Interplanetary flux rope ejected from an X-ray bright point. The smallest magnetic cloud source-region ever observed

By C. Mandrini, S. Pohjolainen, S. Dasso, L. Green, P. Démoulin, L. Driel-Gesztelyi, C. Copperwheat, C. Foley. 2005

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In Astronomy and Astrophysics

Citations in the corpus

On the Magnetic Flux Budget in Low-Corona Magnetic Reconnection and Interplanetary Coronal Mass Ejections (2007, background): “…typically magnetic flux and helicity, and the solar progenitors, such as magnetic flux in filaments (Lepping et al. 1997), coronal dimming flux (Webb et al. 2000; Mandrini et al. 2005; Attrill et al. 2006), and the total magnetic flux and helicity in source active regions (Leamon et al. 2004).”
Photospheric flux cancellation and associated flux rope formation and eruption (2010, methodology): “Previously, dimming signatures of eruptions have been used to investigate the flux content of the erupting flux rope and make a link with in situ observations of flux ropes at 1AU (e.g. Webb et al. 2000; Mandrini et al. 2005; Attrill et al. 2006; Jian et al. 2006).”
NUMERICAL SIMULATION OF AN EUV CORONAL WAVE BASED ON THE 2009 FEBRUARY 13 CME EVENT OBSERVED BY STEREO (2009, background): “…core coronal dimming regions (i.e. black regions, bottom panels of Figure 1), located on either side of the bright post-eruptive arcade (PEA) mark the footpoints of the erupting flux rope (e.g. Webb et al. 2000; Mandrini et al. 2005; Crooker & Webb 2006; Attrill et al. 2006; McIntosh et al. 2007).”
The Calm before the Storm: The Link between Quiescent Cavities and Coronal Mass Ejections (2006, background): “…(Tanaka 1991; Leka et al. 1996; Lites et al. 1995), apparent shear/rotational motions at the photosphere (Lopez Fuentes 2000; Green et al. 2002; Mandrini et al. 2005; Gibson et al. 2004), observed properties of coronal prominences (Priest et al. 1989; Rust 1994; Rust & Kumar 1994; Lites & Low…”
The magnetic field in the solar atmosphere (2014, background): “The majority of ejecta, including CMEs associated with disappearing filaments (Yurchyshyn et al., 2001; Cho et al., 2013) or eruptive X-ray loops (Mandrini et al., 2005; Zheng et al., 2011), propagate away from the Sun in the form of magnetic clouds (MCs) and hence actively carry helicity away.”
A Comparative Study between Eruptive X-Class Flares Associated with Coronal Mass Ejections and Confined X-Class Flares (2007, background): “On the other hand, Mandrini et al. (2005) reported the smallest CME event ever observed by 2005, in which the CME originated from the smallest source region, a tiny dipole, and developed into the smallest magnetic cloud.”