Refinements to flare energy estimates: A followup to “Energy partition in two solar flare/CME events” by A. G. Emslie et al.

By A. Emslie, Brian R. Dennis, Gordon D. Holman, H. Hudson. 2005

159 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/849a3c8d7f2a2c8be87dd8846ee96312dfa8f6f3

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In Astronomy and Astrophysics

Citations in the corpus

Hard X-ray emission from the solar corona (2008, background): “We note that the fraction of flare energy that eventually appears in particles accelerated by the CME-driven shock may be large (of order 10 %; see Emslie et al 2005; Mewaldt et al 2005).”
TOWARD RELIABLE BENCHMARKING OF SOLAR FLARE FORECASTING METHODS (2012, background): “However, complete flare forecasts will require a deeper physical understanding of magnetic energy release and partitioning of energy between flare emission at different temperatures, acceleration of CMEs, and acceleration of high-energy particles (Emslie et al. 2005).”
GLOBAL ENERGETICS OF THIRTY-EIGHT LARGE SOLAR ERUPTIVE EVENTS (2012, methodology): “It is important to realize (Emslie et al. 2005) that these four components are not separate flare energy components and therefore cannot be summed together to obtain a total flare thermal energy.”
Acceleration in Fast Halo CMEs and Synchronized Flare HXR Bursts (2008, unknown): “…of electrons accelerated during a flare, and since a large fraction of the flare energy goes into fast particles (e.g., Dennis et al. 2003; Emslie et al. 2005), our results provide strong evidence for a feedback relationship between the largescale CME acceleration and the energy release…”
Highly Efficient Modeling of Dynamic Coronal Loops (2005, background): “It is thought, for example, that a sizable fraction of the total energy of a flare goes into nonthermal electrons (Saint-Hilaire & Benz 2002; Emslie et al. 2005).”
Global Properties of Solar Flares (2011, background): “We also have the evidence from hard X-rays, γ-rays, and solar energetic particles that particle acceleration plays a major role in energy transport The thick-target model invoking electrons (Neupert 1968; Kane and Donnelly 1971; Brown 1971; Hudson 1972) resulted naturally from these requirements.”
The standard flare model in three dimensions - I. Strong-to-weak shear transition in post-flare loops (2012, background): “On the one hand, the modeled energy values are typical of those estimated in solar flares (Emslie et al. 2005; Fletcher et al. 2011) and CMEs (Vourlidas et al. 2000, 2010).”
The standard flare model in three dimensions II: upper limit on solar flare energy (2012, background): “But current observational energy estimates imply that the kinetic energy of a CME can be the same as (Emslie et al. 2005) and up to three times higher than (Emslie et al. 2012) the bolometric energy of its associated flare.”
An Observational Overview of Solar Flares (2011, methodology): “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).”