000002912 001__ 2912
000002912 005__ 20160825074927.0
000002912 0247_ $$2DOI$$a10.1051/0004-6361/201628130
000002912 037__ $$aSCART-2016-0012
000002912 100__ $$aRyan, Daniel
000002912 245__ $$aEffects of flare definitions on the statistics of derived flare distributions
000002912 260__ $$c2016
000002912 520__ $$aThe statistical examination of solar flares is crucial to revealing their global characteristics and behaviour. Such examinations can tackle large-scale science questions or give context to detailed single-event studies. However, they are often performed using standard but basic flare detection algorithms relying on arbitrary thresholds. This arbitrariness may lead to important scientific conclusions being drawn from results caused by subjective choices in algorithms rather than the true nature of the Sun. In this paper, we explore the effect of the arbitrary thresholds used in the Geostationary Operational Environmental Satellite (GOES) event list and Large Yield RAdiometer (LYRA) Flare Finder algorithms. We find that there is a small but significant relationship between the power law exponent of the GOES flare peak flux frequency distribution and the flare start thresholds of the algorithms. We also find that the power law exponents of these distributions are not stable, but appear to steepen with increasing peak flux. This implies that the observed flare size distribution may not be a power law at all. We show that depending on the true value of the exponent of the flare size distribution, this deviation from a power law may be due to flares missed by the flare detection algorithms. However, it is not possible determine the true exponent from GOES/XRS observations. Additionally we find that the PROBA2/LYRA flare size distributions are artificially steep and clearly non-power law. We show that this is consistent with an insufficient degradation correction. This means that PROBA2/LYRA should not be used for flare statistics or energetics unless degradation is adequately accounted for. However, it can be used to study variations over shorter timescales and for space weather monitoring. 
000002912 536__ $$aSTCE; IAP P7/$$c08 CHARM; PRODEX/$$f4000103240; FP7/284461/eHEROES; STATICA/08/IN.1/I1879
000002912 594__ $$aSTCE
000002912 700__ $$aDominique, Marie
000002912 700__ $$aSeaton, Daniel
000002912 700__ $$aStegen, Koen
000002912 700__ $$aWhite, Arthur
000002912 773__ $$nA133$$pAstronomy & Astrophysics$$v592$$y2016
000002912 8560_ $$fmarie.dominique@observatoire.be
000002912 85642 $$ahttp://adsabs.harvard.edu/abs/2016A%26A...592A.133R
000002912 85642 $$ahttp://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2016A%26A...592A.133R&link_type=PREPRINT&db_key=AST
000002912 8564_ $$s855556$$uhttp://publi2-as.oma.be/record/2912/files/1606.04472v1.pdf
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000002912 905__ $$apublished in
000002912 980__ $$aREFERD