Abstract
The magnetospheric models can essentially be divided into open and closed magnetospheric models. In the open model first proposed by Dungey (1961) the polar field lines are connected to the interplanetary magnetic field (Figure 1a). These field lines are convected downstream in the antisolar direction with the solar wind to form the geomagnetic tail. Solar particles can reach the polar cap by following these connected open field lines adiabatically.
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© 1974 D. Reidel Publishing Company, Dordrecht-Holland
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Scholer, M. (1974). Energetic Solar Particle Access into the Geomagnetic Tail. In: Page, D.E. (eds) Correlated Interplanetary and Magnetospheric Observations. Astrophysics and Space Science Library, vol 42. Springer, Dordrecht. https://doi.org/10.1007/978-94-010-2172-2_26
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DOI: https://doi.org/10.1007/978-94-010-2172-2_26
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