2013
DOI: 10.1007/s11207-012-0211-6
|View full text |Cite
|
Sign up to set email alerts
|

Coronal Hole Influence on the Observed Structure of Interplanetary CMEs

Abstract: We report on the coronal hole (CH) influence on the 54 magnetic cloud (MC) and non-MC associated coronal mass ejections (CMEs) selected for studies during the Coordinated Data Analysis Workshops (CDAWs) focusing on the question if all CMEs are flux ropes. All selected CMEs originated from source regions located between longitudes 15E-15W. Xie, Gopalswamy, and St, Cyr (2013, Solar Phys., doi:10.1007/s11207-012-0209-0) found that these MC and non-MC associated CMEs are on average deflected towards and away from … Show more

Help me understand this report
View preprint versions

Search citation statements

Order By: Relevance

Paper Sections

Select...
1
1
1
1

Citation Types

3
43
0

Year Published

2013
2013
2017
2017

Publication Types

Select...
7
2

Relationship

3
6

Authors

Journals

citations
Cited by 56 publications
(46 citation statements)
references
References 32 publications
3
43
0
Order By: Relevance
“…However, there are many disk-center eruptions that are not observed as MCs. Propagation effects such as deflection in the corona (Xie, Gopalswamy and St. Cyr, 2013;Mäkelä et al, 2013) seem to be responsible for the non-cloud appearance of these events at 1 AU, even though there is no difference in the source properties of cloud and non-cloud ICMEs Yashiro et al, 2013). Therefore, it is possible to estimate the expected poloidal flux of the non-cloud ICMEs at 1 AU from the RC flux.…”
Section: Discussionmentioning
confidence: 99%
“…However, there are many disk-center eruptions that are not observed as MCs. Propagation effects such as deflection in the corona (Xie, Gopalswamy and St. Cyr, 2013;Mäkelä et al, 2013) seem to be responsible for the non-cloud appearance of these events at 1 AU, even though there is no difference in the source properties of cloud and non-cloud ICMEs Yashiro et al, 2013). Therefore, it is possible to estimate the expected poloidal flux of the non-cloud ICMEs at 1 AU from the RC flux.…”
Section: Discussionmentioning
confidence: 99%
“…CME interactions can also result in CME deflection and merger (Shen et al 2012). In the declining phase, low-latitude coronal holes appear frequently, so CME deflection by such coronal holes becomes important (Gopalswamy et al 2009d;Mohamed et al 2012;Mäkelä et al 2013). The deflections are thought to be caused by the magnetic pressure gradient between the eruption region and the coronal hole (Gopalswamy et al 2010d;Shen et al 2011;Gui et al 2011).…”
Section: Propagation Effects: Deflection Interaction and Rotation Omentioning
confidence: 99%
“…The empirical relationships established between HSS characteristics and the related geomagnetic activity provides an advance warning of impending CIR storms (Tsurutani et al 2006;Verbanac et al 2011). Coronal holes also deflect CME-driven shocks and CMEs that have important space weather consequences (Gopalswamy 2010(Gopalswamy , 2009dOlmedo et al 2012;Kay et al 2013;Mäkelä et al 2013). The deflection by coronal holes can be so large that CMEs originating from close the disk center of the Sun do not arrive at Earth while the shocks do.…”
Section: Coronal Holes and Cirsmentioning
confidence: 99%
“…This requires estimating the number of FRs expected from the observed number of CMEs. Recent studies conclude that a large fraction (Vourlidas et al, 2013) or even most of the CMEs Mäkelä et al, 2013) have a flux rope structure. The CMEs observed in-situ (ICMEs) without flux ropes would be cases crossed by the spacecraft close to the FR boundary, or even outside the FR (e.g.…”
Section: Are Mcs And/or Small Frs Related To Cmes?mentioning
confidence: 99%