Direct Detection of a Coronal Mass Ejection-Associated Shock in Large Angle and Spectrometric Coronagraph Experiment White-Light Images

By A. Vourlidas, S. Wu, A. Wang, P. Subramanian, R. Howard. 2003

191 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/bafe86d902621c380ec245255e26c193f8d993f7

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In Astronomy and Astrophysics

Citations in the corpus

Ultraviolet spectroscopy of the extended solar corona (2006, methodology): “Vourlidas et al. (2003) show an example in which the observed electron density increase matches that predicted by an MHD model of a CME with appropriate velocity and angular width.”
Three-dimensional MHD Simulation of the 2003 October 28 Coronal Mass Ejection: Comparison with LASCO Coronagraph Observations (2008, background): “More recently, Vourlidas et al. (2003) observed a similar feature with LASCO that they identified as a shock wave.”
Global Properties of Solar Flares (2011, background): “The left panel (Vourlidas et al. 2003) illustrates the importance of the wave flank, while the event in the right panel (Ontiveros and Vourlidas 2009) has a disk-center origin that obscures this geometrically.”
THE LONGITUDINAL PROPERTIES OF A SOLAR ENERGETIC PARTICLE EVENT INVESTIGATED USING MODERN SOLAR IMAGING (2011, unknown): “Combined analysis of white-light images and numerical simulations showed evidence that the leading edges of these clouds may be the location of an outflowing shock (e.g., Vourlidas et al. 2003; Manchester et al. 2008).”
A Global Picture of CMEs in the Inner Heliosphere (2004, background): “Exceptions are the shock signatures observed by UVCS (Raymond et al., 2000) and white-light shock signatures (Sheeley et al., 2000; Vourlidas et al., 2003).”
QUANTITATIVE MEASUREMENTS OF CORONAL MASS EJECTION-DRIVEN SHOCKS FROM LASCO OBSERVATIONS (2008, methodology): “We note that the earlier paper by Vourlidas et al. (2003) discussed shock signatures related to rather small and fast events (such as surges and jets).”
Solar Orbiter (2012, background): “…studies of LASCO images obtained during the rising phase of Solar Cycle 23 have demonstrated the feasibility of detecting CME-driven shocks from a few to ∼20 RSun and of measuring their density compression ratio and propagation direction (Vourlidas et al., 2003; Ontiveros and Vourlidas, 2009).”
AUTOMATED LASCO CME CATALOG FOR SOLAR CYCLE 23: ARE CMEs SCALE INVARIANT? (2008, background): “Both physical and technical reasons account for a difference in detection of first appearance (both earlier and later), we list some of them below: [1] CMEs can drive waves or shocks ahead of them (e.g. Vourlidas et al. 2003).”
How Many CMEs Have Flux Ropes? Deciphering the Signatures of Shocks, Flux Ropes, and Prominences in Coronagraph Observations of CMEs (2012, methodology): “A certain number of the remaining events appear to be related to Hα and/or 304 Å surges similar to the event studied by Vourlidas et al. (2003).”
An Observational Overview of Solar Flares (2011, background): “Indeed, the coronagraphic observations show image evidence, in many cases, for CME-driven shocks in the middle corona (Vourlidas et al. 2003; Ontiveros & Vourlidas 2009).”
OBSERVATIONS AND INTERPRETATION OF A LOW CORONAL SHOCK WAVE OBSERVED IN THE EUV BY THE SDO/AIA (2011, background): “Coronal shocks have been identified from white light coronagraph images by morphology and density enhancement (e.g., Vourlidas et al. 2003; Ontiveros & Vourlidas 2009) and from UV spectra (Raymond et al. 2000; Mancuso & Bemporad 2009) by measuring oxygen kinetic temperatures.”
The Physical Processes of CME/ICME Evolution (2017, methodology): “Perhaps the most compelling observational evidence for shocks appearing in LASCO images is presented in Raymond et al. (2000), Mancuso et al. (2002), and Vourlidas et al. (2003).”
The association of coronal mass ejections with their effects near the Earth (2005, background): “These density waves are surprisingly difficult to detect optically even with the modern, most sensitive coronagraphs (Vourlidas et al., 2003).”