Simulations of coronal disconnection events

Journal Article · Tue Sep 01 04:00:00 EDT 1992 · Journal of Geophysical Research; (United States)

DOI:https://doi.org/10.1029/92JA00443· OSTI ID:6967619

Linker, J A; Van Hoven, G ^[1]; McComas, D J ^[2]

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1. Univ. of California, Irvine (United States)
2. Los Alamos National Lab., NM (United States)

The lack of evidence for magnetic disconnection of coronal mass ejection (CMEs) from the Sun has long been a puzzle, as it implies a buildup of the interplanetary magnetic field (IMF) magnitude over time. Such a buildup is ruled out by observations. Magnetic reconnection above helmet streamer configurations could provide a mechanism for maintaining the observed relative constancy of the (IMF) [McComas et al., 1989]; McComas et al. [1991] showed observational evidence of reconnection above a streamer. The authors investigate this interpretation using time-dependent MHD simulations. They model the opening of new magnetic flux on the Sun (as might occur in a CME or other transient event) as an increase in magnetic flux at the poles of a simulated corona. They find that this perturbation can in fact cause reconnection above an equatorial helmet streamer, and the resultant density signature is similar to the observations of McComas et al. [1991].

• OSTI ID: 6967619
• Journal Information: Journal of Geophysical Research; (United States), Journal Name: Journal of Geophysical Research; (United States) Vol. 97:A9; ISSN JGREA2; ISSN 0148-0227
• Country of Publication: United States
• Language: English

Related Subjects

661300* -- Other Aspects of Physical Science-- (1992-)
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
ATMOSPHERES
COMPUTERIZED SIMULATION
FLUCTUATIONS
INTERPLANETARY MAGNETIC FIELDS
MAGNETIC FIELDS
MAGNETIC FLUX
MAGNETIC RECONNECTION
MASS TRANSFER
MATHEMATICAL MODELS
PLASMA DENSITY
SIMULATION
SOLAR ATMOSPHERE
SOLAR CORONA
STAR MODELS
STELLAR ATMOSPHERES
STELLAR CORONAE
TIME DEPENDENCE
VARIATIONS