Temporal aspects and frequency distributions of solar soft X-ray flares

By Astrid Veronig, M. Temmer, A. Hanslmeier, W. Otruba, M. Messerotti. 2002

214 citations recorded by the source corpus.

A statistical analysis of almost 50 000 soft X-ray (SXR) flares observed by GOES during the period 1976–2000 is presented. On the basis of this extensive data set, statistics on temporal properties of soft X-ray flares, such as duration, rise and decay times with regard to the SXR flare classes is presented. Correlations among distinct flare parameters, i.e. SXR peak flux, fluence and characteristic times, and frequency distributions of flare occurrence as function of the peak flux, the fluence and the duration are derived. We discuss the results of the analysis with respect to statistical flare models, the idea of coronal heating by nanoflares, and elaborate on implications of the obtained results on the Neupert effect in solar flares.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/2a7bc9f0f7396d00d0001f72289220d501b8f884

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In Astronomy and Astrophysics

1. M. Temmer
2. Nat Gopalswamy
3. H. Hudson
4. B. Vršnak
5. S. Yashiro
6. I. Usoskin
7. C. Schrijver
8. R. Howard

Citations in the corpus

• 25 Years of Self-Organized Criticality: Solar and Astrophysics (2014, background): “…with the OSO-3 spacecraft (Hudson et al. 1969), the Explorer (Drake 1971), Yohkoh/SXT (Shimizu 1995; Shimojo and Shibata 1999), the SMM/BCS (Lee et al. 1999), and the GOES spacecraft (Lee et al. 995; Feldman et al. 1997; Veronig et al. 2002a,b; Yashiro et al. 2006; Aschwanden and Freeland 2012).”
• Different Power-Law Indices in the Frequency Distributions of Flares with and without Coronal Mass Ejections (2006, background): “Veronig et al. (2002) examined almost 50,000 X-ray flares recorded during 1976 to 2000 and obtained α = 2.11 ± 0.13 for the peak flux, α = 2.03 ± 0.09 for the fluence, and α = 2.93 ± 0.12 for the duration.”
• RHESSI Microflare Statistics. I. Flare-Finding and Frequency Distributions (2008, methodology): “At similar energies, Veronig et al. (2002) analyzed GOES flares and found an average of 18.2 minutes.”
• Statistical properties of superflares on solar-type stars based on 1-min cadence data (2015, background): “The power-law slope for the correlation between the duration of solar flares and X-ray fluence observed with the GOES is about 1/3 (Veronig et al. 2002).”
• Estimating the frequency of extremely energetic solar events, based on solar, stellar, lunar, and terrestrial records (2012, background): “…from the impulsive (fast-rise) to the decay phase, the spectral irradiance typically follows the so-called Neupert effect [Neupert , 1968; Veronig et al., 2002b]: lower-energy emissions (e.g., soft X-rays) behave, to first order, as the time integral of high-energy emissions such as hard…”
• Magnetic Reconnection in Astrophysical and (2009, background): “The distribution of flare energy emission rates follows a power-law over several decades (Dennis 1985, Nita et al. 2002, Veronig et al. 2002, Su et al. 2006).”
• The 1859 space weather event revisited: limits of extreme activity (2013, background): “Figure 5 in Veronig et al. (2002), which relates flare SXR fluence to SXR intensity (or classification), and Figure 3 indicate that a flare with bolometric energy of 10 33 erg (~6 x 10 33 erg) flare will correspond to a class ~X85 (~700) SXR flare.”
• Investigation of the Neupert effect in solar flares. I. Statistical properties and the evaporation model (2002, methodology): “On the basis of flare frequency distributions, Lee et al. (1993, 1995) and Veronig et al. (2002a) found inconsistencies with the linearly formulated Neupert effect as given in Eq.”
• RHESSI Microflare Statistics. II. X-Ray Imaging, Spectroscopy, and Energy Distributions (2007, background): “1 (Drake 1971; Lee et al. 1995; Feldman et al. 1997; Veronig et al. 2002).”
• Implications of X-ray Observations for Electron Acceleration and Propagation in Solar Flares (2011, methodology): “A high correlation and time coincidence between the soft X-ray peak and hard X-ray end time was generally found, but a significant fraction of events also had a different timing (Veronig et al. 2002c).”