Predicting Flares D. Shaun Bloomfield Astrophysics Research Group Trinity College Dublin Flare Group E, Solar24 9th December 2008 D. Shaun Bloomfield Trinity.

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Presentation transcript:

Predicting Flares D. Shaun Bloomfield Astrophysics Research Group Trinity College Dublin Flare Group E, Solar24 9th December 2008 D. Shaun Bloomfield Trinity College Dublin

When do large flares happen? Flare Group E, Solar24 9th December 2008 D. Shaun Bloomfield Trinity College Dublin

Flare Frequencies oFlare frequency-energy distribution power law holds over multiple decades (Aschwanden 2000) oCan determine flare rates from numbers of events measured oIndividual active regions (ARs) have power law indices close to whole Sun value (Wheatland 2000) Flare Group E, Solar24 9th December 2008 D. Shaun Bloomfield Trinity College Dublin

Flare Timings and Probabilities oFlare frequency-waiting times show Poisson-like exponential distribution (Moon et al. 2001) oCan determine probability of one or more flares above a given energy cut-off (Gallagher et al. 2002) ε = 1 – exp( -λΔT ) oUsed with mean flare rates for each McIntosh class ono variation within class Flare Group E, Solar24 9th December 2008 D. Shaun Bloomfield Trinity College Dublin

Bayesian Probabilities prob(λ|D, I AR ) = prob(D|λ, I AR ) * prob(λ|I AR ) / prob(D|I AR ) (1) (2) (3) (4) (1) – probability distribution of flare rate given flare data and AR info. (2) – probability distribution of flare data given flare rate and AR info. (3) – probability distribution of flare rate given AR info. (4) – probability distribution of flare data given AR info. (normalisation term) oCan construct prob(D|λ, I AR ) by combining the phenomenological eqns. (Wheatland 2004) oCan convert probability distribution of flare rates (1) into the probability distribution of flare probabilities from the previous relation for Poisson- based flare probabilities λ = ln( 1 – ε ) / ΔT Flare Group E, Solar24 9th December 2008 D. Shaun Bloomfield Trinity College Dublin

Conditions for Flaring oPeak flare magnitude vs peak spot area (Sammis et al. 2000) oBig, bad, and ugly? Flare Group E, Solar24 9th December 2008 D. Shaun Bloomfield Trinity College Dublin

Data for Analysis oGOES X-ray flare event listings oflare times, flare magnitudes, associated AR oSolar EUV images oflare locations and AR association (backward extension of Sam Freeland’s SoHO/EIT flare location archive beyond 2002) oFrom mid-2009, PROBA2/SWAP 171Å images at nominal 1-min cadence oNOAA SWPC AR summaries onumber of spots, total spot area, longitudinal extent, location, McIntosh and Mt Wilson magnetic classifications oSoHO/MDI AR magnetograms opeak and average |B|, length and curvature of neutral line, peak and average dB/dl along neutral line, fractal dimension Flare Group E, Solar24 9th December 2008 D. Shaun Bloomfield Trinity College Dublin

Final Data Product oAutomated code updating with additional X-ray events and AR evolution oAR-specific flare probabilities hosted on oComparison with NOAA SWPC and Poisson-based predictions Flare Group E, Solar24 9th December 2008 D. Shaun Bloomfield Trinity College Dublin