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HMI Data Driven Magnetohydrodynamic Model Predicted Active Region Photospheric Heating Rates: Their Scale Invariant, Flare Like Power Law Distributions, and Their Possible Association With Flares
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Author and Affiliation:
Goodman, Michael L.(Jacobs Engineering and Science Services and Skills Augmentation Group (ESSSA), Huntsville, AL, United States);
Kwan, Chiman(Applied Research, LLC, Rockville, MD, United States);
Ayhan, Bulent(Applied Research, LLC, Rockville, MD, United States);
Shang, Eric L.(Applied Research, LLC, Rockville, MD, United States)
Abstract: A data driven, near photospheric, 3 D, non-force free magnetohydrodynamic model pre- dicts time series of the complete current density, and the resistive heating rate Q at the photosphere in neutral line regions (NLRs) of 14 active regions (ARs). The model is driven by time series of the magnetic field B observed by the Helioseismic & Magnetic Imager on the Solar Dynamics Observatory (SDO) satellite. Spurious Doppler periods due to SDO orbital motion are filtered out of the time series for B in every AR pixel. Errors in B due to these periods can be significant. The number of occurrences N(q) of values of Q > or = q for each AR time series is found to be a scale invariant power law distribution, N(Q) / Q-s, above an AR dependent threshold value of Q, where 0.3952 < or = s < or = 0.5298 with mean and standard deviation of 0.4678 and 0.0454, indicating little variation between ARs. Observations show that the number of occurrences N(E) of coronal flares with a total energy released > or = E obeys the same type of distribution, N(E) / E-S, above an AR dependent threshold value of E, with 0.38 < or approx. S < or approx. 0.60, also with little variation among ARs. Within error margins the ranges of s and S are nearly identical. This strong similarity between N(Q) and N(E) suggests a fundamental connection between the process that drives coronal flares and the process that drives photospheric NLR heating rates in ARs. In addition, results suggest it is plausible that spikes in Q, several orders of magnitude above background values, are correlated with times of the subsequent occurrence of M or X flares.
Publication Date: May 15, 2017
Document ID:
20170005369
(Acquired Jun 16, 2017)
Subject Category: SOLAR PHYSICS; STATISTICS AND PROBABILITY
Report/Patent Number: M17-5865
Document Type: Conference Paper
Publication Information: (SEE 20170005342)
Meeting Information: Applied Space Environments Conference 2017; 15-19 May 2017; Huntsville, AL; United States
Meeting Sponsor: Universities Space Research Association; Huntsville, AL, United States
NASA; Washington, DC, United States
Contract/Grant/Task Num: NNM12AA41C
Financial Sponsor: NASA Marshall Space Flight Center; Huntsville, AL, United States
Organization Source: NASA Marshall Space Flight Center; Huntsville, AL, United States
Description: 1p; In English
Distribution Limits: Unclassified; Publicly available; Unlimited
Rights: Copyright; Distribution under U.S. Government purpose rights; under NASA contract NNM12AA41C
NASA Terms: MAGNETOHYDRODYNAMICS; PHOTOSPHERE; SOLAR FLARES; MAGNETIC FIELDS; HELIOSEISMOLOGY; CURRENT DENSITY; TIME SERIES ANALYSIS; SOLAR X-RAYS; ERRORS; SOLAR OBSERVATORIES
Availability Notes: Abstract Only
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