The Proper Treatment of Coronal Mass Ejection Brightness: A New Methodology and Implications for Observations

By A. Vourlidas, R. Howard. 2006

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In Astronomy and Astrophysics

Citations in the corpus

A synoptic view of solar transient evolution in the inner heliosphere using the Heliospheric Imagers on STEREO (2009, background): “Another contributory factor would be the reduction in scattering efficiency if the transients diverge from the Thomson scatter sphere, the surface of maximum scattering [Vourlidas and Howard, 2006], as they propagate outward.”
The Wide-Field Imager for Solar Probe Plus (WISPR) (2014, background): “Vourlidas and Howard (2006) have shown that the observing geometry must be taken into account for the proper interpretation of coronagraph and heliospheric imager observations.”
Coronal Mass Ejections: Observations (2012, background): “This emission has an angular dependence which must be accounted for in the measured brightness (e.g., Billings, 1966; Vourlidas and Howard, 2006; Howard and Tappin, 2009).”
Heliospheric Images of the Solar Wind at Earth (2008, unknown): “For a given elongation angle , the main contribution to the Thomson scattered emission is expected to occur from the region that is closest to the Sun (Vourlidas & Howard 2006).”
GEOMETRIC TRIANGULATION OF IMAGING OBSERVATIONS TO TRACK CORONAL MASS EJECTIONS CONTINUOUSLY OUT TO 1 AU (2010, background): “Projection and Thomson-scattering effects may affect the tracks in the timeelongation maps in ways that are difficult to assess quantitatively without detailed modeling of the coronal brightness (Vourlidas & Howard 2006; Lugaz et al. 2008, 2009).”
Three-dimensional MHD Simulation of the 2003 October 28 Coronal Mass Ejection: Comparison with LASCO Coronagraph Observations (2008, background): “The reason the CME fades in and out is because of multiple crossings of the Thomson sphere by dense arcs that propagate through the field of view of HI2A as illustrated in Figure 10 (Vourlidas & Howard 2006).”
Interplanetary Coronal Mass Ejections Observed in the Heliosphere: 1. Review of Theory (2009, background): “Vourlidas and Howard (2006) showed that the locus of all points where χ = 90◦ formed a sphere with the Sun-observer line as the diameter (their Fig.”
Deriving the radial distances of wide coronal mass ejections from elongation measurements in the heliosphere - application to CME-CME interaction (2009, methodology): “Beyond COR-2 FOV, only STEREO-A/SECCHI observed these eruptions originating from an active region behind the eastern limb.”
COMPREHENSIVE ANALYSIS OF CORONAL MASS EJECTION MASS AND ENERGY PROPERTIES OVER A FULL SOLAR CYCLE (2010, background): “The emission mechanism, Thomson scattering, is well understood and the total and polarized brightness intensities can be easily calculated if the LOS electron distribution is known or can be estimated (Billings 1966; Hayes et al. 2001; Vourlidas & Howard 2006).”
CONNECTING SPEEDS, DIRECTIONS AND ARRIVAL TIMES OF 22 CORONAL MASS EJECTIONS FROM THE SUN TO 1 AU (2014, background): “This signal arises for a HI observer due to Thomson scattering of photospheric light off solar wind electrons, over a range of distances along the line-of-sight (Vourlidas & Howard 2006; Howard & DeForest 2012b).”
RECONSTRUCTING CORONAL MASS EJECTIONS WITH COORDINATED IMAGING AND IN SITU OBSERVATIONS: GLOBAL STRUCTURE, KINEMATICS, AND IMPLICATIONS FOR SPACE WEATHER FORECASTING (2010, background): “The brightest part of the CME to a spacecraft is the region (point P) where the CME intersects with the “Thomson surface”, a spherical front with the Sun-spacecraft line as the diameter which has the maximum Thomson scattering strength (Vourlidas & Howard 2006), as illustrated in Figure 15 (left).”