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dc.contributor.authorZhu, Chunming
dc.contributor.authorQui, Jiong
dc.contributor.authorLiewer, Paulett
dc.contributor.authorVourlidas, Angelos
dc.date.accessioned2021-09-16T19:49:43Z
dc.date.available2021-09-16T19:49:43Z
dc.date.issued2020-04
dc.identifier.citationZhu, Chunming, Jiong Qiu, Paulett Liewer, Angelos Vourlidas, Michael Spiegel, and Qiang Hu. “How Does Magnetic Reconnection Drive the Early-Stage Evolution of Coronal Mass Ejections?” The Astrophysical Journal 893, no. 2 (April 24, 2020): 141. doi:10.3847/1538-4357/ab838a.en_US
dc.identifier.issn1538-4357
dc.identifier.urihttps://scholarworks.montana.edu/xmlui/handle/1/16446
dc.description.abstractTheoretically, coronal mass ejection (CME) kinematics are related to magnetic reconnection processes in the solar corona. However, the current quantitative understanding of this relationship is based on the analysis of only a handful of events. Here we report a statistical study of 60 CME-flare events from 2010 August to 2013 December. We investigate kinematic properties of CMEs and magnetic reconnection in the low corona during the early phase of the eruptions, by combining limb observations from STEREO with simultaneous on-disk views from SDO. For a subset of 42 events with reconnection rate evaluated by the magnetic fluxes swept by the flare ribbons on the solar disk observed from SDO, we find a strong correlation between the peak CME acceleration and the peak reconnection rate. Also, the maximum velocities of relatively fast CMEs (≳600 km s−1) are positively correlated with the reconnection flux, but no such correlation is found for slow CMEs. A time-lagged correlation analysis suggests that the distribution of the time lag of CME acceleration relative to reconnection rate exhibits three peaks, approximately 10 minutes apart, and on average, acceleration-led events have smaller reconnection rates. We further compare the CME total mechanical energy with the estimated energy in the current sheet. The comparison suggests that, for small-flare events, reconnection in the current sheet alone is insufficient to fuel CMEs. Results from this study suggest that flare reconnection may dominate the acceleration of fast CMEs, but for events of slow CMEs and weak reconnection, other mechanisms may be more important.en_US
dc.language.isoen_USen_US
dc.titleHow Does Magnetic Reconnection Drive the Early-stage Evolution of Coronal Mass Ejections?en_US
dc.typeArticleen_US
mus.citation.extentfirstpage141en_US
mus.citation.issue2en_US
mus.citation.journaltitleThe Astrophysical Journalen_US
mus.citation.volume893en_US
mus.identifier.doi10.3847/1538-4357/ab838aen_US
mus.relation.collegeCollege of Letters & Scienceen_US
mus.relation.departmentPhysics.en_US
mus.relation.universityMontana State University - Bozemanen_US
mus.data.thumbpage21en_US


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