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Author: Mohamad Shalaby Publisher: ISBN: Category : Active galactic nuclei Languages : en Pages : 145
Book Description
Blazars are the main source of extragalactic very high energy gamma-rays. These gamma rays annihilate on the extragalactic background light, producing electron-positron pair beams with TeV energies. The pair beams are very dilute, with beam-IGM density ratio of $\alpha \sim 10^{-15}$, ultra-relativistic, $\gamma \sim 10^6$, and energetically subdominant ($\gamma \alpha \sim 10^{-9}$). Such pair beams suffer from prevailing cosmological scale, linear beam-plasma instabilities. The associated instability growth rates suggest that at least initially these overwhelmingly dominate inverse Compton cooling, currently the only alternative mechanism by which the pair beams lose energy. Therefore, the full non-linear evolution of the instabilities is key to determining the mechanism by which these pair-beams lose their energy. Kinetic numerical simulations are the only method by which we can currently study the full non-linear evolution of the blazar-induced beam-plasma instabilities. However, the extreme parameters of the pair beams make direct simulations via existing particle-in-cell (PIC) codes infeasible. To address this, we developed a new Spatially Higher-order Accurate, Relativistic PIC algorithm (SHARP). A one dimensional implementation of the SHARP algorithm (SHARP-1D) is given in detail. We show explicitly that SHARP-1D can overcome a number of the limitations of existing PIC algorithms. Using SHARP-1D, we demonstrate a number of points that are important to correctly simulate the full evolution of beam-plasma instabilities. We show that convergence for PIC algorithms requires increasing both spatial resolution and the number of particles per cell concurrently. For a beam-plasma system, we show that the spectral resolution is another important resolution criteria and under-resolved simulations can lead to erroneous physical conclusions. We quantify the required box sizes to faithfully resolve the spectral support of the instabilities. When the background plasmas contain structure, we show that a significant fraction of beam energy (similar to that in uniform plasma simulations; $\sim 20$\%) is, still, lost during the linear evolution of the electrostatic unstable modes. Compared to uniform plasma growth rates, we find lower growth rates, however, the non-uniform systems stay longer in the linear regime. Therefore, the IGM inhomogeneities are unlikely to affect the efficiency of beam-plasma instabilities to cool the blazar-induced pair beams.
Author: Mohamad Shalaby Publisher: ISBN: Category : Active galactic nuclei Languages : en Pages : 145
Book Description
Blazars are the main source of extragalactic very high energy gamma-rays. These gamma rays annihilate on the extragalactic background light, producing electron-positron pair beams with TeV energies. The pair beams are very dilute, with beam-IGM density ratio of $\alpha \sim 10^{-15}$, ultra-relativistic, $\gamma \sim 10^6$, and energetically subdominant ($\gamma \alpha \sim 10^{-9}$). Such pair beams suffer from prevailing cosmological scale, linear beam-plasma instabilities. The associated instability growth rates suggest that at least initially these overwhelmingly dominate inverse Compton cooling, currently the only alternative mechanism by which the pair beams lose energy. Therefore, the full non-linear evolution of the instabilities is key to determining the mechanism by which these pair-beams lose their energy. Kinetic numerical simulations are the only method by which we can currently study the full non-linear evolution of the blazar-induced beam-plasma instabilities. However, the extreme parameters of the pair beams make direct simulations via existing particle-in-cell (PIC) codes infeasible. To address this, we developed a new Spatially Higher-order Accurate, Relativistic PIC algorithm (SHARP). A one dimensional implementation of the SHARP algorithm (SHARP-1D) is given in detail. We show explicitly that SHARP-1D can overcome a number of the limitations of existing PIC algorithms. Using SHARP-1D, we demonstrate a number of points that are important to correctly simulate the full evolution of beam-plasma instabilities. We show that convergence for PIC algorithms requires increasing both spatial resolution and the number of particles per cell concurrently. For a beam-plasma system, we show that the spectral resolution is another important resolution criteria and under-resolved simulations can lead to erroneous physical conclusions. We quantify the required box sizes to faithfully resolve the spectral support of the instabilities. When the background plasmas contain structure, we show that a significant fraction of beam energy (similar to that in uniform plasma simulations; $\sim 20$\%) is, still, lost during the linear evolution of the electrostatic unstable modes. Compared to uniform plasma growth rates, we find lower growth rates, however, the non-uniform systems stay longer in the linear regime. Therefore, the IGM inhomogeneities are unlikely to affect the efficiency of beam-plasma instabilities to cool the blazar-induced pair beams.
Author: Ferdinand F. Cap Publisher: Academic Press ISBN: 148327098X Category : Science Languages : en Pages : 575
Book Description
Handbook on Plasma Instabilities, Volume 2 consists of four chapters on plasma instabilities. Chapter 14 discusses the various aspects of microinstabilities. Beam-plasma systems are covered in Chapter 15, while the various stabilization methods are presented in Chapter 16. This book concludes with deliberations on parametric effects in Chapter 17. Other topics discussed include the microinstabilities of a homogeneous unmagnetized plasma; kinetic theory of macroscopic instabilities; basic beam physics; and beam-plasma instabilities. The magnetic field configuration stabilization; macroscopic nonmagnetic stabilization methods; parametric instabilities in homogeneous unmagnetized plasmas; and parametric effects in bounded and inhomogeneous plasmas are also elaborated in this text. This publication is beneficial to students and researchers conducting work on unstable plasma.
Author: Anthony L. Peratt Publisher: Springer Science & Business Media ISBN: 1461227801 Category : Science Languages : en Pages : 373
Book Description
During the past decade our understanding of plasma physics has witnessed an explosive growth due to research in two areas: work directed toward controlled nuclear fusion and work in space physics. This book addresses the growing need to apply these complementary discoveries to astrophysics. Today plasma is recognized as the key element to understanding the generation of magnetic fields in planets, stars and galaxies, the accel- eration and transport of cosmic rays, and many other phenomena occurring in interstellar space, in radio galaxies, stellar atmospheres, quasars, and so forth.
Author: B. Coppi Publisher: IOS Press ISBN: 9781586030735 Category : Astrophysics Languages : en Pages : 556
Book Description
This book illustrates new developments in the fields of space and solar physics, stellar physics, extragalactic physics and cosmology. It also elaborates upon the progress of laboratory plasma physics. One of the topics discussed is the existence of collective processes, both linear and non-linear, that can explain key elements of accretion physics, magnetic reconnection, the formation of 'strange' particle distributions, particle scattering phenomena, etc. Astrophysical plasma are dominated by turbulent or quasi-turbulent processes which interactively associate instabilities, radiation processes and plasma-wave scattering. The resulting scenario, which is outside thermodynamics and conventional statistical physics, is too difficult to describe theoretically, but today there are large-scale experiments and powerful computational tools allowing for the exploration of an almost similarly complex variety of phenomena. Several contributions to this book present indications of the influence of nonlinear phenomena in astrophysical applications. This work marks the fast growth of plasma astrophysics thanks to new observations in the high energy band of the spectrum on the one hand and the possibility of validating and bringing to light relevant new theories by increasingly sophisticated machines on the other.
Author: Ferdinand F. Cap Publisher: Academic Press ISBN: 1483271056 Category : Science Languages : en Pages : 494
Book Description
Handbook on Plasma Instabilities, Volume 3, is primarily intended to serve as a sourcebook for obtaining quick information and literature references pertaining to a specific topic. Such a handbook has to be formulated in a way that enables understanding of any one section without requiring full understanding of any other section. Volume 1 (Chapters 1-13) presents the fundamental concepts of plasma physics with applications, and has more the nature of a textbook treating basic plasma physics, containment, waves, and macroscopic instabilities. Volume 2 (Chapters 14-17) covers various aspects of microinstabilities, beam plasma systems, stabilization methods, and parametric effects. The present volume (Chapters 18-22) starts with a discussion on feedback and dynamic stabilization using parametric and other effects. It then treats nonlinear effects and laser-plasma systems. One chapter is devoted to applications and use of instabilities. It concludes with a report on plasma waves and instabilities in cosmic space.
Author: A. Hasegawa Publisher: Springer Science & Business Media ISBN: 3642659802 Category : Science Languages : en Pages : 229
Book Description
In recent years the significant progress in satellite-based observations of plasma states and associated electromagnetic phenomena in space has resulted in the accumulation of much evidence of various plasma instabilities. Today plasma instabilities are believed to be responsible for electromagnetic radiation as well as for many of the macroscopic dynamics of plasmas in space. Most students who begin to study plasma physics are intrigued by the unstable nature of plasmas compared with other states of matter; however, they often become frustrated because there are so many in stabilities. Such frustration explains in part why there is no textbook which treats this subject exclusively. A description of plasma instabilities in a systematic way is nontrivial and takes a pertinacious effort. This book is an attempt to provide a basic introduction on the subject and covers most of the important instabilities. However, the author must apologize for any omission of references to contributions of individuals who deserve more credit. The reader is assumed to have a general knowledge of plasma physics obtainable in an undergraduate course. The book is intended to be used as a reference text on the subject of plasma instabilities at the under graduate level as well as for a text in a special course in graduate school. Because the book is part of a series on physics and chemistry in space, emphasis is placed on plasma instabilities relevant in space plasmas.
Author: E.M. de Gouveia Dal Pino Publisher: Springer Science & Business Media ISBN: 940115466X Category : Science Languages : en Pages : 298
Book Description
In June of 1996, at the idyllic seaside resort of Guarujá, Brazil, a renowned group of researchers in space and astrophysical plasmas met to provide a forum on Advanced Topics on Astrophysical and Space Plasmas at a school consisting of some 60 students and teachers, mainly from Brazil and Argentina, but also from all the other parts of the globe. The purpose was to provide an update on the latest theories, observations, and simulations of space-astrophysical plasma phenomena. The topics covered included space plasma mechanisms for particle acceleration, nonthermal emission in cosmic plasma, magnetohydrodynamic instabilities in solar, interstellar, and other cosmic objects, magnetic field line reconnection and merging, the nonlinear and often chaotic structure of astrophysical plasmas, and the advances in high performance supercomputing resources to replicate the observed phenomena. The lectures were presented by Professor Mark Birkinshaw of the Harvard-Smithsonian Center for Astrophysics and the University of Bristol; Dr Anthony Peratt, Los Alamos National Laboratory Scientific Advisor to the United States Department of Energy; Dr Dieter Biskamp of the Max Planck Institute for Plasma Physics, Garching, Germany; Professor Donald Melrose, Director, Centre for Theoretical Astrophysics, University of Sydney, Australia; Professor Abraham Chian of the National Institute for Space Research, Brazil; and Professor Nelson Fiedler-Ferrara of the University of São Paulo, Brazil. As summarized by Professor Reuven Opher, Institute of Astronomy and Geophysics, University of São Paulo, the advanced or interested student of space and astrophysical plasmas will find reference to nearly all modern aspects in the field of Plasma Astrophysics and Cosmology in the presented lectures.
Author: V.N Oraevsky Publisher: Routledge ISBN: 1351428217 Category : Science Languages : en Pages : 180
Book Description
For the first time in a single book, Non-Linear Instabilities in Plasmas and Hydrodynamics presents the underlying physics of fast secondary instabilities. This exceptionally well-written, introductory book discusses the basic ideas of the physics of secondary or induced, nonlinear instabilities in wave-sustaining media. The authors, world-renowned experts in the field, have brought together the results of papers scattered throughout the literature to explain subjects as diverse as fluctuation chaos, wave-turbulent instabilities, vortex dynamos, beam-plasma interactions, plasma confinement, and the origins of typhoons in the Earth's atmosphere and magnetic fields in galaxies. Paving the way for new and exciting research in the future, this broad, interdisciplinary book enables a wide range of physicists to apply the concepts discussed to obtain new results in plasma physics, space physics, hydrodynamics, and geophysics.
Author: Mohamad Shalaby
Author: Mohamad Shalaby
Author: Ferdinand F. Cap
Author: Anthony L. Peratt
Author: B. Coppi
Author: Ferdinand F. Cap
Author: A. Hasegawa
Author: E.M. de Gouveia Dal Pino
Author: V.N Oraevsky
Author: S. Peter Gary
Author: William B. Pardo