Overexpanding coronal mass ejections at high heliographic latitudes
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Overexpanding coronal mass ejections at high heliographic latitudes observations and simulations

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Published by National Aeronautics and Space Administration, National Technical Information Service, distributor in [Washington, DC, Springfield, Va .
Written in English


  • Coronal mass ejection.,
  • Ulysses mission.,
  • Expansion.,
  • Simulation.,
  • Solar corona.,
  • Satellite observation.,
  • Solar wind.,
  • Radial distribution.,
  • Solar activity effects.

Book details:

Edition Notes

StatementJ.T. Gosling ... [et al.].
Series[NASA contractor report] -- NASA/CR-208188., NASA contractor report -- NASA CR-208188.
ContributionsGosling, J. T., United States. National Aeronautics and Space Administration.
The Physical Object
Pagination1 v.
ID Numbers
Open LibraryOL15546931M

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high heliographic latitudes [Gosling et al., c]. These events are caused by the overexpansion of CMEs that have speeds comparable to that of the surrounding solar wind plasma. Of six certain CMEs observed poleward of S31 ø during Ulysses' initial transit to high southern latitudes, three had associated shock pairs of this by: Ulysses observations reveal that most coronal mass ejections (CMES) observed in the solar wind far from the Sun at high heliographic latitudes have large radial widths and are still expanding as. Get this from a library! Overexpanding coronal mass ejections at high heliographic latitudes: observations and simulations. [J T Gosling; United States. .   Nine coronal mass ejections (CMEs) have been detected in the solar wind by the Ulysses plasma experiment between 31° and 61° South. One of these events, which was also a magnetic cloud, was directly associated with an event observed by the soft X-ray telescope on Yohkoh in which large magnetic loops formed in the solar corona directly beneath by:

@article{osti_, title = {Coronal mass ejections in the solar wind at high solar latitudes: An overview}, author = {Gosling, J T}, abstractNote = {Ulysses has provided the first direct measurements of coronal mass ejections, CMES, in the solar wind at high heliographic latitudes. This paper provides an overview of new and unexpected results from the plasma experiment on Ulysses, supplemented . Coronal mass ejections and space weather. D. F. Webb1 and N. Gopalswamy2. 1 Institute for Scientific Research, Boston College, Commonwealth Ave., Chestnut Hill, MA USA. 2. NASA Goddard Space Flight Center, Code , Greenbelt, MD , USA. Abstract. Coronal mass ejections (CMEs) are a key feature of coronal and interplanetary File Size: KB.   Coronal mass ejections (CMEs) are large, episodic eruptions of coronal plasma and magnetic flux that are ejected out into the heliosphere at speeds typically 1 ranging from – km s .   A coronal mass ejection (CME) event showing a representation of the flux rope anchored at the sun and the propagation of the magnetic flux rope through space toward Earth.

  How does a Coronal Mass Ejection relate to Solar flares and Sunspots. Looking at how the changing magnetism within the Sun causes these events and what their impact on . The mass emission from the Sun in the form of solar wind defines the heliosphere. The heliospheric plasma originates from the hot corona of the Sun, whether it is the solar wind or the coronal mass ejections (CMEs). While the solar wind speed roughly varies by a factor of 2 depending upon the source region (coronal hole or. What is a coronal mass ejection or CME? The book introduces the solar coronal mass ejection phenomena. This includes both those observed in the corona and those further from the Sun, known as interplanetary coronal mass ejections. We discuss the history and physics behind these phenomena, theories describing their launch and evolution, association with other solar eruptive phenomena Cited by: