Klientu atbalsts: 27018494

Grāmatu iegāde | Jauns profils | Ienākt

E-grāmata: Physics of Interstellar Dust [Taylor & Francis e-book]

Endrik Krugel

Formāts: 584 pages
Sērija : Series in Astronomy and Astrophysics
Izdošanas datums: 07-Jan-2019
Izdevniecība: CRC Press
ISBN-13: 9780429137433

Citas grāmatas par šo tēmu:

Taylor & Francis e-book
Cena: 373,53 €*
* this price gives unlimited concurrent access for unlimited time
Standarta cena: 533,61 €
Ietaupiet 30%

Formāts: 584 pages
Sērija : Series in Astronomy and Astrophysics
Izdošanas datums: 07-Jan-2019
Izdevniecība: CRC Press
ISBN-13: 9780429137433

Citas grāmatas par šo tēmu:

More info about Taylor & Francis e-books

Rokasgrāmatas mājas lapa: https://www.taylorfrancis.com/books/9780429137433

Interstellar dust grains catalyse chemical reactions, absorb, scatter, polarise and re-radiate starlight and constitute the building blocks for the formation of planets. Understanding this interstellar component is therefore of primary importance in many areas of astronomy & astrophysics. For example, observers need to understand how dust effects light passing through molecular clouds. Astrophysicists wish to comprehend how dust enables the collapse of clouds or how it determines the spectral behaviour of protostars, star forming regions or whole galaxies. This book gives a thorough theoretical description of the fundamental physics of interstellar dust: its composition, morphology, size distribution, dynamics, optical and thermal properties, alignment, polarisation, scattering, radiation and spectral features.

This encyclopedic book provides the basic physics towards understanding the solid matter in interstellar space. It includes all the necessary physics, including solid state physics, radiative transport, optical properties, thermodynamics, statistical mechanics and quantum mechanics. It then uses all of this basic physics in the specific case of dust grains in the interstellar medium.

Interstellar dust clouds catalyze simple chemical reactions, absorbs, scatters, polarizes and re-radiates starlight and forms the building blocks for planet and stellar formation. Understanding this interstellar medium is then of primary importance in many areas of astronomy & astrophysics. For example observers need to understand how it effects light passing through dust and molecular clouds, astrophysicists need to comprehend the formation and structure of dust clouds and how it collapses to form stars and planets.

Written in an accessible and descriptive manner, this will be essential supplementary reading for advanced undergraduate and graduate students taking courses on the interstellar medium and active researchers in need of a single source of well illustrated and detailed information.

Preface

xix

1 The dielectric permeability

(43)

1.1 Maxwell's equations

(9)

1.1.1 Electric field and magnetic induction

(1)

1.1.2 Electric polarization of the medium

(1)

1.1.3 The dependence of the dielectric permeability on direction and frequency

(1)

1.1.4 The physical meaning of the electric susceptibility

(2)

1.1.5 Magnetic polarization of the medium

(1)

1.1.6 The magnetic susceptibility

(1)

1.1.7 Dielectrics and metals

(1)

1.1.8 Free charges and polarization charges

(1)

1.1.9 The field equations

(1)

1.2 Waves in a dielectric medium

(5)

1.2.1 The wave equation

(1)

1.2.2 The wavenumber

(1)

1.2.3 The optical constant or refractive index

(1)

1.2.4 Energy dissipation of a grain in a variable field

(2)

1.3 The harmonic oscillator

(7)

1.3.1 The Lorentz model

(1)

1.3.2 Free oscillations

(1)

1.3.3 The general solution to the oscillator equation

(1)

1.3.4 Dissipation of energy in a forced oscillation

(1)

1.3.5 Dissipation of energy in a free oscillation

(1)

1.3.6 The plasma frequency

(1)

1.3.7 Dispersion relation of the dielectric permeability

(2)

1.4 The harmonic oscillator and light

(10)

1.4.1 Attenuation and refraction of light

(1)

1.4.2 Retarded potentials of a moving charge

(2)

1.4.3 Emission of an harmonic oscillator

(1)

1.4.4 Radiation of higher order

(1)

1.4.5 Radiation damping

(1)

1.4.6 The cross section of an harmonic oscillator

(1)

1.4.7 The oscillator strength

(1)

1.4.8 The natural linewidth

(1)

1.5 Waves in a conducting medium

(6)

1.5.1 The dielectric permeability of a conductor

(1)

1.5.2 Conductivity and the Drude profile

(2)

1.5.3 Electromagnetic waves in a plasma with a magnetic field

(1)

1.5.4 Group velocity of electromagnetic waves in a plasma

(1)

1.6 Polarization through orientation

(6)

1.6.1 Polarization in a constant field

(1)

1.6.2 Polarization in a time-variable field

(1)

1.6.3 Relaxation after switching off the field

(1)

1.6.4 The dielectric permeability in Debye relaxation

(3)

2 How to evaluate grain cross sections

(36)

2.1 Defining cross sections

(3)

2.1.1 Cross section for scattering, absorption and extinction

(2)

2.1.2 Cross section for radiation pressure

(1)

2.1.3 Efficiencies, mass and volume coefficients

(1)

2.2 The optical theorem

(4)

2.2.1 The intensity of forward scattered light

(3)

2.2.2 The refractive index of a dusty medium

(1)

2.3 Mie theory for a sphere

(6)

2.3.1 The generating function

(1)

2.3.2 Separation of variables

(2)

2.3.3 Series expansion of waves

(1)

2.3.4 Expansion coefficients

(2)

2.3.5 Scattered and absorbed power

(1)

2.3.6 Absorption and scattering efficiencies

(1)

2.4 Polarization and scattering

(7)

2.4.1 The amplitude scattering matrix

(1)

2.4.2 Angle-dependence of scattering

(2)

2.4.3 The polarization ellipse

(1)

2.4.4 Stokes parameters

(1)

2.4.5 Stokes parameters of scattered light for a sphere

(2)

2.5 The Kramers-Kronig relations

(7)

2.5.1 Mathematical formulation of the relations

(2)

2.5.2 The electric susceptibility and causality

(1)

2.5.3 The Kramers-Kronig relation for the dielectric permeability

(1)

2.5.4 Extension to metals

(1)

2.5.5 Dispersion of the magnetic susceptibility

(1)

2.5.6 Three corollaries of the KK relation

(2)

2.6 Composite grains

(9)

2.6.1 Effective medium theories

(1)

2.6.2 Garnett's mixing rule

(1)

2.6.3 The mixing rule of Bruggeman

(1)

2.6.4 Composition of grains in protostellar cores

(2)

2.6.5 How size, ice and porosity change the absorption coefficient

(4)

3 Very small and very big particles

(39)

3.1 Tiny spheres

(7)

3.1.1 When is a particle in the Rayleigh limit?

(1)

3.1.2 Efficiencies of small spheres from Mie theory

(1)

3.1.3 A dielectric sphere in a constant electric field

(2)

3.1.4 Scattering and absorption in the electrostatic approximation

(1)

3.1.5 Polarization and angle-dependent scattering

(1)

3.1.6 Small-size effects beyond Mie theory

(1)

3.2 A small metallic sphere in a magnetic field

(3)

3.2.1 Slowly varying field

(2)

3.2.2 The magnetic polarizability

(1)

3.2.3 The penetration depth

(1)

3.2.4 Limiting values of the magnetic polarizability

(1)

3.3 Tiny ellipsoids

(9)

3.3.1 Elliptical coordinates

(1)

3.3.2 An ellipsoid in a constant electric field

(1)

3.3.3 Cross section and shape factor

(2)

3.3.4 Randomly oriented ellipsoids

(1)

3.3.5 Pancakes and cigars

(2)

3.3.6 Rotation about the axis of greatest moment of inertia

(2)

3.4 The fields inside a dielectric particle

(4)

3.4.1 Internal field and depolarization field

(1)

3.4.2 Depolarization field and the distribution of surface charges

100

(1)

3.4.3 The local field at an atom

101

(1)

3.4.4 The Clausius-Mossotti relation

101

(2)

3.5 Very large particles

103

(16)

3.5.1 Babinet's theorem

103

(1)

3.5.2 Reflection and transmission at a plane surface

104

(2)

3.5.3 Huygens' principle

106

(3)

3.5.4 Fresnel zones and a check on Huygens' principle

109

(2)

3.5.5 The reciprocity theorem

111

(1)

3.5.6 Diffraction by a circular hole or a sphere

111

(2)

3.5.7 Diffraction behind a half-plane

113

(3)

3.5.8 Particles of small refractive index

116

(1)

3.5.9 X-ray scattering

117

(2)

4 Case studies of Mie calculus

119

(26)

4.1 Efficiencies of bare spheres

119

(8)

4.1.1 Pure scattering

119

(1)

4.1.2 A weak absorber

120

(2)

4.1.3 A strong absorber

122

(1)

4.1.4 A metal sphere

123

(1)

4.1.5 Efficiency versus cross section and volume coefficient

123

(3)

4.1.6 The atmosphere of the Earth

126

(1)

4.2 Scattering by bare spheres

127

(5)

4.2.1 The scattering diagram

127

(1)

4.2.2 The polarization of scattered light

128

(3)

4.2.3 The intensity of scattered light in a reflection nebula

131

(1)

4.3 Coated spheres

132

(1)

4.4 Surface modes in small grains

133

(3)

4.5 Efficiencies of idealized dielectrics and metals

136

(9)

4.5.1 Dielectric sphere consisting of identical harmonic oscillators

136

(2)

4.5.2 Dielectric sphere with Debye relaxation

138

(1)

4.5.3 Magnetic and electric dipole absorption of small metal spheres

139

(2)

4.5.4 Efficiencies for Drude profiles

141

(1)

4.5.5 Elongated metallic particles

142

(3)

5 Particle statistics

145

(30)

5.1 Boltzmann statistics

145

(6)

5.1.1 The probability of an arbitrary energy distribution

145

(1)

5.1.2 The distribution of maximum probability

146

(1)

5.1.3 Partition function and population of energy cells

147

(2)

5.1.4 The mean energy of harmonic oscillators

149

(1)

5.1.5 The Max well ian velocity distribution

149

(2)

5.2 Quantum statistics

151

(9)

5.2.1 The unit cell h3 of the phase space

151

(1)

5.2.2 Bosons and fermions

152

(2)

5.2.3 Bose statistics

154

(2)

5.2.4 Bose statistics for photons

156

(1)

5.2.5 Fermi statistics

157

(1)

5.2.6 Ionization equilibrium and the Saha equation

158

(2)

5.3 Thermodynamics

160

(10)

5.3.1 The ergodic hypothesis

160

(2)

5.3.2 Definition of entropy and temperature

162

(1)

5.3.3 The canonical distribution

163

(1)

5.3.4 Thermodynamic relations for a gas

164

(2)

5.3.5 Equilibrium conditions of the state functions

166

(2)

5.3.6 Specific heat of a gas

168

(1)

5.3.7 The work done by magnetization

168

(1)

5.3.8 Susceptibility and specific heat of magnetic substances

169

(1)

5.4 Blackbody radiation

170

(5)

5.4.1 The Planck function

170

(1)

5.4.2 Low- and high-frequency limit

171

(1)

5.4.3 Wien's displacement law and the Stefan-Boltzmann law

172

(1)

5.4.4 The Planck function and harmonic oscillators

173

(2)

6 The radiative transition probability

175

(26)

6.1 A charged particle in an electromagnetic field

175

(6)

6.1.1 The classical Hamiltonian

175

(1)

6.1.2 The Hamiltonian of an electron in an electromagnetic field

176

(1)

6.1.3 The Hamilton operator in quantum mechanics

177

(2)

6.1.4 The dipole moment in quantum mechanics

179

(1)

6.1.5 The quantized harmonic oscillator

179

(2)

6.2 Small perturbations

181

(2)

6.2.1 The perturbation energy

181

(1)

6.2.2 The transition probability

181

(1)

6.2.3 Transition probability for a time-variable perturbation

182

(1)

6.3 The Einstein coefficients A and B

183

(9)

6.3.1 Induced and spontaneous transitions

183

(3)

6.3.2 Selection rules and polarization rules

186

(1)

6.3.3 Quantization of the electromagnetic field

186

(2)

6.3.4 Quantum-mechanical derivation of A and B

188

(4)

6.4 Potential wells and tunneling

192

(9)

6.4.1 Wavefunction of a particle in a constant potential

192

(1)

6.4.2 Potential walls and Fermi energy

192

(2)

6.4.3 Rectangular potential barriers

194

(4)

6.4.4 The double potential well

198

(3)

7 Structure and composition of dust

201

(38)

7.1 Crystal structure

201

(6)

7.1.1 Translational symmetry

201

(2)

7.1.2 Lattice types

203

(4)

7.1.3 The reciprocal lattice

207

(1)

7.2 Binding in crystals

207

(7)

7.2.1 Covalent bonding

208

(1)

7.2.2 Ionic bonding

209

(2)

7.2.3 Metals

211

(2)

7.2.4 van der Waals forces and hydrogen bridges

213

(1)

7.3 Reddening by interstellar grains

214

(10)

7.3.1 Stellar photometry

214

(2)

7.3.2 The interstellar extinction curve

216

(3)

7.3.3 Two-color diagrams

219

(1)

7.3.4 Spectral indices

220

(2)

7.3.5 The mass absorption coefficient

222

(2)

7.4 Carbonaceous grains and silicate grains

224

(10)

7.4.1 Origin of the two major dust constituents

224

(1)

7.4.2 The bonding in carbon

225

(2)

7.4.3 Carbon compounds

227

(5)

7.4.4 Silicates

232

(1)

7.4.5 A standard set of optical constants

233

(1)

7.5 Grain sizes and optical constants

234

(5)

7.5.1 The size distribution

234

(2)

7.5.2 Collisional fragmentation

236

(3)

8 Dust radiation

239

(36)

8.1 Kirchhoff's law

239

(4)

8.1.1 The emissivity of dust

239

(1)

8.1.2 Thermal emission of grains

240

(1)

8.1.3 Absorption and emission in thermal equilibrium

241

(1)

8.1.4 Equipartition of energy

242

(1)

8.2 The temperature of big grains

243

(8)

8.2.1 The energy equation

243

(1)

8.2.2 Approximate absorption efficiency at infrared wavelengths

243

(2)

8.2.3 Temperature estimates

245

(2)

8.2.4 Relation between grain size and grain temperature

247

(1)

8.2.5 Temperature of dust grains near a star

248

(1)

8.2.6 Dust temperatures from observations

249

(2)

8.3 The emission spectrum of big grains

251

(3)

8.3.1 Constant temperature and low optical depth

251

(2)

8.3.2 Constant temperature and arbitrary optical depth

253

(1)

8.4 Calorific properties of solids

254

(8)

8.4.1 Normal coordinates

254

(2)

8.4.2 Internal energy of a grain

256

(1)

8.4.3 Standing waves in a crystal

257

(1)

8.4.4 The density of vibrational modes in a crystal

258

(1)

8.4.5 Specific heat

259

(2)

8.4.6 Two-dimensional lattices

261

(1)

8.5 Temperature fluctuations of very small grains

262

(6)

8.5.1 The probability density P(T)

263

(1)

8.5.2 The transition matrix

263

(2)

8.5.3 Practical considerations

265

(1)

8.5.4 The stochastic time evolution of grain temperature

266

(2)

8.6 The emission spectrum of very small grains

268

(7)

8.6.1 Small and moderate fluctuations

268

(2)

8.6.2 Strong fluctuations

270

(2)

8.6.3 Temperature fluctuations and flux ratios

272

(3)

9 Dust and its environment

275

(44)

9.1 Grain surfaces

275

(10)

9.1.1 Gas accretion on grains

275

(1)

9.1.2 Physical adsorption and chemisorption

276

(3)

9.1.3 The sticking probability

279

(2)

9.1.4 Thermal hopping, evaporation and reactions with activation barrier

281

(2)

9.1.5 Tunneling between surface sites

283

(1)

9.1.6 Scanning time

284

(1)

9.2 Grain charge

285

(4)

9.2.1 Charge equilibrium in the absence of a UV radiation field

285

(1)

9.2.2 The photoelectric effect

286

(3)

9.3 Grain motion

289

(9)

9.3.1 Random walk

289

(1)

9.3.2 The drag on a grain subjected to a constant outer force

289

(3)

9.3.3 Brownian motion of a grain

292

(1)

9.3.4 The disorder time

293

(2)

9.3.5 Laminar and turbulent friction

295

(1)

9.3.6 A falling rain drop

296

(1)

9.3.7 The Poynting-Robertson effect

297

(1)

9.4 Grain destruction

298

(3)

9.4.1 Mass balance in the Milky Way

298

(1)

9.4.2 Destruction processes

299

(2)

9.5 Grain formation

301

(18)

9.5.1 Evaporation temperature of dust

301

(3)

9.5.2 Vapor pressure of small grains

304

(1)

9.5.3 Critical saturation

305

(2)

9.5.4 Equations for time-dependent homogeneous nucleation

307

(1)

9.5.5 Equilibrium distribution and steady-state nucleation

308

(3)

9.5.6 Solutions to time-dependent homogeneous nucleation

311

(5)

9.5.7 Similarity relations

316

(3)

10 Polarization

319

(28)

10.1 Efficiency of infinite cylinders

319

(8)

10.1.1 Normal incidence and picket fence alignment

319

(3)

10.1.2 Oblique incidence

322

(1)

10.1.3 Routing cylinders

322

(3)

10.1.4 Absorption efficiency as a function of wavelength

325

(2)

10.2 Linear polarization through extinction

327

(12)

10.2.1 Effective optical depth and degree of polarization p(λ)

327

(2)

10.2.2 The Serkowski curve

329

(2)

10.2.3 Polarization p(λ) of infinite cylinders

331

(3)

10.2.4 Polarization p(λ) of ellipsoids in the Rayleigh limit

334

(3)

10.2.5 Polarization p(λ) of spheroids at optical wavelengths

337

(1)

10.2.6 Polarization and reddening

338

(1)

10.3 Polarized emission

339

(3)

10.3.1 The wavelength dependence of polarized emission for cylinders

340

(1)

10.3.2 Infrared emission of spheroids

340

(1)

10.3.3 Polarized emission versus polarized extinction

341

(1)

10.4 Circular polarization

342

(5)

10.4.1 The phase shift induced by grains

343

(1)

10.4.2 The wavelength dependence of circular polarization

344

(3)

11 Grain alignment

347

(30)

11.1 Grain rotation

347

(8)

11.1.1 Euler's equations for a rotating body

347

(2)

11.1.2 Symmetric tops

349

(2)

11.1.3 Atomic magnet in a magnetic field

351

(1)

11.1.4 Rotational Brownian motion

351

(2)

11.1.5 Suprathermal rotation

353

(2)

11.2 Magnetic dissipation

355

(9)

11.2.1 Diamagnetism

355

(1)

11.2.2 Paramagnetism

355

(2)

11.2.3 Ferromagnetism

357

(1)

11.2.4 The magnetization of iron above and below the Curie point

358

(1)

11.2.5 Paramagnetic dissipation: spin-spin and spin-lattice relaxation

359

(1)

11.2.6 The magnetic susceptibility for spin-lattice relaxation

360

(2)

11.2.7 The magnetic susceptibility in spin-spin relaxation

362

(2)

11.3 Magnetic alignment

364

(9)

11.3.1 A rotating dipole in a magnetic field

365

(2)

11.3.2 Timescales for alignment and disorder

367

(1)

11.3.3 Super-paramagnetism

368

(1)

11.3.4 Ferromagnetic relaxation

369

(2)

11.3.5 Alignment of angular momentum with the axis of greatest inertia

371

(1)

11.3.6 Mechanical and magnetic damping

372

(1)

11.4 Non-magnetic alignment

373

(4)

11.4.1 Gas streaming

373

(2)

11.4.2 Anisotropic illumination

375

(2)

12 PAHs and spectral features of dust

377

(19)

12.1 Thermodynamics of PAHs

377

(7)

12.1.1 What are PAHs?

377

(1)

12.1.2 Microcanonic emission of PAHs

378

(1)

12.1.3 The vibrational modes of anthracene

379

(2)

12.1.4 Microcanonic versus thermal level population

381

(1)

12.1.5 Does an ensemble of PAHs have a temperature?

382

(2)

12.2 PAH emission

384

(4)

12.2.1 Photoexcitation of PAHs

384

(1)

12.2.2 Cutoff wavelength for electronic excitation

385

(1)

12.2.3 Photo-destruction and ionization

386

(1)

12.2.4 Cross sections and line profiles of PAHs

387

(1)

12.3 Big grains and ices

388

(2)

12.3.1 The silicate features and the band at 3.4 fim

389

(1)

12.3.2 Icy grain mantles

389

(1)

12.4 An overall dust model

390

(6)

12.4.1 The three dust components

392

(3)

12.4.2 Extinction coefficient in the diffuse medium

395

(1)

12.4.3 Extinction coefficient in protostellar cores

395

(1)

13 Radiative transport

396

(29)

13.1 Basic transfer relations

396

(6)

13.1.1 Radiative intensity and flux

396

(2)

13.1.2 The transfer equation and its formal solution

398

(2)

13.1.3 The brightness temperature

400

(1)

13.1.4 The main-beam-brightness temperature of a telescope

401

(1)

13.2 Spherical clouds

402

(7)

13.2.1 Moment equations for spheres

403

(1)

13.2.2 Frequency averages

404

(1)

13.2.3 Differential equations for the intensity

405

(2)

13.2.4 Integral equations for the intensity

407

(1)

13.2.5 Practical hints

407

(2)

13.3 Passive disks

409

(6)

13.3.1 Radiative transfer in a plane parallel layer

409

(5)

13.3.2 The grazing angle in an inflated disk

414

(1)

13.4 Galactic nuclei

415

(3)

13.4.1 Hot spots in a spherical stellar cluster

415

(1)

13.4.2 Low and high luminosity stars

416

(2)

13.5 Line radiation

418

(7)

13.5.1 Absorption coefficient and absorption profile

418

(1)

13.5.2 The excitation temperature of a line

419

(1)

13.5.3 Radiative transfer in lines

420

(5)

14 Diffuse matter in the Milky Way

425

(36)

14.1 Overview of the Milky Way

425

(2)

14.1.1 Global parameters

425

(1)

14.1.2 The relevance of dust

426

(1)

14.2 Molecular clouds

427

(11)

14.2.1 The CO molecule

428

(3)

14.2.2 Population of levels in CO

431

(4)

14.2.3 Molecular hydrogen

435

(1)

14.2.4 Formation of molecular hydrogen on dust surfaces

435

(3)

14.3 Clouds of atomic hydrogen

438

(10)

14.3.1 General properties of the diffuse gas

438

(1)

14.3.2 The 21 cm line of atomic hydrogen

439

(1)

14.3.3 How the hyperfine levels of atomic hydrogen are excited

440

(3)

14.3.4 Gas density and temperature from the 21cm line

443

(1)

14.3.5 The deuterium hyperfine line

444

(2)

14.3.6 Electron density and magnetic field in the diffuse gas

446

(2)

14.4 HII regions

448

(9)

14.4.1 Ionization and recombination

448

(2)

14.4.2 Dust-free HII regions

450

(3)

14.4.3 Dusty HII regions

453

(2)

14.4.4 Bremsstrahlung

455

(1)

14.4.5 Recombination lines

456

(1)

14.5 Mass estimates of interstellar clouds

457

(4)

14.5.1 From optically thin CO lines

457

(1)

14.5.2 From the CO luminosity

458

(1)

14.5.3 From dust emission

459

(2)

15 Stars and their formation

461

(44)

15.1 Stars on and beyond the main sequence

461

(10)

15.1.1 Nuclear burning and the creation of elements

461

(2)

15.1.2 The binding energy of an atomic nucleus

463

(2)

15.1.3 Hydrogen burning

465

(2)

15.1.4 The 3o process

467

(2)

15.1.5 Lifetime and luminosity of stars

469

(1)

15.1.6 The initial mass function

470

(1)

15.2 Clouds near gravitational equilibrium

471

(15)

15.2.1 Virialized clouds

471

(3)

15.2.2 Isothermal cloud in pressure equilibrium

474

(1)

15.2.3 Structure and stability of Ebert-Bonnor spheres

475

(4)

15.2.4 Free-fall of a gas ball

479

(1)

15.2.5 The critical mass for gravitational instability

480

(2)

15.2.6 Implications of the Jeans criterion

482

(2)

15.2.7 Magnetic fields and ambipolar diffusion

484

(2)

15.3 Gravitational collapse

486

(8)

15.3.1 The presolar nebula

486

(1)

15.3.2 Hydrodynamic collapse simulations

487

(4)

15.3.3 Similarity solutions of collapse

491

(3)

15.4 Disks

494

(11)

15.4.1 Viscous laminar flows

494

(3)

15.4.2 Dynamical equations of the thin accretion disk

497

(1)

15.4.3 The Kepler disk

498

(1)

15.4.4 Why a star accretes from a disk

499

(2)

15.4.5 The stationary accretion disk

501

(1)

15.4.6 Thea-disk

501

(2)

15.4.7 Disk heating by viscosity

503

(2)

16 Emission from young stars

505

(1)

16.1 The earliest stages of star formation

505

(3)

16.1.1 Globules

505

(1)

16.1.2 Isothermal gravitationally-bound clumps

506

(2)

16.2 The collapse phase

508

(10)

16.2.1 Tbe density structure of a protostar

508

(5)

16.2.2 Dust emission from a solar-type protostar

513

(2)

16.2.3 Kinematics of protostellar collapse

515

(3)

16.3 Accretion disks

518

(6)

16.3.1 A flat blackbody disk

518

(3)

16.3.2 Aflatnon-blackbodydisk

521

(1)

16.3.3 Radiative transfer in an inflated disk

522

(2)

16.4 Reflection nebulae

524

(2)

16.5 Cold and warm dust in galaxies

526

(5)

16.6 Starburst nuclei

531

(1)

16.6.1 Repetitive bursts of star formation

531

(4)

16.6.2 Dust emission from starburst nuclei

535

(4)

Appendix A Mathematical formulae

539

(6)

Appendix B List of symbols

545

(4)

References

549

(3)

Index

552

Endrik Krügel Max-Planck-Institut für Radioastronomie, Bonn, Germany

Permanent link: https://www.kriso.lv/db/9780429137433_pe.html

Keywords:

E-grāmata: Physics of Interstellar Dust [Taylor & Francis e-book]

Konts un iestatījumi

Meklēšana

Meklēt datubāzē

Refine By

Tēmas Publishers Subjects

Izvēlieties iepirkumu grozu