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MagPy (v2)

Model Description

Uses SDO/HMI vector magnetograms to measure free energy proxies for each AR on the solar disk.  The free energy proxies include the gradient of the magnetic field across the neutral line, the magnetic shear angle across the neutral line, and others.  These free energy proxies are used to relate to historically derived event rates, and with Poisson statistics, probabilities of the occurrence of >M-class flares, >X-class flare, CMEs, Fast CMEs, and SPEs within the next 24 hours. To determine the optimal function relating solar eruption event rate and total non-potentiality of active regions, extensive data mining process was performed during MagPy training sessions to thousands of magnetic field threshold configurations in order to compare skill scores across the validation results to determine the best set of magnetic field thresholds for operational use.

Model Figure(s) :

Model Inputs Description

HMI Line of sight (hmi.m_720s_nrt) 
HMI vector magnetograms (NRT CEA SHARP [hmi.sharp_cea_720s_nrt] and NRT CCD SHARP [hmi.sharp_720s_nrt])
NOAA SRS (solar region summery)

Model Outputs Description

Full disk flare probabilities, full disk SEP probability, CME probability, and fast CME probability 

Model Caveats

MagPy utilizes a 45-heliocenteric degree cone filter to discard magnetograms on the limbs of the solar disk. These magnetograms, distorted by effects like foreshortening, engender high degrees of error in free-energy proxy calculations and spawn false neutral-lines. As these types of magnetograms can severely skew the correlation between the free energy proxies and event-rates, they are left out of the training dataset. MagPy is most accurate within a 45 degree cone from disk center. 

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Curator: Chiu Wiegand | NASA Official: Dr. Masha Kuznetsova | Privacy and Security Notices | Accessibility | CCMC Data Collection Consent Agreement