Which Photospheric Characteristics are Most Relevant to Active-Region Coronal Mass Ejections?. (arXiv:1909.06088v1 [astro-ph.SR])

Which Photospheric Characteristics are Most Relevant to Active-Region Coronal Mass Ejections?. (arXiv:1909.06088v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Kontogiannis_I/0/1/0/all/0/1">Ioannis Kontogiannis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Georgoulis_M/0/1/0/all/0/1">Manolis K. Georgoulis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Guerra_J/0/1/0/all/0/1">Jordan A. Guerra</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Park_S/0/1/0/all/0/1">Sung-Hong Park</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bloomfield_D/0/1/0/all/0/1">D. Shaun Bloomfield</a>

We investigate the relation between characteristics of coronal mass ejections
and parameterizations of the eruptive capability of solar active regions widely
used in solar flare prediction schemes. These parameters, some of which are
explored for the first time, are properties related to topological features,
namely, magnetic polarity inversion lines (MPILs) that indicate large amounts
of stored non-potential (i.e. free) magnetic energy. We utilize the Space
Weather Database of Notifications, Knowledge, Information (DONKI) and the Large
Angle and Spectrometric Coronograph (LASCO) databases to find flare-associated
coronal mass ejections and their kinematic characteristics while properties of
MPILs are extracted from Helioseismic and Magnetic Imager (HMI) vector
magnetic-field observations of active regions to extract the properties of
source-region MPILs. The correlation between all properties and the
characteristics of CMEs ranges from moderate to very strong. More significant
correlations hold particularly for fast CMEs, which are most important in terms
of adverse space-weather manifestations. Non-neutralized currents and the
length of the main MPIL exhibit significantly stronger correlations than the
rest of the properties. This finding supports a causal relationship between
coronal mass ejections and non-neutralized electric currents in highly sheared,
conspicuous MPILs. In addition, non-neutralized currents and MPIL length carry
distinct, independent information as to the eruptive potential of active
regions. The combined total amount of non-neutralized electric currents and the
length of the main polarity inversion line, therefore, reflect more efficiently
than other parameters the eruptive capacity of solar active regions and the CME
kinematic characteristics stemming from these regions.

We investigate the relation between characteristics of coronal mass ejections
and parameterizations of the eruptive capability of solar active regions widely
used in solar flare prediction schemes. These parameters, some of which are
explored for the first time, are properties related to topological features,
namely, magnetic polarity inversion lines (MPILs) that indicate large amounts
of stored non-potential (i.e. free) magnetic energy. We utilize the Space
Weather Database of Notifications, Knowledge, Information (DONKI) and the Large
Angle and Spectrometric Coronograph (LASCO) databases to find flare-associated
coronal mass ejections and their kinematic characteristics while properties of
MPILs are extracted from Helioseismic and Magnetic Imager (HMI) vector
magnetic-field observations of active regions to extract the properties of
source-region MPILs. The correlation between all properties and the
characteristics of CMEs ranges from moderate to very strong. More significant
correlations hold particularly for fast CMEs, which are most important in terms
of adverse space-weather manifestations. Non-neutralized currents and the
length of the main MPIL exhibit significantly stronger correlations than the
rest of the properties. This finding supports a causal relationship between
coronal mass ejections and non-neutralized electric currents in highly sheared,
conspicuous MPILs. In addition, non-neutralized currents and MPIL length carry
distinct, independent information as to the eruptive potential of active
regions. The combined total amount of non-neutralized electric currents and the
length of the main polarity inversion line, therefore, reflect more efficiently
than other parameters the eruptive capacity of solar active regions and the CME
kinematic characteristics stemming from these regions.

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