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Interplanetary Propagation of Coronal Mass EjectionsAlthough more than ten thousand coronal mass ejections (CMEs) are produced during each solar cycle at the Sun, only a small fraction hits the Earth. Only a small fraction of the Earth-directed CMEs ultimately arrive at Earth depending on their interaction with the solar wind and other large-scale structures such as coronal holes and CMEs. The interplanetary propagation is essentially controlled by the drag force because the propelling force and the solar gravity are significant only near the Sun. Combined remote-sensing and in situ observations have helped us estimate the influence of the solar wind on the propagation of CMEs. However, these measurements have severe limitations because the remote-sensed and in-situ observations correspond to different portions of the CME. Attempts to overcome this problem are made in two ways: the first is to model the CME and get the space speed of the CME, which can be compared with the in situ speed. The second method is to use stereoscopic observation so that the remote-sensed and in-situ observations make measurements on the Earth-arriving part of CMEs. The Solar Terrestrial Relations Observatory (STEREO) mission observed several such CMEs, which helped understand the interplanetary evolution of these CMEs and to test earlier model results. This paper discusses some of these issues and updates the CME/shock travel time estimates for a number of CMEs.
Document ID
20110011249
Acquisition Source
Goddard Space Flight Center
Document Type
Abstract
Authors
Gopalswamy, Nat
(NASA Goddard Space Flight Center Greenbelt, MD, United States)
Date Acquired
August 25, 2013
Publication Date
May 9, 2011
Subject Category
Solar Physics
Meeting Information
Meeting: 2011 CSSE International Symposium: From Solar Storm ot Geomagnetic Storm
Location: Shanghai
Country: China
Start Date: May 9, 2011
End Date: May 12, 2011
Sponsors: Peking Univ.
Distribution Limits
Public
Copyright
Work of the US Gov. Public Use Permitted.
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