Electron Bremsstrahlung Hard X-Ray Spectra, Electron Distributions, and Energetics in the 2002 July 23 Solar Flare

By Gordon D. Holman, L. Sui, Richard A. Schwartz. 2003

282 citations recorded by the source corpus.

Subfields: Artificial Intelligence, Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/cc8d2116794ad1dcce74ee6552b1c3afebe0b97d

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Citations in the corpus

The Relationship Between Solar Radio and Hard X-ray Emission (2011, background): “The structure of the 35 GHz light curve is representative of all radio frequencies above 4 GHz, and 60–100 keV is representative of the light curves for all hard X-rays above 30 keV; below 30 keV, the X-rays show less temporal fine structure in their light curves (Holman et al. 2003).”
Hard X-ray emission from the solar corona (2008, background): “We are not aware of any systematic RHESSI studies of the superhot sources as such, but the data contain interesting examples (e.g., Holman et al 2003).”
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.””
A UNIFIED COMPUTATIONAL MODEL FOR SOLAR AND STELLAR FLARES (2015, background): “Fortunately, the Ramaty High Energy Solar Spectroscopic Imager (RHESSI; Lin et al. 2002) observes this bremsstrahlung radiation from which it is possible to deduce the injected electron spectrum (e.g., Holman et al. 2003).”
Recent Advances in Understanding Particle Acceleration Processes in Solar Flares (2011, methodology): “Historically,a low-energy cutoffEc was assumed simply in order to keep the injected power ∫ ∞ Ec E0F0(E0)dE0 finite (e.g., Brown 1971; Holman et al. 2003).”
Radiative Hydrodynamic Models of the Optical and Ultraviolet Emission from Solar Flares (2005, methodology): “Recently, Holman et al. (2003) analyzed hard X-ray spectra observed with RHESSI to obtain the injected electron energy spectrum at 20 s intervals throughout the 23 July 2002 X-class solar flare.”
RHESSI Observations of Particle Acceleration and Energy Release in an Intense Solar Gamma-Ray Line Flare (2003, methodology): “The rate of energy deposition by the accelerated electrons peaks at∼1029 ergs s 1 above∼20 keV during the rise phase and drops to∼ ergs s 1 at the start of the impulsive282 # 10 phase, decreasing to below 1028 ergs s 1 by 0040 UT (Holman et al. 2003).”
Sixty-five years of solar radioastronomy: flares, coronal mass ejections and Sun–Earth connection (2008, background): “45a) allows to confirm the existence in the onset phase of a coronal non-thermal source inferred from HXR observations and which contains a large amount of energy (Lin et al. 2003; Holman et al. 2003; White et al. 2003).”
TIME-RESOLVED PROPERTIES AND GLOBAL TRENDS IN dMe FLARES FROM SIMULTANEOUS PHOTOMETRY AND SPECTRA (2013, methodology): “The accelerated electron distribution in the Allred et al. (2006) models employs a double power-law energy distribution of beam electrons with a minimum cutoff energy, Ec, which is assumed to be 37 keV (inferred from solar flare hard X-ray observations with RHESSI (Holman et al. 2003)).”
X-ray sources and magnetic reconnection in the X3.9 flare of 2003 November 3 (2006, background): “7 gave an acceptable reduced χ2 ∼ 1, though we note that the fits are not unique (for more detailed discussions on this kind of forward fitting technique applied to RHESSI spectra see Holman 2003; Holman et al. 2003; Sui et al. 2005).”
Deducing Electron Properties from Hard X-ray Observations (2011, methodology): “8), for example (Holman et al. 2003).”
Impulsive Phase Flare Energy Transport by Large-Scale Alfvén Waves and the Electron Acceleration Problem (2007, background): “…fraction of flare energy resides in these electrons (Kane & Donnelly 1971; Lin & Hudson 1976; Holman et al. 2003), and calculations under the assumptions of the thick-target model yield numbers on the order of 1034– 1037 electrons accelerated per second (e.g., Miller 1997; Holman et al. 2003).”
Observation of energetic electrons within magnetic islands (2008, background): “Studies of energy release during solar flares, in particular, indicate that up to 50p of the released energy is carried by accelerated 20–100 keV suprathermal electron”
An Observational Overview of Solar Flares (2011, methodology): “The standard collisional thick-target electron beam model requires electron fluxes up to a few×1035 electrons per second (Holman et al. 2003) leaving the corona.”