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Dynamical Astrochemistry [Kõva köide]

(University College London, UK), (University College London, UK), (University of Leeds, UK), (Osservatorio Astronomico di Palermo, Italy), (University College London, UK)
  • Formaat: Hardback, 304 pages, kõrgus x laius: 234x156 mm, kaal: 602 g, No
  • Ilmumisaeg: 13-Dec-2017
  • Kirjastus: Royal Society of Chemistry
  • ISBN-10: 1782627766
  • ISBN-13: 9781782627760
Teised raamatud teemal:
Dynamical AstrochemistrySuurem pilt
  • Formaat: Hardback, 304 pages, kõrgus x laius: 234x156 mm, kaal: 602 g, No
  • Ilmumisaeg: 13-Dec-2017
  • Kirjastus: Royal Society of Chemistry
  • ISBN-10: 1782627766
  • ISBN-13: 9781782627760
Teised raamatud teemal:
Püsilink: https://www.kriso.ee/db/9781782627760.html
Märksõnad:
Written by leading experts in this area, this is the first book specifically devoted to the astrochemistry of dynamically evolving astronomical regions.

Astrochemistry is a well-established interdisciplinary subject and the methods for describing time-dependent chemistry in static or slowly-changing regions of interstellar space have been well-developed over many years. Existing astrochemical books normally describe the subject in terms of chemistry in static or slowly-varying astronomical situations but the most significant astronomical regions are those in which the physical conditions change on timescales that are comparable to or shorter than chemical timescales.

Written by leading experts in this area, this is the first book specifically devoted to the astrochemistry of dynamically evolving astronomical regions. It provides a comprehensive description of this important area of science, stressing in particular the methods that have been developed for specific purposes. It will be of interest to researchers in astrochemistry, including both chemists and physicists and could form the basis of a postgraduate course for research students in chemistry and physics.

Arvustused

This book will no doubt stand as the definitive work in this field for some time to come. If you have even a passing interest in the interstellar medium, either in the Milky Way or in other galaxies, you should read it. Furthermore, you will be able to give it to every future PhD student on their first day and say start here. * The Observatory magazine, Volume 138, No. 1266 *

Chapter 1 Chemistry and Dynamics in the Interstellar Medium
1(20)
1.1 Introduction
1(3)
1.2 Interstellar and Circumstellar Chemistry---A Brief Summary
4(9)
1.2.1 Gas-phase Chemistries
5(4)
1.2.2 Surface Processes on Bare Interstellar Grains
9(2)
1.2.3 Chemistry in Interstellar Ices
11(2)
1.3 Interstellar and Circumstellar Dynamics
13(3)
1.4 Structure of This Book
16(5)
References
19(2)
Chapter 2 Shocks and Turbulence and Their Effects on Chemistry
21(42)
2.1 Introduction
21(3)
2.2 Basics of Single-fluid Hydrodynamics
24(5)
2.2.1 The Single-fluid Hydrodynamic Equations
24(3)
2.2.2 Single-fluid Hydrodynamic Sound Waves
27(1)
2.2.3 Jump Conditions for Plane-parallel Hydrodynamic Shocks
28(1)
2.3 Postshock Molecular Processes
29(5)
2.3.1 H2 Level Populations
30(1)
2.3.2 Chemistry in Shocked Material
31(2)
2.3.3 Molecular Line Radiative Losses
33(1)
2.3.4 Dissociative Shocks
33(1)
2.4 Basics of Single-fluid Ideal MHD
34(6)
2.4.1 The Single-fluid Ideal MHD Equations
34(2)
2.4.2 MHD Waves
36(1)
2.4.3 Single-fluid MHD Shocks
37(3)
2.5 Basics of Multi-fluid Models of MHD Shocks
40(7)
2.5.1 J-type and C-type Shocks
40(3)
2.5.2 The Equations Governing Time-dependent Plane-parallel Multi-fluid Flow
43(1)
2.5.3 Some Applications of Perpendicular Shock Models and an Instability
44(3)
2.6 Detailed Treatments of Grains in Multi-fluid Shock Models
47(3)
2.6.1 A Runaway Effect in a Perpendicular Shock Model
48(1)
2.6.2 A Particle Trajectory Approach to Grain Dynamics in Perpendicular Shocks
49(1)
2.6.3 Grains in Oblique Shocks
49(1)
2.7 Basics of Hydrodynamic Turbulence and of MHD Turbulence
50(13)
2.7.1 The Reynolds Number and the Kolmogorov Spectrum
51(1)
2.7.2 Intermittency
52(1)
2.7.3 Turbulent Viscosity, Boundary Layers and Diffusion
53(1)
2.7.4 MHD Turbulence
54(2)
2.7.5 The Effects of Turbulence on Structure
56(3)
References
59(4)
Chapter 3 Non-thermal Chemistry in the Interstellar Medium
63(70)
3.1 Introduction
63(4)
3.2 Molecular Gas
67(9)
3.2.1 Molecular Clouds
67(5)
3.2.2 The Origin of Turbulence in Molecular Clouds
72(1)
3.2.3 Chemical Transitions in the Diffuse Molecular Gas
73(3)
3.3 Observational Evidence of Turbulent Motions
76(6)
3.4 Chemistry in Turbulent Regions
82(27)
3.4.1 Chemistry in a Magnetized Burgers Vortex
83(7)
3.4.2 Non-equilibrium Chemistry in Magnetized Shocks
90(6)
3.4.3 Non-equilibrium Chemistry in Ideal MHD Simulations: the Sulfur Problem
96(7)
3.4.4 Formation and Excitation of Molecular Hydrogen in Turbulent Dissipation Regions
103(6)
3.5 Dust in Magnetized Turbulence
109(16)
3.5.1 Dust Motions in Magnetized Turbulence
110(3)
3.5.2 Formation of PAHs by Turbulence-induced Shattering Events
113(8)
3.5.3 Dust Accretion in Turbulent Flows: Effects on Chemistry
121(4)
3.6 Chemistry in Transient Small Scale Regions
125(8)
References
129(4)
Chapter 4 Gas Dynamics under Gravity: Star Formation
133(51)
4.1 Formation of Low Mass Stars
135(6)
4.1.1 Introduction
135(1)
4.1.2 The Evolution and Classification of Low Mass Protostars and Prestellar Cores
135(3)
4.1.3 The Paradigm of Spherically Symmetric Isothermal Collapse
138(1)
4.1.4 Hydrostatic Equilibrium of a Single, Isolated, Spherical Cloud
139(2)
4.2 The Hydrodynamics of Gravitational Collapse
141(2)
4.2.1 Magnetically Controlled Collapse and Ambipolar Diffusion
142(1)
4.3 The Chemical Perspective
143(4)
4.3.1 Timescales and the Importance of Chemistry
143(2)
4.3.2 The Nature of Chemical Processes
145(2)
4.4 Chemistry Controlling Collapse
147(1)
4.4.1 MHD Wave Damping
147(1)
4.4.2 Ambipolar Diffusion
148(1)
4.5 Chemistry Diagnosing Physics
148(14)
4.5.1 The Quasi-Statically Contracting Starless Core: L1544
150(4)
4.5.2 Detection and Characterizing Infall Associated with Star Formation
154(4)
4.5.3 The Class 0 Source B335
158(4)
4.6 Later Stages---'Hot Corinos'
162(1)
4.6.1 The Case of IRAS 16293--2422
162(1)
4.7 Other Collapse/Evolution Scenarios and Protoplanetary Disks
163(4)
4.7.1 Episodic Accretion
163(1)
4.7.2 Filamentary Collapse
163(1)
4.7.3 Protoplanetary Discs
164(3)
4.8 Formation of High Mass Stars
167(1)
4.9 Theories of Massive Star Formation
167(3)
4.10 Characterization of the Early Stages of High Mass Star Formation
170(1)
4.11 Chemistry of the Early Stages of Star Formation
171(2)
4.12 Observational Tracers of the Massive-Star-Formation Process
173(7)
4.13 Conclusions
180(4)
References
180(4)
Chapter 5 Stellar Jets and Outflows
184(40)
5.1 Introduction
184(1)
5.2 Observations of Jets and Outflows
185(9)
5.2.1 Observations of Jets
185(3)
5.2.2 Observations of Molecular Outflows from Low Mass Protostars
188(4)
5.2.3 Observations of Outflows from High Mass Stars
192(2)
5.3 Chemistry in Jets
194(20)
5.3.1 Jet Launch Processes
196(1)
5.3.2 A Coupled Chemical-dynamical Model for Protostellar Disc Winds
197(2)
5.3.3 Chemical Results from a Protostellar Disc Wind Model
199(2)
5.3.4 Implications for Jet Chemistry
201(2)
5.3.5 Downstream Jet Chemistry and Structure
203(6)
5.3.6 The Terminal Working Surface and Its Chemistry
209(5)
5.4 Outflows
214(4)
5.4.1 The Outflow/Core Interface
214(1)
5.4.2 Chemistry in the Mixing Zone
215(3)
5.4.3 Outflow Morphologies and Chemistry
218(1)
5.5 Conclusions
218(6)
References
219(5)
Chapter 6 Outflows and Explosions of Evolved Stars
224(34)
6.1 Introduction
224(1)
6.2 Stellar Evolution
224(6)
6.2.1 The Hertzsprung-Russell Diagram
225(1)
6.2.2 Evolutionary Tracks of Solar-mass and Intermediate-mass Stars
226(4)
6.2.3 The Evolution of High-mass Stars
230(1)
6.3 Dynamics of Winds and Mass-loss
230(2)
6.3.1 Simple Steady Hydrodynamic Wind
230(1)
6.3.2 Driving AGB Winds with Stellar Pulsations and Radiation Pressure on Dust
231(1)
6.4 Dust Formation in AGB Outflows
232(2)
6.4.1 Dust in Carbon-rich Outflows
232(1)
6.4.2 Dust in Oxygen-rich Outflows
233(1)
6.4.3 The Influence of an Active Galactic Nucleus
234(1)
6.5 Masers and Measurements of the Magnetic Fields in AGB Outflows
234(1)
6.6 Novae
235(13)
6.6.1 Introduction
235(1)
6.6.2 A Physical Model of Novae
236(1)
6.6.3 The Molecule Formation Epochs
237(1)
6.6.4 Early Stage Chemistry
238(5)
6.6.5 Carbon Dust Formation
243(3)
6.6.6 Silicate Dust Formation
246(1)
6.6.7 Alternative Chemical Pathways to Carbon Dust Formation
246(1)
6.6.8 The Subsequent Evolution of the Dust
247(1)
6.7 Supernovae
248(10)
6.7.1 Supernova Types and Outflow Dynamics
248(1)
6.7.2 Molecule Formation
249(3)
6.7.3 Dust Formation
252(2)
6.7.4 Late Stage Molecules and Dust
254(2)
References
256(2)
Chapter 7 Conclusions: Where Do We Go from Here?
258(13)
7.1 What We Know Now About Dynamical Astrochemistry in the Milky Way
258(2)
7.2 Some Outstanding Questions Remaining for Dynamical Astrochemistry in the Milky Way
260(2)
7.2.1 Shocks
260(1)
7.2.2 Turbulence and Small-scale Structure
261(1)
7.2.3 Star Formation
261(1)
7.2.4 Jets and Outflows
262(1)
7.2.5 Evolved Stars, Novae and Supernovae
262(1)
7.3 Applications of Dynamical Astrochemistry to Two Special Environments
262(7)
7.3.1 Astrochemistry in the Early Universe
262(4)
7.3.2 The Astrochemistry of External Galaxies
266(3)
7.4 Final Remarks
269(2)
References
270(1)
Subject Index 271