The life of a CME and the development of a MIR: From the Sun to 58 AU

Details The life of a CME and the development of a MIR: From the Sun to 58 AU The life of a CME and the development of a MIR: From the Sun to 58 AU

Apr 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002jgra..107.1041r&link_type=abstract

Journal of Geophysical Research (Space Physics), Volume 107, Issue A4, pp. SSH 1-1, CiteID 1041, DOI 10.1029/2001JA000175

Physics

13

Interplanetary Physics: Ejecta, Driver Gases, And Magnetic Clouds, Interplanetary Physics: Solar Wind Plasma, Interplanetary Physics: Interplanetary Magnetic Fields

Scientific paper

Large coronal mass ejections (CMEs) have major effects on the structure of the solar wind in the heliosphere. The plasma and magnetic field can be compressed ahead of CMEs to form merged interaction regions (MIRs). One signature of some CMEs that can be used to track them through the heliosphere is an enhanced alpha abundance. We use this signature and a one-dimensional MHD model to track a CME from an active region on the Sun to Wind (1 AU), then to Ulysses (5.3 AU) and finally to Voyager 2 (58 AU). The arrival times of the CME ejecta at the three spacecraft are identified primarily by the increased alpha abundance. The observed plasma profiles and timing are close to those predicted by propagating data outward (from Earth to Ulysses and from Ulysses to Voyager 2) using the MHD model and give us confidence we are observing the same events at all three spacecraft. This event and a subsequent CME bracket a developing MIR and thus allow us to track the development of this structure.

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