Magnetic Flux Emergence, Activity, Eruptions and Magnetic Clouds: Following Magnetic Field from the Sun to the Heliosphere

Part of the Space Sciences Series of ISSI book series (SSSI, volume 32)

Abstract

We present an overview of how the principal physical properties of magnetic flux which emerges from the toroidal fields in the tachocline through the turbulent convection zone to the solar surface are linked to solar activity events, emphasizing the effects of magnetic field evolution and interaction with other magnetic structures on the latter. We compare the results of different approaches using various magnetic observables to evaluate the probability of flare and coronal mass ejection (CME) activity and forecast eruptive activity on the short term (i.e. days). Then, after a brief overview of the observed properties of CMEs and their theoretical models, we discuss the ejecta properties and describe some typical magnetic and composition characteristics of magnetic clouds (MCs) and interplanetary CMEs (ICMEs). We review some individual examples to clarify the link between eruptions from the Sun and the properties of the resulting ejecta. The importance of a synthetic approach to solar and interplanetary magnetic fields and activity is emphasized.

Keywords

Magnetic flux emergence Magnetic observables Flare Coronal mass ejection Magnetic cloud ICME 

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Copyright information

© Springer Science+Business Media, BV 2008

Authors and Affiliations

  1. 1.University College LondonMullard Space Science LaboratorySurreyUK
  2. 2.Observatoire de ParisLESIA, FRE 2461(CNRS)Meudon Principal CedexFrance
  3. 3.Konkoly Observatory of Hungarian Academy of SciencesBudapestHungary

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