The Heliospheric Magnetic Field

@article{Owens2013TheHM,
  title={The Heliospheric Magnetic Field},
  author={Mathew J. Owens and Robert J. Forsyth},
  journal={Living Reviews in Solar Physics},
  year={2013},
  volume={10},
  pages={1-52}
}
The heliospheric magnetic field (HMF) is the extension of the coronal magnetic field carried out into the solar system by the solar wind. It is the means by which the Sun interacts with planetary magnetospheres and channels charged particles propagating through the heliosphere. As the HMF remains rooted at the solar photosphere as the Sun rotates, the large-scale HMF traces out an Archimedean spiral. This pattern is distorted by the interaction of fast and slow solar wind streams, as well as… 
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References

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The Heliospheric Magnetic Field (HMF) is the physical framework in which energetic particles and cosmic rays propagate. Changes in the large scale structure of the magnetic field lead to short- and
The global heliospheric magnetic field
The heliospheric magnetic field originates on the Sun. Portions of the solar field extend up into the corona, the Sun’s outermost atmosphere, where the solar wind originates. The perfectly
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The magnetic field in the heliosphere evolves in response to the photospheric field at its base. This evolution, together with the rotation of the Sun, drives space weather through the continually
The Heliospheric Magnetic Field and Its Extension to the Inner Heliosheath
The general structure of the heliospheric magnetic field is well known and has been extensively studied, mostly in the inner heliosphere, out to the orbit of Saturn. Beyond 10 AU, the Pioneer and now
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The orientation of the heliospheric magnetic field (HMF) in near‐Earth space is generally a good indicator of the polarity of HMF foot points at the photosphere. There are times, however, when the
Direct observational evidence for a heliospheric magnetic field with large excursions in latitude
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Heliospheric Modulation of Galactic Cosmic Rays During Solar Cycle 23
Galactic cosmic rays (GCRs) encounter an outward-moving solar wind with cyclic magnetic-field fluctuation and turbulence. This causes convection and diffusion in the heliosphere. The GCR counts from
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