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CME Propagation CSI 769 / ASTR 769 Lect. 11, April 10 Spring 2008.

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Presentation on theme: "CME Propagation CSI 769 / ASTR 769 Lect. 11, April 10 Spring 2008."— Presentation transcript:

1 CME Propagation CSI 769 / ASTR 769 Lect. 11, April 10 Spring 2008

2 CME Flux Rope Model Lepping, R.P., Jones, J.A., Burlaga. “Magnetic Field Structure of Interplanetary Magnetic Clouds at 1 AU” JGR, Vol. 95, No. A8, 11957-11965, 1990

3 CME MSOE Model Siscoe, G.L., Crooker, N.U., Elliott, H.A., “Initial-Condition Influences on CME Expansion and Propagation” Solar Physics, Vol. 239, 293-316, DOI: 10.1007/s11207-006- 0302-3, 2006 MSOE: Melon-Seed-Overpressure-Expansion Model

4 Interplanetary CME (ICME) CME propagates into the interplanetary space, plowing through the ambient solar wind The magnetic structure of ICME at 1 AU is similar to that in its solar origin, which is highly helical (called flux rope) At 1 AU, it is called magnetic cloud highly organized magnetic field is observed, e.g., smooth rotation Large scale, crossing the Earth for ~ 24 hours Magnetic Cloud

5 ICME Identification Dst B/Bz Vel Np Tp Texp β Sun 2004/07/27 storm (-182 nT) Shock Front: discontinuity ICME (ejecta): B enhance Bz rotation Low Plasma β Low Tp High Q Fe ----- SH (Shock Sheath) Solar Sources

6 Fast and Slow Wind Solar Wind: Bimodal Fast wind originates from coronal hole, Slow wind originates from regions close to streamer belts or heliospheric current sheet SW heliographic latitudinal Distribution (Ulysses observation)

7 Corotating Interaction Region (CIR) When a low latitude coronal hole appears (across the heliographic equator), fast wind exists in the ecliptic plane.

8 Corotating Interaction Region (CIR) The jetline of fast wind is less curved than that of slow wind Fast streams “catching up” with slow streams, compressing the preceding stream and produce a high pressure region. The interaction region is at the leading edge of the fast stream Since low-latitude coronal holes can live over several solar rotations, this structure can recur several times This is commonly called “corotating interaction region” or CIR A pair of forward and reverse shocks forms

9 CIR Corotating Interaction Region: Caused by the interaction of fast SW originated from coronal hole with preceding slow SW CIR/SI

10 IMF

11 The End

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