On the Magnetic Flux Budget in Low-Corona Magnetic Reconnection and Interplanetary Coronal Mass Ejections

By J. Qiu, Qiang Hu, T. Howard, V. Yurchyshyn. 2007

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In Astronomy and Astrophysics

Citations in the corpus

CONNECTING SPEEDS, DIRECTIONS AND ARRIVAL TIMES OF 22 CORONAL MASS EJECTIONS FROM THE SUN TO 1 AU (2014, background): “This is thought to arise from the role played by magnetic reconnection during CME eruption, namely through a possible formation of their interior magnetic flux rope (e.g. Qiu & Yurchyshyn 2005; Qiu et al. 2007; Möstl et al. 2009c).”
Coronal Mass Ejections: Observations (2012, background): “Recent quantitative comparison between reconnected flux at the eruption site and the azimuthal flux in flux ropes in the solar wind suggest that the two fluxes are approximately the same (Qiu et al., 2007), implying that the flux ropes are formed during the eruption process rather than present in th”
Multispacecraft observation of magnetic cloud erosion by magnetic reconnection during propagation (2012, background): “Evaluation of MC magnetic flux budget is also very relevant to the study of coronal processes during eruption [Qiu et al., 2007].”
The Interaction of Successive Coronal Mass Ejections: A Review (2016, background): “…a typical CME carries about 1032 erg of energy (Vourlidas et al., 2000; Hudson, Bougeret, and Burkepile, 2006) and 1021 Mx of magnetic flux (Dasso et al., 2005; Qiu et al., 2007; Wang et al., 2015) into IP space, associated with reconfiguration of coronal magnetic fields in the CME source region.”
The standard flare model in three dimensions - III. Slip-running reconnection properties (2013, background): “They correspond to flare ribbons (Qiu et al. 2007), and join the coronal HFT by a cusp-shaped feature.”
History and development of coronal mass ejections as a key player in solar terrestrial relationship (2016, background): “From these observations, he inferred that the angular extent of the corpuscular stream ejected at the time of the beginning of the flare was ~90o (similar to a modern CME extent) and that the transit time of the stream to Earth to be ~25.5 h.”
Properties of Ground Level Enhancement Events and the Associated Solar Eruptions During Solar Cycle 23 (2012, background): “The reconnection process that results in the flare also produces the flux rope that moves out as the CME (Qiu et al. 2007).”
Photospheric flux cancellation and associated flux rope formation and eruption (2010, background): “The CME, observed by SOHO/LASCO, displayed a flux rope structure and propagated westward with a projected velocity of≈300 km s−1.”
The standard flare model in three dimensions II: upper limit on solar flare energy (2012, background): “Qiu et al. (2007) and Kazachenko et al. (2012) reported a ratio of 25% and 31% for the Oct 28 flare, respectively.”
The SOHO/LASCO CME Catalog (2009, background): “…between reconnected flux at the eruption site and the azimuthal flux in flux ropes in the solar wind suggest that the two fluxes are approximately the same (Qiu et al. 2007), implying that the flux ropes are formed during the eruption process rather than present in the pre-eruption state.”