Large-Angle Spectrometric Coronagraph Measurements of the Energetics of Coronal Mass Ejections

By A. Vourlidas, P. Subramanian, K. Dere, R. Howard. 2000

256 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/8f3d748b169fb8294a9e56e0b32e5f4f22534245

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In Astronomy and Astrophysics

1. M. Temmer
2. A. Vourlidas
3. Nat Gopalswamy
4. N. Lugaz
5. W. Manchester IV
6. R. Howard
7. H. Hudson
8. S. Yashiro

Citations in the corpus

• Ultraviolet spectroscopy of the extended solar corona (2006, background): “Coronal mass ejections (CMEs) are dramatic eruptions of prominence and coronal plasma at speeds ranging from 100 to 2500 km s , and typical masses are 10 to 10 g (e.g., Sheeley et al. 1999; Vourlidas et al. 2000; Yashiro et al. 2004).”
• A Statistical Study of Main and Residual Accelerations of Coronal Mass Ejections (2006, background): “…effect is due to the angular-dependence of the electron Thomson scattering: the scattering is less efficient when an electron is further away from the plane of the sky (Vourlidas et al. 2000) In Table 1 we list the observed properties of the 50 events selected in the order of observation date.”
• Visibility of coronal mass ejections as a function of flare location and intensity (2005, background): “Therefore the detection efficiency of the Earthdirected CMEs is lower, since the CMEs are farther from the Sun when the CME material reaches above the coronagraph occulting disk (see Appendix A of Hundhausen [1993], Vourlidas et al. [2000] , and Andrews [2002] for details).”
• Global Properties of Solar Flares (2011, background): “The CME in particular contains a great deal of kinetic energy (e.g., Vourlidas et al. 2000); Emslie et al. (2005) show, for two major flares (the RHESSI flares of SOL2002-04-21T01:51 and SOL200207-23T00:35), that the CME kinetic energy is of the same order of magnitude as the radiated energy.”
• COMPREHENSIVE ANALYSIS OF CORONAL MASS EJECTION MASS AND ENERGY PROPERTIES OVER A FULL SOLAR CYCLE (2010, methodology): “Second, the final mass is underestimated by only ∼ 2x as was shown by calculations (Vourlidas et al. 2000), models (Lugaz et al. 2005) and more recently by stereoscopic mass measurements (Colaninno & Vourlidas 2009).”
• The Interaction of Successive Coronal Mass Ejections: A Review (2016, background): “Trigger and Initiation of CMEs As the largest explosive phenomenon on the Sun, a typical CME carries about 1032 erg of energy (Vourlidas et al., 2000; Hudson, Bougeret, and Burkepile, 2006) and 1021 Mx of magnetic flux (Dasso et al., 2005; Qiu et al., 2007; Wang et al., 2015) into IP space,…”
• Three-dimensional MHD Simulation of the 2003 October 28 Coronal Mass Ejection: Comparison with LASCO Coronagraph Observations (2008, background): “However, the mass increase seen in LASCO observations is attributed to mass entering the coronagraph field of view from below the occulter (Vourlidas et al. 2000).”
• Energy partition in two solar flare/CME events (2004, methodology): “From the mass, projected velocity, and position data follow estimates of the total kinetic (UK) and potential (UF) energies [Vourlidas et al., 2000].”
• The standard flare model in three dimensions - I. Strong-to-weak shear transition in post-flare loops (2012, background): “Key words. magnetic reconnection – magnetohydrodynamics (MHD) – Sun: coronal mass ejections (CMEs) – Sun: flares – Sun: UV radiation”
• An Observational Overview of Solar Flares (2011, background): “These observations permit an estimate of the mass distribution of the CME (Poland et al. 1981; Vourlidas et al. 2000, 2002).”
• QUANTITATIVE MEASUREMENTS OF CORONAL MASS EJECTION-DRIVEN SHOCKS FROM LASCO OBSERVATIONS (2008, methodology): “These are calibrated images from which a pre-event has been subtracted thus removing the background corona (Vourlidas et al. 2000).”
• GLOBAL ENERGETICS OF THIRTY-EIGHT LARGE SOLAR ERUPTIVE EVENTS (2012, background): “This excess brightness can therefore be converted to excess mass of the CME under the usual assumptions that (1) all of the CME mass is concentrated on the plane of the sky, and (2) the CME material consists of 90% H and 10% He (Poland et al. 1981; Vourlidas et al. 2000, 2010).”
• NO TRACE LEFT BEHIND: STEREO OBSERVATION OF A CORONAL MASS EJECTION WITHOUT LOW CORONAL SIGNATURES (2009, background): “Standard assumptions in mass measurements are (1) that all of the CME material is located in the plane of the sky (therefore, it gives a lower limit for the true CME mass) and (2) that the corona is completely ionized (Vourlidas et al. 2000).”
• The Role of Magnetic Reconnection in the Observable Features of Solar Eruptions (2004, result): “The value of tor deduced here is comparable to the observational results obtained by Lepping et al. (1997) and Vourlidas et al. (2000), which are 7:5 1020 and 1:3 1021 Mx on average, respectively.”
• On the three-dimensional configuration of coronal mass ejections (2004, background): “…bubbles, arcades comprised of Article published by EDP Sciences and available at http://www.aanda.org or http://dx.doi.org/10.1051/0004-6361:20035776 loops, or curved flux tubes (e.g. Crifo et al. 1983; Schwenn 1986; MacQueen 1993; Vourlidas et al. 2000; Plunkett et al. 2000; Zhao et al. 2002).”