Investigating Magnetic Field Line Lengths in Interplanetary Coronal Mass Ejections Using Energetic Electron Events

Details Investigating Magnetic Field Line Lengths in Interplanetary Coronal Mass Ejections Using Energetic Electron Events Investigating Magnetic Field Line Lengths in Interplanetary Coronal Mass Ejections Using Energetic Electron Events

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsh32a..05k&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SH32A-05

Astronomy and Astrophysics

Astrophysics

[7513] Solar Physics, Astrophysics, And Astronomy / Coronal Mass Ejections, [7524] Solar Physics, Astrophysics, And Astronomy / Magnetic Fields

Scientific paper

About one quarter of the observed interplanetary coronal mass ejections (ICMEs) are characterized by enhanced magnetic fields that smoothly rotate in direction over time scales of about 10 to 50 hours. These ICMEs have the appearance of magnetic flux ropes and are known as “magnetic clouds” (MCs). In a flux rope, the twist of the magnetic field increases with distance from the flux-rope axis. The total lengths of the twisted field lines can be determined using solar energetic particles of known speeds when the solar release time and the 1 AU onset times of the particles are known. A recent examination of about 30 electron events in and near eight ICMEs showed no obvious indication that the field line lengths were longest near the MC boundaries and shortest at the MC axis or outside the MC, contrary to the expectations for a flux-rope. In this study, we use the impulsive beamed electron events observed with the EPAM instrument on the ACE spacecraft to determine the field line lengths inside a sample of ICMEs included in the catalog of Richardson and Cane (2010). In particular, we apply this technique for the first time to ICMEs that are not MCs and compare the field line lengths inside MCs and non-MC ICMEs and in the ambient solar wind outside the ICMEs.

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