”

Section: Three-dimensional Reconstruction Of Cmes and Resultsmentioning

confidence: 52%

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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Section: Three-dimensional Reconstruction Of Cmes and Resultsmentioning

confidence: 52%

The Solar Mass Ejection Imager and Its Heliospheric Imaging Legacy

et al. 2013

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“…to determine the distance of the heliospheric interstellar boundary, or the dynamic solar wind pressure at Mars, and its effect on the Martian magnetosphere . In combination with Faraday rotation (FR) observations, bulk densities allow the remote determination of heliospheric vector magnetic field components globally (Jensen et al, 2010). This combination of bulk density measurements combined with FR observations planned from radio arrays such as the Murchison Widefield Array (MWA) or the LOw Frequency ARray (LOFAR) now under construction may usher in a whole new remote-sensing capability.…”

Section: Discussionmentioning

confidence: 99%

A Heliospheric Imager for Deep Space: Lessons Learned from Helios, SMEI, and STEREO

et al. 2010

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The zodiacal-light photometers on the twin Helios spacecraft, the Solar Mass Ejection Imager (SMEI) on the Coriolis spacecraft, and the Heliospheric Imagers (HIs) on the Solar-TErrestrial RElations Observatory (STEREO) twin spacecraft all point the way to optimizing future remote-sensing Thomson-scattering observations from deep space. Such data could be provided by wide-angle viewing instruments on Solar Orbiter, Solar Probe, or other deep-space probes. Here, we present instrument specifications required for a successful heliospheric imager, and the measurements and data-processing steps that make the best use of this remote-sensing system. When this type of instrument is properly designed and calibrated, its data are capable of determining zodiacal-dust properties, and of threedimensional reconstructions of heliospheric electron density over large volumes of the inner heliosphere. Such systems can measure fundamental properties of the inner heliospheric plasma, provide context for the in-situ monitors on board spacecraft, and enable physicsbased analyses of this important segment of the Sun-spacecraft connection.Remote Sensing of the Inner Heliosphere

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“…Analysis of the magnetic field perturbation of the 1983 Alfven perturbations inferred that the efflux energy at 4 solar radii was at least 6×10 19 W. It approximately accounts for 20% of the wave energy required to accelerate the solar wind (Jensen & Russell 2009). Further, the Faraday rotation observations of CME/ICMEs have demonstrated the usefulness of determining the critical parameters, such as the orientation and radius of a flux cylinder in the interplanetary space (Jensen et al 2010).…”

Section: Turbulence In the Fast/slow Solar Wind Flowsmentioning

confidence: 99%

Commission 49: Interplanetary Plasma and Heliosphere

Gopalswamy¹,

Mann²,

Bougeret³

et al. 2011

Proc. IAU

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Commission 49 (Interplanetary Plasma and Heliosphere) is part of IAU Division II (Sun and Heliosphere). The research topics include large-scale solar disturbances such as coronal mass ejections (CMEs), shocks, and corotating interaction regions (CIRs) propagating into the heliosphere. The disturbances propagate through the solar wind, which essentially defines the heliosphere. The solar disturbances provide large-scale laboratory to study plasma processes over various time and spatial scales, the highest spatial scale being the size of the heliosphere itself (~100 AU). These solar disturbances are related to solar activity in the form of active regions and coronal holes. Solar eruptions are accompanied by particle acceleration and the particles can be hazardous to life on earth in various ways from modifying the ionosphere to damaging space technology and increasing lifetime radiation dosage to astronauts and airplane crew. Particle acceleration in solar eruptions poses fundamental physics questions because the underlying mechanisms are not fully understood. One of important processes is the particle acceleration by shocks, which occurs throughout the heliosphere. The heliosphere has both neutral and ionized material, with interesting interaction between the two components.

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Faraday Rotation Response to Coronal Mass Ejection Structure

Cited by 27 publications

References 19 publications

The Solar Mass Ejection Imager and Its Heliospheric Imaging Legacy

The Solar Mass Ejection Imager and Its Heliospheric Imaging Legacy

A Heliospheric Imager for Deep Space: Lessons Learned from Helios, SMEI, and STEREO

Commission 49: Interplanetary Plasma and Heliosphere

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