El. knyga: Physical Processes in the Interstellar Medium New edition [Wiley Online]

Chapter 1 Interstellar Matter--An Overview		1	(17)
1.1 Neutral Gas		1	(4)
1.2 Photon-Ionized Gas		5	(3)
1.3 Collision-Ionized Gas		8	(2)
1.4 Magnetic Fields and Cosmic Rays		10	(1)
1.5 Galactic Distribution		11	(4)
1.6 Gravitational Mass		15	(3)
Chapter 2 Elastic Collisions and Kinetic Equilibrium		18	(14)
2.1 Inverse-Square Forces		19	(3)
2.2 Short-Range Forces		22	(3)
2.3 Velocity Distribution Function		25	(3)
2.4 Thermodynamic Equilibrium		28	(4)
Chapter 3 Radiative Processes		32	(38)
3.1 Radiative Transfer		32	(2)
3.2 Emission and Absorption Coefficients		34	(6)
a. Absorption coefficient k(v)		36	(3)
b. Effect of stimulated emission on k(v)		39	(1)
3.3 Emission Lines		40	(6)
a. Optical recombination lines		40	(2)
b. Hydrogen 21-cm emission line		42	(2)
c. Radio maser lines		44	(2)
3.4 Absorption Lines		46	(11)
a. Hydrogen 21-cm line		47	(3)
b. Wide H and H(2) optical lines		50	(1)
c. Narrow optical lines		51	(6)
3.5 Continuous Emission and Absorption by Thermal Electrons		57	(4)
a. Free-free radio and X-ray emission		59	(1)
b. Continuous absorption of radio sources		60	(1)
3.6 Refraction by Free Electrons		61	(9)
a. Dispersion of pulsar signals		61	(2)
b. Interstellar scintillation		63	(2)
c. Faraday rotation		65	(5)
Chapter 4 Excitation		70	(33)
4.1 Excitation by Collisions		71	(16)
a. Collisional rate coefficients		71	(5)
b. Theory for systems with two or three levels		76	(2)
c. Optical emission lines observed from heavy atoms		78	(3)
d. Molecular radio lines		81	(6)
4.2 Excitation by Recombination		87	(7)
a. Lower quantum levels		88	(1)
b. Higher quantum levels		89	(2)
c. Radio recombination lines		91	(3)
4.3 Photon Pumping		94	(9)
a. Atomic levels		95	(1)
b. H(2) rotational levels		96	(7)
Chapter 5 Ionization and Dissociation		103	(28)
5.1 Ionization of Hydrogen		105	(11)
a. Absorption and recombination coefficients		105	(2)
b. H II regions without dust		107	(4)
c. Effect of dust on H II regions		111	(3)
d. Ionization by energetic particles		114	(2)
5.2 Ionization of Heavy Atoms		116	(6)
a. Photon ionization		117	(1)
b. Collisional ionization		118	(1)
c. Charge exchange and reactions with molecules		119	(3)
5.3 Formation and Dissociation of Molecules		122	(9)
a. Equilibrium abundance of H(2)		123	(3)
b. Equilibrium of HD		126	(1)
c. Other molecules		127	(4)
Chapter 6 Kinetic Temperature		131	(18)
6.1 H II Regions		133	(6)
a. Heating function XXX		134	(2)
b. Cooling function XXX and resultant T(E)		136	(3)
6.2 H I Regions		139	(10)
a. Cooling function XXX		140	(2)
b. Heating function XXX		142	(7)
Chapter 7 Optical Properties of Grains		149	(22)
7.1 Optical Efficiency Factors		151	(3)
7.2 Selective Extinction		154	(6)
a. Spatial distribution of grains		154	(3)
b. Variation of extinction with wavelength		157	(3)
7.3 General Extinction		160	(4)
a. Ratio of general-to-selective extinction		160	(1)
b. Mean density and surface area of grains		161	(2)
c. Visible nebulae and representative clouds		163	(1)
7.4 Scattering		164	(2)
a. Diffuse galactic light		164	(1)
b. Scattered light in H II regions		165	(1)
7.5 Infrared Emission		166	(5)
Chapter 8 Polarization and Grain Alignment		171	(20)
8.1 Optical Properties of Nonspherical Particles		172	(2)
8.2 Observed Polarization		174	(8)
a. Dependence on color excess		174	(1)
b. Dependence on wavelength		175	(3)
c. Dependence on galactic longitude		178	(3)
d. Circular polarization		181	(1)
8.3 Alignment		182	(9)
a. Conservative torques		183	(2)
b. Accelerating collisional torques		185	(2)
c. Retarding magnetic torque		187	(4)
Chapter 9 Physical Properties of Grains		191	(23)
9.1 Temperature of the Solid Material		191	(7)
a. H I regions		192	(3)
b. H II regions		195	(3)
9.2 Electric Charge		198	(3)
a. Electron and ion collisions		198	(1)
b. Photoelectric emission		199	(2)
9.3 Radiative Acceleration		201	(4)
a. Gyration around magnetic field		202	(1)
b. Dynamical friction with gas		203	(2)
9.4 Evolution of Grains		205	(9)
a. Formation and growth		205	(4)
b. Denudation and disruption		209	(5)
Chapter 10 Dynamical Principles		214	(12)
10.1 Basic Equations		214	(4)
a. Virial theorem		217	(1)
10.2 Shock Fronts		218	(4)
a. Perfect gas, B=0		219	(2)
b. Hydromagnetic shocks		221	(1)
10.3 Instabilities		222	(4)
a. Rayleigh-Taylor instability		223	(3)
Chapter 11 Overall Equilibrium		226	(20)
11.1 Parameters of the Interstellar Gas		226	(6)
a. Physical state		226	(4)
b. Energy source for cloud motions		230	(2)
11.2 Galactic Equilibrium		232	(7)
a. Spherically symmetric system		232	(1)
b. Plane one-dimensional system		233	(2)
c. Equilibrium in a plane gravitational potential		235	(4)
11.3 Equilibrium of Clouds		239	(7)
a. Spherical cloud, B=0		241	(1)
b. Magnetized cloud		242	(4)
Chapter 12 Explosive Motions		246	(24)
12.1 H II Regions		246	(9)
a. Ionization fronts		247	(2)
b. Initial ionization of the gas		249	(2)
c. Expansion of the ionized gas		251	(4)
12.2 Supernova shells		255	(7)
a. Initial expansion of supernova material		255	(2)
b. Intermediate nonradiative expansion		257	(2)
c. Late isothermal expansion		259	(2)
d. Numerical solutions		261	(1)
12.3 Effect of explosions on clouds		262	(8)
a. H I cloud engulfed by an H II ionization front		262	(4)
b. H I cloud engulfed by a shock front		266	(4)
Chapter 13 Gravitational Motion		270	(28)
13.1 Accretion		270	(6)
a. Uniform streaming of a cold gas		270	(2)
b. Spherical adiabatic inflow		272	(3)
c. Uniform adiabatic streaming		275	(1)
13.2 Spiral Density Waves		276	(5)
a. Equations for gas motion in a spiral disk		277	(3)
b. Occurrence of shock fronts		280	(1)
13.3 Gravitational Condensation and Star Formation		281	(17)
a. Gravitational instability		282	(4)
b. Gravitational collapse of a sphere		286	(2)
c. Fragmentation		288	(3)
d. Transfer of angular momentum		291	(2)
e. Decrease of magnetic flux		293	(5)
Symbols		298	(9)
Index		307

Lyman Spitzer, Jr. studied at Yale and Cambridge Universities and earned his Ph.D. under Henry Norris Russell at Princeton University. Following research at Harvard, teaching at Yale, and war work in New York, Spitzer succeeded Russell as professor and observatory director at Princeton in 1947. He promptly hired Martin Schwarzschild, with whom he built a major research department. Spitzer worked in many areas of theoretical astrophysics, including spectral line formation, the dynamical evolution of star clusters, and star formation. His most important work was on the physics of the interstellar medium. He showed that there must be at least two phases - high temperature clouds around hot stars and cooler intercloud regions, and led in studies of interstellar dust grains and magnetic fields. Spitzer was the first to propose a large telescope in space (in 1946) - he was analyzing data from the Hubble Space Telescope the day he died. He led the development and operation of the ultraviolet astronomy satellite Copernicus. An early leader in attempts to harness controlled thermonuclear fusion on earth, he was the founder and first director of the Princeton Plasma Physics Laboratory (originally called Project Matterhorn). Lyman Spitzer, Jr., died in 1997. One of NASA's four Great Observatories is named the Spitzer Space Telescope in his memory.