Ionospheres provides a comprehensive description of the physical, plasma and chemical processes controlling the behavior of ionospheres. The relevant transport equations and related coefficients are derived in detail and their applicability and limitations are described. Relevant wave processes are outlined and important ion chemical processes and reaction rates are presented. The various energy deposition and transfer mechanisms are described in some detail, and a chapter is devoted to the various processes controlling the upper atmosphere and exosphere. The second half of the book presents our current understanding of the structure, chemistry, dynamics and energetics of the terrestrial ionosphere, and other solar system bodies. The final chapter describes ionospheric measurement techniques. The book will form a comprehensive and lasting reference for scientists interested in ionospheres, and it will also prove an ideal textbook for graduate students. It contains extensive student problem sets, and an answer book is available for instructors.

[1] We present the results of model calculations, using our new, four-species, spherical MHD model. Our results are compared with the relevant and limited available data. The resulting comparisons help us to increase our understanding of the interaction processes between the solar wind and the Martian atmosphere/ionosphere. This new model with a spherical grid structure allowed us to use small ($10 km) radial grid spacing in the ionospheric region. We found that the calculated bow shock positions agree reasonably well with the observed values. The calculated results vary with interplanetary magnetic field orientation, solar cycle conditions, and subsolar location. We found that our calculated ion densities, with parameters corresponding to solar cycle minimum conditions, reproduced the Viking 1 observed ion densities well. The calculated solar cycle maximum densities, above $140 km, are also consistent with the appropriate Mars Global Surveyor radio occultation electron densities. Both the calculated solar cycle maximum and solar cycle minimum total transterminator and escape fluxes are significantly smaller than our previously published values. This decrease is due to the improved temperature values used for the recombination rates in this new model, which in turn results in lower ion densities and lower fluxes.

This combination of text and reference book describes the physical, plasma and chemical processes controlling the behaviour of ionospheres, upper atmospheres and exospheres. It summarises the structure, chemistry, dynamics and energetics of the terrestrial ionosphere and other solar system bodies, and discusses the processes, mechanisms and transport equations for solving fundamental research problems. This second edition incorporates new results, model developments and interpretations from the last 10 years. It includes the latest material on neutral atmospheres; the terrestrial ionosphere at low, middle and high latitudes; and planetary atmospheres and ionospheres, where results from recent space missions have yielded fresh data. Appendices outline physical constants, mathematical formulas, transport coefficients, and other important parameters for ionospheric calculations. This is an essential resource for researchers studying ionospheres, upper atmospheres, aeronomy and plasma physics. It is also an ideal textbook for graduate-level courses, with supplementary problem sets, and solutions for instructors at www.cambridge.org/9780521877060.

The theory and observations relating to electron temperatures in the F region of the ionosphere are reviewed. The review is divided into three basic parts. In the first part the theory concerning electron heating, cooling, and energy transport processes is reviewed, and all the relevant expressions are updated. In the second part the behavior of F region electron temperatures, as measured by satellites, rockets, and incoherent scatter radars, is discussed. This portion covers electron temperature variations with altitude, latitude, local time, season, geomagnetic activity, and solar cycle. The third part is primarily devoted to a discussion of the various attempts to compare measured and calculated F region electron temperatures.

An expression for the linear electromagnetic ion cyclotron convective growth rate has been derived, considering multiple ions in the energetic anisotropic component of the plasma (which provides the free energy for the instability) as well as in the cold component of the plasma. This represents a modification of recent treatments investigating electromagnetic ion cyclotron growth rates which have considered only hydrogen ions in the energetic component. Four major effects on the growth and propagation characteristics result from inclusion of heavy ions in the energetic component. Some wave growth occurs at low frequencies below the corresponding marginally unstable wave mode for each heavy ion. Enhanced quasi-monochronomatic peaks in the convective growth rate appear just below the O + and He + gyrofrequency and can be quite pronounced for certain plasma conditions. Stop bands, decreased group velocity and other effects normally attributed to cold heavy ions can be produced or enhanced by heavy ions in the energetic plasma component. Partial or complete suppression of wave growth at frequencies above the marginally unstable wave mode for a particular energetic heavy ion can greatly alter the growth rates that would occur in the absence of this energetic heavy ion. The expression for the linear electromagnetic ion cyclotron convective growth rate along with appropriate plasma parameters was used to investigate the nature of linear wave growth in the plasmapause region. The frequencies of peaks in the convective growth rate given by this model compare favorably with wave measurements in this region. It is conceivable that through wave-particle interactions, electromagnetic ion cyclotron waves could supply the energy source for various plasmapause region phenomena such as the O + torus, the plasma cloak, and stable auroral red arcs. during varying amounts of geomagnetic activity. This is consistent with the theory of Cornwall et al. [ 1970]. Although the indirect evidence presented above and by other investigators is convincing, there still remains the problem of reconciling existing wave measurements with ion cyclotron wave theory. A possible explanation may result from our changing concept of the near plasmapause environment. The presence of heavy ions in the magnetospheric plasma has recently been discovered (e.g., Cornwall and Schultz [1979] and references therein). The plasma in this region consists of an energetic component (ring current plasma) and a cold component (plasmaspheric plasma), both of which contain heavy ions. The ring current is dominated by positive ions with energy _< 200 keV [Williams, 1983]. During the recovery phase of magnetic storms, the low-energy (0.2-17 keV) portion of the ring current at or below L values of 4 is composed mainly of O + and He + [Lundin et al., 1980]. Furthermore, there appears to be a marked composition boundary near L -4, with the heavy ions O + and He + dominating equatorward and with H + dominating poleward. This may be consistent with the much shorter lifetime of H...