Energy partition in two solar flare/CME events

By A. Emslie, H. Kucharek, Brian R. Dennis, Nat Gopalswamy, Gordon D. Holman, G. Share, A. Vourlidas, T. Forbes, Peter T. Gallagher, G. Mason and 5 more. 2004

230 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/58b75b680a5983ee5dc17b029241d651de74a6fc

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In Astronomy and Astrophysics

1. M. Temmer
2. H. Hudson
3. D. Webb
4. T. Howard
5. Tibor Török
6. Nat Gopalswamy
7. T. Wiegelmann
8. S. Krucker

Citations in the corpus

• EVOLUTION OF MAGNETIC FIELD AND ENERGY IN A MAJOR ERUPTIVE ACTIVE REGION BASED ON SDO/HMI OBSERVATION (2011, methodology): “…heating, CME lift-off, and flare radiation are expected to be on the same order of magnitude, if not greater than the nonthermal electron energy (Emslie et al. 2004), the estimated total energy budget has to be on the order of 1032 erg. Based to this analysis, the computed pre-flare Ef (2.47 ×…”
• Proton, helium, and electron spectra during the large solar particle events of October-November 2003 (2005, background): “The double-power law representation of Band et al. [1993] was found to provide a better fit to these spectra than the more conventional spectral form due to Ellison and Ramaty [1985] .”
• Coronal Mass Ejections: Observations (2012, background): “However, the vast majority of the ejected energy assumes the form of mechanical energy carried by the CME and not the associated solar flare, even in the most energetic cases (Emslie et al., 2004).”
• GLOBAL ENERGETICS OF THIRTY-EIGHT LARGE SOLAR ERUPTIVE EVENTS (2012, methodology): “Finally, the SEP spectra in this study were integrated from 0.03 MeV nucleon−1 to 300 MeV nucleon−1, rather than from 0.01 MeV nucleon−1 to 1000 MeV nucleon−1 as in Emslie et al. (2004) and Mewaldt et al. (2005, 2008a).”
• RHESSI Microflare Statistics. II. X-Ray Imaging, Spectroscopy, and Energy Distributions (2007, background): “…in the few events with the largest nonthermal component are only 10%, so this cannot explain the fact that in some of these small flares the rate of energy release is comparable to larger flares, 1027Y 1030 erg s 1 (Holman 2003; Emslie et al. 2004; Saint-Hilaire & Benz 2005; Sui et al. 2005, 2007).”
• Implications of X-ray Observations for Electron Acceleration and Propagation in Solar Flares (2011, background): “Holman et al. (2003), Emslie et al. (2004), and Saint-Hilaire and Benz (2005), in determining the low-energy cutoff, obtained the “highest value for Ec that still fits the data.””
• Coronal mass ejections of solar cycle 23 (2006, background): “Up to 15% of the CME kinetic energy goes into the accelerated particles (Emslie et al. 2004), suggesting that the CME-driven shocks are efficient particle accelerators.”
• Confined and Ejective Eruptions of Kink-unstable Flux Ropes (2005, result): “The simulation shows a strong magnetic energy release, 25% of the initial value, which agrees with the magnitude observed in ejective solar eruptions (Forbes 2000; Emslie et al. 2004).”
• Magnetic Reconnection in Astrophysical and (2009, background): “…and postflare magnetic energies can be measured and compared with the energy in fast particles, it is found that the magnetic energy decrease during the flare is of the same order as the energy in fast particles (and also comparable to the energy associated with mass ejection; Emslie et al. 2004).”
• An Observational Overview of Solar Flares (2011, background): “The energetics of two X-class flares (SOL2002-04-21T01:51 and SOL2002-07-23T00:35) have been analyzed in a very comprehensive study made possible by overlapping observations at a variety of wavelengths (Emslie et al. 2004, 2005).”
• Refinements to flare energy estimates: A followup to “Energy partition in two solar flare/CME events” by A. G. Emslie et al. (2005, methodology): “Then the radiative loss rate from plasma at that temperature can be calculated using the Chianti version of the Cox and Tucker [1969] radiative cooling rates for coronal abundances.”
• WHY IS THE GREAT SOLAR ACTIVE REGION 12192 FLARE-RICH BUT CME-POOR? (2015, unknown): “A detailed analysis, similar to those performed on eruptive flares (e.g., Emslie et al. 2004; Feng et al. 2013), will be worthwhile and may shed light on the triggering mechanism.”
• A MAGNETIC RECONNECTION MECHANISM FOR ION ACCELERATION AND ABUNDANCE ENHANCEMENTS IN IMPULSIVE FLARES (2009, background): “On the other hand, the extraordinary efficiency of particle acceleration in flares (Lin & Hudson 1971; Emslie et al. 2004) requires that the wave generation mechanism in flares must also be very efficient—at present no mechanism with the required efficiency has been identified.”