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Cosmic magnetic fields /
Magnetic fields are important in the Universe and their effects contain the key to many astrophysical phenomena that are otherwise impossible to understand. This book presents an up-to-date overview of this fast-growing topic and its interconnections to plasma processes, astroparticle physics, high...
| Clasificación: | Libro Electrónico |
|---|---|
| Autor principal: | |
| Formato: | Electrónico eBook |
| Idioma: | Inglés |
| Publicado: |
Cambridge :
Cambridge University Press,
2016.
|
| Colección: | Cambridge astrophysics series ;
53. |
| Temas: | |
| Acceso en línea: | Texto completo |
MARC
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| 100 | 1 | |a Kronberg, Philipp P., |d 1939- | |
| 245 | 1 | 0 | |a Cosmic magnetic fields / |c Philipp P. Kronberg, University of Toronto. |
| 264 | 1 | |a Cambridge : |b Cambridge University Press, |c 2016. | |
| 300 | |a 1 online resource | ||
| 336 | |a text |b txt |2 rdacontent | ||
| 337 | |a computer |b c |2 rdamedia | ||
| 338 | |a online resource |b cr |2 rdacarrier | ||
| 490 | 1 | |a Cambridge astrophysics series ; |v 53 | |
| 504 | |a Includes bibliographical references and index. | ||
| 588 | 0 | |a Online resource; title from PDF title page (EBSCO, viewed October 13, 2016). | |
| 520 | |a Magnetic fields are important in the Universe and their effects contain the key to many astrophysical phenomena that are otherwise impossible to understand. This book presents an up-to-date overview of this fast-growing topic and its interconnections to plasma processes, astroparticle physics, high energy astrophysics, and cosmic evolution. The phenomenology and impact of magnetic fields are described in diverse astrophysical contexts within the Universe, from galaxies to galaxy clusters, the filaments and voids of the intergalactic medium, and out to the largest redshifts. The presentation of mathematical formulae is accessible and is designed to add insight into the broad range of topics discussed. Written for graduate students and researchers in physics, astrophysics and related disciplines, this volume will inspire readers to devise new ways of thinking about magnetic fields in space on galaxy scales and beyond. | ||
| 546 | |a Text in English. | ||
| 505 | 0 | |a Cover -- Half-title -- Series information -- Title page -- Copyright information -- Dedication -- Table of contents -- Preface -- 1 A brief history and background -- 1.1 Overview of some early results and concepts -- 1.2 Observational techniques and results: past, present, and future prospects -- References -- 2 Methods for probing magnetic fields in diffuse astrophysical plasmas -- 2.1 Introduction -- 2.2 Some basics of polarised EM waves -- 2.3 Zeeman splitting of spectral lines -- 2.4 Polarisation of optical starlight and dust radiation as a probe of interstellar fields -- 2.5 Radio telescope techniques for polarimetry -- 2.6 Faraday rotation -- 2.6.1 Faraday rotation combined with independent thermal electron densities -- 2.6.2 When is Faraday rotation negligible? -- 2.7 The concept of Faraday depth and magnetic field probes in the 3rd dimension -- 2.7.1 Idealised models -- 2.7.2 Faraday rotation in cosmic radio sources -- 2.8 The Crab Nebula as a 3-D Faraday synthesis model -- 2.9 Some instrumental and measurement effects involved in Faraday rotation imaging -- 2.10 Faraday tomography to model magnetic structures in the 3rd dimension -- 2.11 Total energy and magnetic field estimates for synchrotron-radiating clouds -- 2.12 Prospects for magnetic field measurement in other energy bands -- 2.12.1 Far ultraviolet and X-ray observations -- 2.12.2 Extragalactic fields, high energy cosmic rays, and?-rays -- References -- 3 Mechanisms for magnetic field generation and regeneration -- 3.1 Introduction -- 3.2 Some basic equations and the magnetic induction equation -- 3.3 Battery processes and seed fields -- 3.3.1 General comments -- 3.3.2 Gas dynamics and the Biermann battery effect -- 3.4 The role of cosmic ray pressure in galactic magnetic fields -- 3.5 Magnetic reconnection -- 3.5.1 Introduction and early insights. | |
| 505 | 8 | |a 3.5.2 Particle acceleration in reconnection configurations -- 3.5.3 Reconnection studies in the Earth's near-space -- 3.5.4 Ion and electron acceleration in reconnection zones -- 3.5.5 Reconnection in 3-D and the role of advanced computer simulations -- 3.6 Effects of neutral gas -- References -- 4 Galactic ''microcosms'' of extragalactic magnetic systems -- 4.1 Introductory comments -- 4.2 The Sun -- 4.2.1 Magnetic fields in the Solar tachocline -- 4.2.2 Magnetic phenomena above the photosphere -- 4.2.3 Magnetic processes in the outer Solar wind -- 4.3 Magnetic fields in other stars -- 4.3.1 Brief overview of stellar magnetic field measurements -- 4.3.2 Dynamical and magnetic effects in stars compared -- 4.3.3 Magnetic flux removal by stellar jets -- 4.4 Jets from Galactic stars -- 4.5 Molecular clouds and the role of magnetic fields in star formation -- 4.5.1 Observations and numbers -- 4.5.2 Summary -- 4.6 The generation and regeneration of magnetic fields in supernova remnants -- 4.6.1 The Crab Nebula and other plerion-type supernova remnants -- 4.6.2 Magnetic fields and CR energisation in shell-type supernova remnants -- 4.6.3 Electron acceleration by lower hybrid waves -- 4.7 A magnetised jet in the Galactic centre -- References -- 5 Magnetic field configurations in large galaxies -- 5.1 Introduction -- 5.1.1 Some specific questions and puzzles -- 5.1.2 Instrumental capabilities -- 5.2 Our Milky Way -- a spiral galaxy from within -- 5.2.1 Basic features of the large scale magnetic structure -- 5.2.2 Magnetic field structure within the Galactic disc -- 5.2.3 Magnetic field strength variation with Galactocentric radius -- 5.3 Magnetic structures of spiral galaxies -- 5.3.1 Magnetic structure in ''grand design'' spiral galaxies -- 5.3.2 Off-plane and 3-D galaxy halo field configurations. | |
| 505 | 8 | |a 5.3.3 Optical polarisation as a magnetic field tracer in galaxies -- 5.4 Some dynamical and energetic aspects of galaxies -- 5.5 Basic principles of the galactic?-? dynamo -- 5.5.1 A very brief history -- 5.5.2 Some basics of the mean field galactic dynamo theory -- 5.5.3 Some simple solutions to the Mean Field Dynamo Equation -- 5.5.4 Some limitations of galactic mean field dynamo theory -- 5.5.5 Modifications of the galactic dynamo when incorporating disc outflow -- 5.5.6 The régime of very strong stellar/SN-driven galactic outflows -- References -- 6 Magnetic field outflow from dwarf and starburst galaxies -- 6.1 Introduction -- 6.2 Star formation in galaxies and associated magnetised outflows -- 6.2.1 Outflows measured in edge-on galaxies -- 6.2.2 Magnetic fields in strong outflows and ''starbursts'' -- 6.2.3 Magnetic structures in dwarf galaxies -- 6.2.4 Summary of the star-driven magnetic outflow story -- 6.2.5 Could a galaxy self-seed its own large scale magnetic field? -- 6.2.6 Magnetic amplification within outflow winds due to strongly shearing flows -- 6.3 IGM seeding due to ''conventional'' stellar processes in galaxies -- References -- 7 Extragalactic jets and lobes -- I -- 7.1 How much energy and from where? -- 7.1.1 Some background and earlier history -- 7.1.2 What creates the collimated high energy flows? -- 7.2 Jets as electromagnetically driven systems -- 7.3 Representative model simulations of radio lobes fed by a Poynting flux jet -- 7.3.1 Examples of computational frameworks -- 7.3.2 Extensions to classical, non-relativistic MHD simulations -- 7.3.3 Non-relativistic MHD simulations of a ''magnetic tower'', Poynting flux-dominated jet -- 7.3.4 Instabilities and disruption in magnetic tower jets and lobes -- 7.4 Tests of kpc scale jet-lobe systems in different environments. | |
| 505 | 8 | |a 7.4.1 Radio lobes: The importance of magnetic pressure and stability -- 7.4.2 Galaxy cluster bubble tests for the role of magnetism in BH-powered radio/X-ray lobes -- 7.5 Some specific ideas on extraction of magnetic energy at the central BH -- 7.5.1 General comments -- 7.6 Electromagnetic extraction of collimated power flow at the black hole -- 7.7 Another concept: Extraction of BH energy from the inner accretion disc, outside the ergosphere -- 7.8 Summary of two SMBH jet models -- 7.9 Simulations of protostellar jets -- References -- 8 Extragalactic jets and lobes -- II. More on magnetic energy flows into the IGM from galaxy nuclei -- 8.1 Introduction -- 8.2 An electric circuit model for energy flow from a supermassive black hole -- 8.2.1 Analogy of an electrical circuit -- 8.2.2 Observational manifestations of the energy dissipation -- 8.3 Plasma parameter estimates for a ''typical'' BH-driven jet-lobe system outside of a large galaxy cluster -- 8.3.1 3C303 -- a case study of a well-studied, moderately powerful radio galaxy -- 8.3.2 What causes a jet's sudden disruption? -- 8.3.3 Milli-arcsecond jet structures close to the black hole progenitor -- 8.4 Extragalactic jets as transmission lines and CR accelerators -- 8.4.1 Jets as analogues of a transmission line -- 8.4.2 Particle acceleration in jets -- 8.5 Probes of the internal gas physics in magnetised radio lobes and halos -- 8.5.1 Test for the relative lobe-internal energies in relativistic electrons and magnetic fields using Inverse Compton scattered CMB photons -- 8.5.2 Magnetic field deduced from self-Compton and synchrotron emission in radio hotspots -- 8.5.3 Faraday rotation, depolarisation,?B, and nth in radio lobes -- 8.6 SMBH masses and magnetisation of the IGM -- 8.7 Some basic calculations relating to BH-powered outflow. | |
| 505 | 8 | |a 8.8 Observational/experimental quantification of BH energy output to the IGM -- 8.9 Implications of constraints imposed by the energy gap in Fig. 8.2 -- 8.10 Additional calculations of global energy release from galactic BHs into the IGM and estimates of the photon energy component -- 8.10.1 The average mass density of central galactic black holes -- 8.10.2 Global estimates of magnetic energy density from galaxies -- 8.11 Some consequences of ''captured'' energy release from galactic BHs -- 8.12 Summary of some questions -- References -- 9 Magnetic fields associated with clusters and groups of galaxies -- 9.1 Introduction -- 9.1.1 Prologue to intracluster gas studies -- 9.1.2 Early radio and optical indications of an ICM -- 9.1.3 Introduction -- 9.1.4 A single dominant BH-powered source for the Coma Cluster's enhanced radio halo? -- 9.1.5 Overview of the causes of the cluster halo emission -- 9.2 Methods for probing galaxy cluster magnetic fields -- 9.2.1 General -- 9.2.2 Two-dimensional RM mapping of a single cluster using background radio sources -- 9.2.3 A statistical RM probe by ''stacking'' many clusters -- 9.2.4 Multiple source 2-D Faraday rotation mapping over a single cluster -- 9.2.5 Deduction of the ICM magnetic field strength from?RM (?,?) for varying model cluster parameters -- 9.2.6 Further prospects for 3-D magnetic probes of clusters -- 9.3 Magnetic fields and cluster cooling -- 9.4 Energy components of the intracluster medium (ICM) -- 9.5 Regeneration and amplification of magnetic fields in the intracluster medium -- 9.5.1 Scenarios before and after cluster formation that influence the magnetic state of the intracluster medium -- 9.5.2 Field regeneration in merger-driven shocks and turbulence -- 9.5.3 Comments on injection of magnetic fields into the ICM by galactic supermassive black holes. | |
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| 650 | 6 | |a Champs magnétiques. | |
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