Articles | Volume 37, issue 3
Review paper
08 May 2019
Review paper |  | 08 May 2019

Kinematic models of the interplanetary magnetic field

Christoph Lhotka and Yasuhito Narita

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Cited articles

Alazraki, G. and Couturier, P.: Solar wind acceleration caused by the gradient of Alfvén wave pressure, Astron. Astrophys., 13, 380–389, 1971. a
Alfvén, H.: On the theory of comet tails, Tellus, 9, 92–96,, 1957. a
Banaszkiewicz, M., Axford, W. I., and McKenzie, J. F.: An analytic solar magnetic field model, Astron. Astrophys., 337, 940–944, 1998. a
Belcher, J. W.: Alfvénic wave pressures and the solar wind, Astrophys. J., 168, 509,, 1971. a
Benkhoff, J., van Casteren, J., Hayakawa, H., Fujimoto, M., Laakso, H., Novara, M., Ferri, P., Middleton, H. R., and Ziethe, R.: BepiColombo – Comprehensive exploration of Mercury: Mission overview and science goals, Planet. Space Sci., 58, 2–20,, 2010. a
Short summary
The interplanetary magnetic field is a consequence of the solar magnetic field and the solar wind. Different magnetic field models exist in literature that allow us to better understand how the solar field extends throughout the solar system. We highlight different aspects of these different interplanetary magnetic field models and discuss possible applications. Verification of these models will become possible using data from the Parker Solar Probe and BepiColombo space mission.