The origin and development of the May 1997 magnetic cloud

By D. Webb, R. Lepping, L. Burlaga, C. Deforest, D. Larson, S. Martin, S. Plunkett, D. Rust. 2000

178 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/b5161cc2c5a3700a6d7125830c4d8672ce73551b

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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): “In the past, very few studies (mostly case studies) have been made comparing the relevant physical parameters of MCs with their solar progenitors (Lepping et al. 1997; Webb et al. 2000; Mandrini et al. 2005; Attrill et al. 2006).”
The Role of Magnetic Reconnection in the Observable Features of Solar Eruptions (2004, methodology): “The in situ measurements give the toroidal field inside the magnetic cloud, H0, from 15 to 30 nT (or from 1:5 10 4 to 3:0 10 4 G), and r0 varies from 0.1 to 0.4 AU (Lepping et al. 1990, 1997; Webb et al. 2000).”
Coronal “Wave”: Magnetic Footprint of a Coronal Mass Ejection? (2007, unknown): “There appear to be two types: deep core dimmings, sometimes shown to correspond to the footpoints of the erupted flux rope (e.g., Webb et al. 2000), and a more widespread dimming, observed to correspond well to the spatial extent of CMEs detected in coronagraph data (Thompson et al. 2000a).”
Numerical simulation of the 12 May 1997 interplanetary CME event (2004, background): “The simulated CME propagates on and slightly ahead of the moderate fast stream that results from the excursion of the southern coronal hole toward the helio-equator (Figure 3). The initially fast ICME propagates into the dense slow streamer belt (Figure 4). Faster flow from behind and dense slow pla”
A summary of WIND magnetic clouds for years 1995-2003: model-fitted parameters, associated errors and classifications (2006, background): “Webb et al. (2001) discuss the solar sources of both kinds of major geoeffective solar wind structures, i.”
On the nature of EIT waves, EUV dimmings and their link to CMEs (2004, background): “Sometimes dimmings (and TCHs in particular) appear in pairs, suggesting that such a double (twin) dimming represents the footpoints of an ejected interplanetary flux rope (Webb et al. 2000).”
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).”
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).”
The association of coronal mass ejections with their effects near the Earth (2005, background): “Further studies (e.g. Webb et al., 2000; Cane et al., 2000; Gopalswamy et al., 2001c; Vršnak and Gopalswamy, 2002; Michalek et al., 2002; González- Esparza et al., 2003a,b; Yurchyshyn et al., 2003) tried to improve the prediction accuracy, but they all keep suffering from the problem of deducing…”