Preliminary three‐dimensional analysis of the heliospheric response to the 28 October 2003 CME using SMEI white‐light observations

Jackson, B. V.; Buffington, A.; Hick, P. P.; Wang, X.; Webb, D. F.

doi:10.1029/2004ja010942

Cited by 84 publications

(92 citation statements)

References 33 publications

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“…In the case of our simulation, we believe that the CME mass increases faster than what is observed because of the excess speed of the CME. For the observed event, the (excess) mass continues to increase by almost an order of magnitude, to 13:6 ; 10 16 g as measured with SMEI on October 29, 12:00 UT, as the CME passed the Earth (Jackson et al 2006). …”

Section: Cme Massmentioning

confidence: 99%

“…For this event, flare loops were observed by TRACE (Su et al 2006), and the global coronal field has been reconstructed from data taken from the Michelson Doppler Imager (MDI) aboard the Solar and Heliospheric Observatory (SOHO) spacecraft ( Liu & Hayashi 2006). Dense plasma associated with the October 28 CME has been observed to propagate past the Earth by the Solar Mass Ejection Imager (SMEI; Jackson et al 2006) and was also detected by interplanetary scintillation (Tokumaru et al 2007). Finally, the event was observed in situ by Wind and the Advanced Composition Explorer (ACE; Skoug et al 2004;Zurbuchen et al 2004), which reveal magnetohydrodynamic (MHD) quantities in the solar wind as well as ion abundances.…”

Section: Introductionmentioning

confidence: 99%

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Three‐dimensional MHD Simulation of the 2003 October 28 Coronal Mass Ejection: Comparison with LASCO Coronagraph Observations

Manchester

Vourlidas

Tóth

et al. 2008

Astrophysical Journal

155

118

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We numerically model the coronal mass ejection (CME) event of 2003 October 28 that erupted from AR 10486 and propagated to Earth in less than 20 hr, causing severe geomagnetic storms. The magnetohydrodynamic (MHD) model is formulated by first arriving at a steady state corona and solar wind employing synoptic magnetograms. We initiate two CMEs from the same active region, one approximately a day earlier that preconditions the solar wind for the much faster CME on the 28th. This second CME travels through the corona at a rate of over 2500 km s À1 , driving a strong forward shock. We clearly identify this shock in an image produced by the Large Angle Spectrometric Coronagraph (LASCO) C3 and reproduce the shock and its appearance in synthetic white-light images from the simulation. We find excellent agreement with both the general morphology and the quantitative brightness of the model CME with LASCO observations. These results demonstrate that the CME shape is largely determined by its interaction with the ambient solar wind and may not be sensitive to the initiation process. We then show how the CME would appear as observed by wide-angle coronagraphs on board the Solar Terrestrial Relations Observatory (STEREO) spacecraft. We find complex time evolution of the white-light images as a result of the way in which the density structures pass through the Thomson sphere. The simulation is performed with the Space Weather Modeling Framework (SWMF).

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Section: Cme Massmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Three‐dimensional MHD Simulation of the 2003 October 28 Coronal Mass Ejection: Comparison with LASCO Coronagraph Observations

Manchester

Vourlidas

Tóth

et al. 2008

Astrophysical Journal

155

118

View full text Add to dashboard Cite

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“…Note that GSE longitude is the angle from the x-axis to the y-axis, and the latitude is the angle from the x -y plane. Figure 3 shows the three-dimensional (3-D) electron density field reconstructed from SMEI data just as the ICME transits Earth (Jackson et al, 2006). Densities between 10 cm −3 and 30 cm −3 with a 1/R 2 gradient removed are shown.…”

Section: Mulligan -Russell Model Inversionmentioning

confidence: 99%

“…SMEI electron density reconstruction just as the ICME transits Earth. Densities are contoured between 10 cm −3 and 30 cm −3 with a 1/R 2 gradient removed (Jackson et al, 2006). "Can" diagram of the rope orientation for the magnetic flux rope fit is superposed; note the overall shape and orientation of the axial dipole field line is similar to that of the dense loop structure.…”

Section: Modeling the Fr Response From A Cme/icmementioning

confidence: 99%

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Faraday Rotation Response to Coronal Mass Ejection Structure

et al. 2010

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We present the results from modeling the coronal mass ejection (CME) properties that have an effect on the Faraday rotation (FR) signatures that may be measured with an imaging radio antenna array such as the Murchison Widefield Array (MWA). These include the magnetic flux rope orientation, handedness, magnetic-field magnitude, velocity, radius, expansion rate, electron density, and the presence of a shock/sheath region. We find that simultaneous multiple radio source observations (FR imaging) can be used to uniquely determine the orientation of the magnetic field in a CME, increase the advance warning time on the geoeffectiveness of a CME by an order of magnitude from the warning time possible from in-situ observations at L 1 , and investigate the extent and structure of the shock/sheath region at the leading edge of fast CMEs. The magnetic field of the heliosphere is largely "invisible" with only a fraction of the interplanetary magnetic-field lines convecting past the Earth; remote sensing the heliospheric magnetic field through FR imaging from the MWA will advance solar physics investigations into CME evolution and dynamics.

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MHD heliosphere with boundary conditions from a tomographic reconstruction using interplanetary scintillation data

et al. 2014

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Observations of interplanetary scintillation (IPS) provide a set of data that is used in estimating the solar wind parameters with reasonably good accuracy. Various tomography techniques have been developed to deconvolve the line-of-sight integration effects ingrained in observations of IPS to improve the accuracy of solar wind reconstructions. Among those, the time-dependent tomography developed at the University of California, San Diego (UCSD) is well known for its remarkable accuracy in reproducing the solar wind speed and density at Earth by iteratively fitting a kinematic solar wind model to observations of IPS and near-Earth spacecraft measurements. However, the kinematic model gradually breaks down as the distance from the Sun increases beyond the orbit of Earth. Therefore, it would be appropriate to use a more sophisticated model, such as a magnetohydrodynamics (MHD) model, to extend the kinematic solar wind reconstruction beyond the Earth's orbit and to the outer heliosphere. To test the suitability of this approach, we use boundary conditions provided by the UCSD time-dependent tomography to propagate the solar wind outward in a MHD model and compare the simulation results with in situ measurements and also with the corresponding kinematic solution. Interestingly, we find notable differences in proton radial velocity and number density at Earth and various locations in the inner heliosphere between the MHD results and both the in situ data and the kinematic solution. For example, at 1 AU, the MHD velocities are generally larger than the spacecraft data by up to 150 km s −1 , and the amplitude of density fluctuations is also markedly larger in the MHD solution. We show that the MHD model can deliver more reasonable results at Earth with an ad hoc adjustment of the inner boundary values. However, we conclude that the MHD model using the inner boundary conditions derived from kinematic simulations has little chance to match IPS and in situ data as well as the kinematic model does unless it too is iteratively fit to the observational data and measurements.

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Preliminary three‐dimensional analysis of the heliospheric response to the 28 October 2003 CME using SMEI white‐light observations

Cited by 84 publications

References 33 publications

Three‐dimensional MHD Simulation of the 2003 October 28 Coronal Mass Ejection: Comparison with LASCO Coronagraph Observations

Three‐dimensional MHD Simulation of the 2003 October 28 Coronal Mass Ejection: Comparison with LASCO Coronagraph Observations

Faraday Rotation Response to Coronal Mass Ejection Structure

MHD heliosphere with boundary conditions from a tomographic reconstruction using interplanetary scintillation data

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