Mapping CMEs into the Heliosphere Using Observed Photospheric Magnetic Fields and Coronal Field Modeling

Details Mapping CMEs into the Heliosphere Using Observed Photospheric Magnetic Fields and Coronal Field Modeling Mapping CMEs into the Heliosphere Using Observed Photospheric Magnetic Fields and Coronal Field Modeling

May 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm..sh61a04l&link_type=abstract

American Geophysical Union, Spring Meeting 2001, abstract #SH61A-04 INVITED

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2111 Ejecta, Driver Gases, And Magnetic Clouds

Scientific paper

Virtually all concepts and current models of coronal eruptive activity involve initiation by changes in the photospheric magnetic field followed by opening coronal magnetic fields. The photospheric field changes may include flux emergence or reconfiguration by shearing or other motions, all of which should have an observable signature. Our efforts have focused on searching for such signatures using magnetograph data-based potential field source surface models as a tool. Although these models cannot include the MHD physics that must play a role in coronal transients, they provide a flexible and effective means of data-based numerical experimentation. They also reproduce the general solar cycle trends in the coronal field configuration that have been shown to control the magnetic field characteristics of interplanetary CMEs or ICMEs. But case studies in which changes localized in time are compared against the appearance of specific ICMEs are difficult to both construct and interpret. While part of the reason stems from use of scalar magnetograms and a current-free coronal model, the construction of global magnetic field maps that preserve the key time-dependent features is also a great challenge. We describe the current state of this effort and its implications for eventual realistic modeling of CME initiation and CME/ICME connections from solar magnetic field observations.

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