Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh42a..03l&link_type=abstract
American Geophysical Union, Fall Meeting 2011, abstract #SH42A-03
Astronomy and Astrophysics
Astrophysics
[2111] Interplanetary Physics / Ejecta, Driver Gases, And Magnetic Clouds, [2134] Interplanetary Physics / Interplanetary Magnetic Fields, [7513] Solar Physics, Astrophysics, And Astronomy / Coronal Mass Ejections
Scientific paper
A CME flux rope is a magnetic structure propelled from the Sun during a solar eruption, which often includes a solar flare, a prominence disruption and the CME. CME flux ropes begin at the low corona over the polarity inversion lines (PILs) of the photospheric radial magnetic field. Solar eruptions have been explained as the loss of equilibrium of flux ropes held down by the coronal field. The flux ropes may be emerged from the solar interior or gradually formed in the low corona. Alternatively, the CME flux ropes form during the eruptions by magnetic reconnection under the sheared coronal arcades over the PILs. The source regions of CMEs can be large sunspot active regions with kilogauss magnetic field, quiescent prominences in decayed magnetic field and coronal streamers over the quiet Sun. After the initiation of the eruption, the CME flux ropes undergo acceleration (deceleration), expansion, rotation, distortion and interaction with the ambient solar wind during the propagation in the heliosphere. The internal plasma and magnetic field of the CME flux ropes are measured when the structure encounters a spacecraft in the solar wind. The interplanetary CMEs (ICMEs) at 1AU have radial dimension ranging 0.1 to 0.5 AU, speed ranging 300 to 1000 km/s, and internal magnetic field ranging 10 to 50 nT. A significant fraction of ICMEs are flux rope type or magnetic clouds (MCs), the field of which are quite consistent with the field produced by a cylindrical flux rope with various orientations. Most MCs produce out-of ecliptic plane magnetic field. When the MCs contain both northward and southward field, they are bipolar MCs. The polarity of the bipolar MCs has been found to have a solar cycle dependence and follows the solar dipole field. MCs containing extended strong southward field cause the most intense geomagnetic disturbances.
Kilpua E.
Li Yadong
Luhmann Janet G.
Lynch Benjamin J.
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