Sign on
ADS Classic will be deprecated in May 2019 and retired in October 2019. Please redirect your searches to the new ADS modern form or the classic form. More info can be found on our blog.

SAO/NASA ADS Astronomy Abstract Service


· Find Similar Abstracts (with default settings below)
· Electronic Refereed Journal Article (HTML)
· arXiv e-print (arXiv:1301.2176)
· References in the article
· Citations to the Article (30) (Citation History)
· Refereed Citations to the Article
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Coronal Hole Influence on the Observed Structure of Interplanetary CMEs
Authors:
Mäkelä, P.; Gopalswamy, N.; Xie, H.; Mohamed, A. A.; Akiyama, S.; Yashiro, S.
Affiliation:
AA(The Catholic University of America, Washington, DC, USA; NASA Goddard Space Flight Center, Greenbelt, USA), AB(NASA Goddard Space Flight Center, Greenbelt, USA), AC(The Catholic University of America, Washington, DC, USA; NASA Goddard Space Flight Center, Greenbelt, USA), AD(The Catholic University of America, Washington, DC, USA; NASA Goddard Space Flight Center, Greenbelt, USA), AE(The Catholic University of America, Washington, DC, USA; NASA Goddard Space Flight Center, Greenbelt, USA), AF(The Catholic University of America, Washington, DC, USA; NASA Goddard Space Flight Center, Greenbelt, USA)
Publication:
Solar Physics, Volume 284, Issue 1, pp.59-75 (SoPh Homepage)
Publication Date:
05/2013
Origin:
SPRINGER
Keywords:
Sun, Coronal holes, Coronal mass ejections, Magnetic clouds, Ejecta
Abstract Copyright:
(c) 2013: Springer Science+Business Media Dordrecht
DOI:
10.1007/s11207-012-0211-6
Bibliographic Code:
2013SoPh..284...59M

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 the Sun-Earth line, respectively. We used a CH influence parameter (CHIP) that depends on the CH area, average magnetic field strength, and distance from the CME source region to describe the influence of all on-disk CHs on the erupting CME. We found that for CHIP values larger than 2.6 G the MC and non-MC events separate into two distinct groups where MCs (non-MCs) are deflected towards (away) from the disk center. Division into two groups was also observed when the distance to the nearest CH was less than 3.2×105 km. At CHIP values less than 2.6 G or at distances of the nearest CH larger than 3.2×105 km the deflection distributions of the MC and non-MCs started to overlap, indicating diminishing CH influence. These results give support to the idea that all CMEs are flux ropes, but those observed to be non-MCs at 1 AU could be deflected away from the Sun-Earth line by nearby CHs, making their flux rope structure unobservable at 1 AU.
Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)


Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints