The book provides a comprehensive overview of the eruptive and wave phenomena in the solar atmosphere. One of the ongoing problems in solar physics is the heating of the solar corona. Currently there is a competition between two mechanisms in explaining the heating, i.e., dissipation of energy by waves and small scale frequent coronal magnetic reconnection. However, some studies indicate this may be a joint effect of these two possible mechanisms. Kelvin-Helmholtz Instability (KHI) of propagating magnetohydrodynamic modes in solar flowing structures plays an important role in the solar atmosphere. It can trigger the onset of wave turbulence leading to effective plasma heating and particle acceleration. KHI is a multifaceted phenomenon and the purpose of this book is to illuminate its (instability) manifestation in various solar jets like spicules, dark mottles, surges, macrospicules, Extreme Ultraviolet (EUV) and X-ray jets, as well as rotating, tornado-like, jets, solar wind, and coronal mass ejections.The modeling of KHI is performed in the framework of ideal magnetohydrodynamics. The book consists of 12 chapters and is intended primarily for advanced undergraduate and postgraduate students, as well as early career researchers.
In recent years there has been growing interest in the nucleon-nucleon correl ations inside nuclei. In many respects the motions of the nucleons can be very well described by an overall mean field, so that the motion of each nucleon is governed by the mean field due to all the other nucleons. This concept underlies the Fermi-gas, Hartree-Fock and shell models and has enabled a range of nuclear properties to be calculated, often to surprising accuracy. It gradually became clear, however, that these mean-field models are limited by the effects due to the very strong interactions between the nucleons that occur at short distances; these are the short-range correlations. They are responsible for instance for the high-momentum components in the nucleon momentum dis tribution, and prevent the simultaneous description of the nuclear density and momentum distributions by the same mean field. It thus becomes necessary to develop methods for including the effects of nucleon correlations in nuclei, and these are the main subject of this book. Some related problems of nuclear structure were discussed in an earlier book by the same authors: Nucleon Momentum and Density Distributions in Nuclei (Clarendon Press, Oxford, 1988). The main aim of that book was to study the effects of nucleon-nucleon correlations, both short-range and tensor, on the nucleon momentum distribution, which is particularly sensitive to these correl ations, and on the nucleon density distribution.
The book provides a comprehensive overview of the eruptive and wave phenomena in the solar atmosphere. One of the ongoing problems in solar physics is the heating of the solar corona. Currently there is a competition between two mechanisms in explaining the heating, i.e., dissipation of energy by waves and small scale frequent coronal magnetic reconnection. However, some studies indicate this may be a joint effect of these two possible mechanisms. Kelvin-Helmholtz Instability (KHI) of propagating magnetohydrodynamic modes in solar flowing structures plays an important role in the solar atmosphere. It can trigger the onset of wave turbulence leading to effective plasma heating and particle acceleration. KHI is a multifaceted phenomenon and the purpose of this book is to illuminate its (instability) manifestation in various solar jets like spicules, dark mottles, surges, macrospicules, Extreme Ultraviolet (EUV) and X-ray jets, as well as rotating, tornado-like, jets, solar wind, and coronal mass ejections.The modeling of KHI is performed in the framework of ideal magnetohydrodynamics. The book consists of 12 chapters and is intended primarily for advanced undergraduate and postgraduate students, as well as early career researchers.
This will help us customize your experience to showcase the most relevant content to your age group
Please select from below
Login
Not registered?
Sign up
Already registered?
Success – Your message will goes here
We'd love to hear from you!
Thank you for visiting our website. Would you like to provide feedback on how we could improve your experience?
This site does not use any third party cookies with one exception — it uses cookies from Google to deliver its services and to analyze traffic.Learn More.