How do Heliospheric Remote-Sensing Observations Limit Magnetic Flux Rope Models?

Details How do Heliospheric Remote-Sensing Observations Limit Magnetic Flux Rope Models? How do Heliospheric Remote-Sensing Observations Limit Magnetic Flux Rope Models?

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh24a..02r&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SH24A-02

Astronomy and Astrophysics

Astrophysics

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

Scientific paper

In-situ measurements of coronal mass ejecta (CMEs) display a range of properties, only some of which can be accounted for by current global MHD models. In fact, first-principle models that include the initiation and eruption of the ejecta necessarily produce well-defined flux ropes, whereas only a fraction of CMEs observed in-situ appear to contain a flux rope. In this talk, we summarize our current understanding of the observed properties of interplanetary flux ropes and ejecta in general. We explore ideas that the dichotomy between CMEs and flux ropes might be due to: (1) an observational selection effect, that is, all CMEs do in fact contain flux ropes and that the trajectory of the spacecraft through the event is what determines whether a flux rope is also encountered; (2) interactions of an erupting flux rope with itself or between neighboring flux ropes to produce complex structures in which the flux-rope structure has been significantly modified or destroyed; (3) an evolutionary process, such as relaxation to a low plasma-beta state, which governs whether a flux rope is present or not; or (4) the existence of two (or more) intrinsic mechanisms for producing CMEs, some of which produce flux ropes and some that do not. To assess these ideas, we compare model results with a selection of CMEs observed by the Ulysses, ACE, and STEREO spacecraft.

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