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Variation in the magnetic field at the Earth's surface resulting from a change in the magneto-sheath position caused by changes in the solar wind momentum density flux, irrespective of the Dessler-Parker-Sckopke relations. The figure is obtained for the case where the magnetopause is at a distance of 10 Earth radii, and the position changes by one Earth radius. The scale on the color code is in nT, where the right column refers to the right outer hand side figure, the left scale to the two others.
Source publication
Sudden pulses in the model solar wind sets the Earth's magnetosphere into damped oscillatory motions. A simple model is capable of explaining many of the basic properties of these oscillations, giving scaling laws for their characteristics in terms of the parameters of the problem, such as the Solar wind momentum density. The period of the oscillat...
Context in source publication
Context 1
... account here only for the first one mentioned, but w unt for both. This is possible in part because of the s total energy of the radiation belt to the change in the m dy allows for predicting the magnetic field perturbation Basically, the perturbations can be explained by a supe features accounted for by the relative motion of these d e shown in Figs. 3 and 4. The figures show the absolut ntial (with respect to the local Earth surface) and the ve ole to be vertical. l simulations for a range of the dynamic response to n in Fig. 1, and the dynamic ith small arrows giving the g the direction of the local on of a bow-shock and a ertical dashed lines indicate hat Log (n) = 0 corresponds right ...
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Citations
It is argued that a simple model based on magnetic image arguments suffices to give a convincing insight into both the basic static as well as some transient dynamic properties of the near-Earth'ss magnetosphere, particularly accounting for damped oscillations being excited in response to impulsive perturbations. The parameter variations of the frequency are given. Qualitative results can also be obtained for heating due to the compression of the radiation belts. The properties of this simple dynamic model for the solar wind–magnetosphere interaction are discussed and compared to observations. In spite of its simplicity, the model gives convincing results concerning the magnitudes of the near-Earth's magnetic and electric fields. The database contains ground-based results for magnetic field variation in response to shocks in the solar wind. Here, the observations also include data from the two Van Allen satellites.
