Latitudinal structure of a Coronal Mass Ejection inferred from ULYSSES and GEOTAIL observations

Details Latitudinal structure of a Coronal Mass Ejection inferred from ULYSSES and GEOTAIL observations Latitudinal structure of a Coronal Mass Ejection inferred from ULYSSES and GEOTAIL observations

May 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995georl..22.1169h&link_type=abstract

Geophysical Research Letters (ISSN 0094-8276), vol. 22, no. 10, p. 1169-1172

Physics

13

Latitude, Propagation Velocity, Solar Corona, Solar Wind Velocity, Stellar Mass Ejection, Data Correlation, Magnetic Flux, Proton Energy, Proton Flux Density, Ulysses Mission

Scientific paper

We present the first observations of a Coronal Mass Ejection (CME) by two spacecraft separated substantially in heliographic latitude. Ulysses and Geotail both see similar features in the plasma and magnetic field parameters during an interval in which Geotail is located in the deep magnetosheath (greater than 150 Earth radii) and Ulysses is located in the solar wind at 5 AU, approximately 20 S of Geotail, and approximately 51 W (in the direction of solar rotation) of Geotail. Based on the similarity in plasma and magnetic field parameters and similar inferred ejection times from the Sun for both features we argue that the same CME is observed by both spacecraft. The portion of the CME observed by Ulysses is traveling much faster than the portion observed by Geotail. Thus the CME has significant latitudinal structure since at any given time the high latitude portion of the CME extends much further out in radial distance. Furthermore, this implies that a simple calculation of the arrival time of a CME at the Earth may not be done if the observing spacecraft is located substantially away from the ecliptic plane.

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