Accretion processes in star formation / Lee Hartmann.

Title from publisher's bibliographic system (viewed on 05 Oct 2015).

1.1 Molecular clouds 2 -- 1.2 The IMF, clusters, and binaries 4 -- 1.3 Young stars 5 -- 1.4 Protostars 9 -- 1.5 Long-wavelength emission: dusty envelopes and disks 10 -- 1.6 Imaging of disks 12 -- 1.7 Disk accretion 14 -- 1.8 Disks and planet formation 16 -- 1.9 A picture of star and planet formation 18 -- 2 Beginnings: molecular clouds 21 -- 2.1 Large-scale properties of molecular clouds 21 -- 2.2 Turbulence and cloud lifetimes 23 -- 2.3 Molecular cloud formation and dispersal 26 -- 2.4 Flows, magnetic fields, and cloud formation 30 -- 2.5 Gravity and fragmentation 32 -- 2.6 Sheets and filaments 34 -- 2.7 Turbulence and cloud structure 40 -- 3 Initial conditions for protostellar collapse 43 -- 3.1 Molecular cloud cores 43 -- 3.2 Virial theorem and cloud stability 46 -- 3.3 Centrally concentrated clouds 49 -- 3.4 Core lifetimes and equilibrium 53 -- 3.5 Stability of magnetized clouds 54 -- 3.6 Ambipolar diffusion of magnetic flux 55 -- 3.7 The magnetic flux "problem(s)" 57 -- 4 Protostellar cloud collapse 60 -- 4.1 Free-fall collapse of a uniform cloud 60 -- 4.2 Similarity solution for collapse 61 -- 4.3 Generalized models of protostellar collapse 65 -- 4.4 Rotating collapse 68 -- 4.5 Time evolution of rotating collapse 73 -- 4.6 Disk formation 74 -- 4.7 Massive protostars 76 -- 5 Protostellar collapse: observations vs. theory 82 -- 5.1 Protostellar luminosities and accretion 84 -- 5.2 SEDs of spherical infalling envelopes 86 -- 5.3 SEDs for rotating collapse models 91 -- 5.4 A case study: L1551 IRS 5 94 -- 5.5 The Class 0 sources 98 -- 5.6 Flat spectrum sources 100 -- 5.7 Spatial distribution of emission 103 -- 5.8 Detection of infall from line profiles 104 -- 5.9 Massive protostars 108 -- 6 Binaries, clusters, and the IMF 112 -- 6.1 Observations of binary and multiple systems 113 -- 6.2 Theories of multiple stellar system formation 115 -- 6.3 Evolution of multiple systems during accretion 116 -- 6.4 Young clusters 118 -- 6.5 Cluster formation 121 -- 6.6 The Initial Mass Function 123 -- 6.7 Theories of the IMF 125 -- 7 Disk accretion 129 -- 7.1 Energy minimization and angular momentum conservation 130 -- 7.2 The thin accretion disk 132 -- 7.3 The steady optically thick disk 139 -- 7.4 The [alpha] disk 142 -- 7.5 Sources of viscosity: the magnetorotational instability 143 -- 7.6 The ionization problem 146 -- 7.7 Gravitational instability and angular momentum transport 148 -- 7.8 Disk boundary layers 152 -- 7.9 Disk irradiation 155 -- 8 The disks of pre-main-sequence stars 158 -- 8.1 Disk imaging 161 -- 8.2 Disk SEDs 163 -- 8.3 Long-wavelength emission and disk masses 168 -- 8.4 Disk/magnetosphere accretion 173 -- 8.5 Accretion rates 177 -- 8.6 What drives accretion? 180 -- 8.7 The WTTS 183 -- 8.8 The Herbig Ae/Be stars 184 -- 8.9 The transitional disks 185 -- 9 The FU Orionis objects 188 -- 9.1 Basic observational properties 189 -- 9.2 The accretion disk model 192 -- 9.3 Disk kinematics 196 -- 9.4 Disk properties 200 -- 9.5 Time variability and circumstellar envelopes 203 -- 9.6 Outburst mechanisms 205 -- 9.7 The boundary layer problem 210 -- 9.8 Outburst statistics and evolutionary significance 211 -- 10 Disk winds, jets, and magnetospheric accretion 213 -- 10.1 Outflows and jets 213 -- 10.2 P Cygni profiles 216 -- 10.3 FU Ori disk winds 219 -- 10.4 T Tauri winds 222 -- 10.5 Mass loss rates 223 -- 10.6 Magnetocentrifugal acceleration and collimation 228 -- 10.7 Magnetohydrodynamic flows 229 -- 10.8 MHD disk winds 233 -- 10.9 Applications of MHD disk wind theory 237 -- 10.10 Models of magnetospheric accretion 240 -- 11 Disk accretion and early stellar evolution 247 -- 11.1 Pre-main-sequence stellar evolutionary tracks 247 -- 11.2 Protostellar properties 252 -- 11.3 The "birthline" 253 -- 11.4 Birthlines: comparison with observations 259 -- 11.5 Age estimates 261 -- 11.6 Star formation histories 264 -- 12 Disk evolution and planet formation 268 -- 12.1 Clearing of optically thick disks 269 -- 12.2 Viscous disk evolution 272 -- 12.3 Binaries 275 -- 12.4 Disk evaporation 276 -- 12.5 Dust evolution 279 -- 12.6 Core accretion and planet formation 284 -- 12.7 Gaseous gravitational instability and planet formation 285 -- 12.8 Migration 286 -- 12.9 Disk gaps and holes 287 -- 12.10 Debris disks 288 -- 12.11 Speculations 290 -- Appendix 1 Basic hydrodynamic and MHD equations 292 -- Appendix 2 Jeans masses and fragmentation 294 -- Appendix 3 Basic radiative transfer 298.

Our understanding of the formation of stars and planetary systems has changed greatly since the first edition of this book was published. This new edition has been thoroughly updated, and now includes material on molecular clouds, binaries, star clusters and the stellar initial mass function (IMF), disk evolution and planet formation. This book provides a comprehensive picture of the formation of stars and planetary systems, from their beginnings in cold clouds of molecular gas to their emergence as new suns with planet-forming disks. At each stage gravity induces an inward accretion of mass, and this is a central theme for the book. The author brings together current observations, rigorous treatments of the relevant astrophysics, and 150 illustrations, to clarify the sequence of events in star and planet formation. It is a comprehensive account of the underlying physical processes of accretion for graduate students and researchers.