Titlebook: Exploration of the Polar Upper Atmosphere; Proceedings of the N Charles S. Deehr,Jan A. Holtet Conference proceedings 1981 D. Reidel Publis

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A Review of Optical F-Region Processes in the Polar Atmosphereof some important F-region emissions in the polar regions are reviewed. The importance of optical emissions for the determination of the quantum yields and quenching coefficients is illustrated for the 0.(.P), 0.(.D), N(.D), n(.P) and 0(.D) states and a set of values deduced from recent experiments

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Neutral Winds in the Polar Capbility of the assumptions made in the reduction of data from a single station. Examples of observations made in the Auroral Zone indicating substantial wind gradients and vertical winds are given. Such observations indicate the importance of small scale disturbances in the Polar thermosphere. Data f

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Difference in Polar Atmospheric Optical Emissions Between Mid-Day and Night-Time Aurorasines, the [OII] lines at 3727-29A and 7320-30A as well as [NI] lines at 3466A and 5199-5201A are prominent. Unlike the night-time auroras, the cusp auroras are almost devoid of N.IP and N.2P bands. N.ING bands in mid-day auroras are probably enhanced through resonant scattering of sunlight by N.ions

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The Solar Wind-Magnetosphere-Ionosphere System: An Overviewdistinct plasma regions, features two important characteristics: (1) As one proceeds from the main particle, energy and momentum source on the sun through the solar wind, the magnetosheath, magnetosphere and ionosphere to the sinks in the neutral atmosphere, one observes an increasingly important fe

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The Distant Magnetosphere: Reconnection in the Boundary Layers, Cusps and Tail Lobesd/or an appreciable intrinsic magnetic moment. If the system is lacking both of these qualities completely, the plasma will impinge directly on it, as, for instance, the solar wind does on the moon. In case of a zero or weak magnetic moment, but with the existence of an extended atmosphere, the plas

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Plasma Sheet Dynamics: Effects on, and Feedback from, the Polar Ionospherearticles; in a systematic approach appropriate to a tutorial lecture, it is more conveniently described by reference to the configuration of the magnetic field. The magnetic field lines within the magnetosphere can be divided into two broad morphological classes: the basically dipolar (although some

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https://doi.org/10.1007/978-1-4302-6101-8an altitude of 100 km. Looking at Fig. 1, we see that the altitude extent of the middle atmosphere varies with latitude and season such that’, for example, the lower boundary of the middle atmosphere, the tropopause, is at about 17 km (about 80 mb) at the equator and at about 8 or 9 km at the pole (

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