恒星结构与演化-第二版-(影印版)
本书特色
[
《恒星结构与演化（第二版）(英文影印版)》详细地介绍了恒星的结构和演化理论。从恒星的组成成分讲起，讲解了恒星中的热核反应过程、热核反应之后的产物、超新星爆发等等一系列想象和理论。对于白矮星、中子星和黑洞也都做了详细介绍。本书适合天体物理方向的科研工作者和研究生阅读。
]
内容简介
[
恒星是*常见的星体。满天星斗中，除了有限的几颗外都是恒星。而白矮星、中子星和黑洞也都是恒星演化的产物。恒星并不能恒久存在，也有初生、也会死亡。《恒星结构与演化（第二版）(英文影印版)》正是刻画恒星壮丽一生的学术著作。科研工作者乃至有一定基础的天文爱好者都不应错过这一佳作。
]
目录
part i the basic equations 1 coordinates, mass distribution, and gravitational fieldin spherical stars1.1 eulerian description1.2 lagrangian description1.3 the gravitational field 2 conservation of momentum2.1 hydrostatic equilibrium2.2 the role of density and simple solutions2.3 simple estimates of central values pc; tc2.4 the equation of motion for spherical symmetry2.5 the non-spherical case2.6 hydrostatic equilibrium in general relativity2.7 the piston model 3 the virial theorem3.1 stars in hydrostatic equilibrium3.2 the virial theorem of the piston model3.3 the kelvin-helmholtz timescale3.4 the virial theorem for non-vanishing surface pressure 4 conservation of energy4.1 thermodynamic relations4.2 the perfect gas and the mean molecularweight4.3 thermodynamic quantities for the perfect, monatomic gas4.4 energy conservation in stars4.5 global and local energy conservation4.6 timescales 5 transport of energy by radiation and conduction5.1 radiative transport of energy5.1.1 basic estimates5.1.2 diffusion of radiative energy5.1.3 the rosseland mean for5.2 conductive transport of energy5.3 the thermal adjustment time of a star5.4 thermal properties of the piston model 6 stability against local, non-spherical perturbations6.1 dynamical instability6.2 oscillation of a displaced element6.3 vibrational stability6.4 the thermal adjustment time6.5 secular instability6.6 the stability of the piston model 7 transport of energy by convection7.1 the basic picture7.2 dimensionless equations7.3 limiting cases, solutions, discussion7.4 extensions of the mixing-length theory 8 the chemical composition8.1 relative mass abundances8.2 variation of composition with time8.2.1 radiative regions8.2.2 diffusion8.2.3 convective regions 9 mass loss part ii the overall problem 10 the differential equations of stellar evolution10.1 the full set of equations10.2 timescales and simplifications 11 boundary conditions11.1 central conditions11.2 surface conditions11.3 influence of the surface conditions and properties ofenvelope solutions11.3.1 radiative envelopes11.3.2 convective envelopes11.3.3 summary11.3.4 the t _r stratification 12 numerical procedure12.1 the shootingmethod12.2 the henyey method12.3 treatment of the first- and second-order time derivatives12.4 treatment of the diffusion equation12.5 treatment of mass loss12.6 existence and uniqueness part iii properties of stellar matter 13 the perfect gas with radiation13.1 radiation pressure13.2 thermodynamic quantities 14 ionization14.1 the boltzmann and saha formulae14.2 ionization of hydrogen14.3 thermodynamical quantities for a pure hydrogen gas14.4 hydrogen-heliummixture14.5 the general case14.6 limitation of the saha formula 15 the degenerate electron gas15.1 consequences of the pauli principle15.2 the completely degenerate electron gas15.3 limiting cases15.4 partial degeneracy of the electron gas 16 the equation of state of stellar matter16.1 the ion gas16.2 the equation of state16.3 thermodynamic quantities16.4 crystallization16.5 neutronization16.6 real gas effects 17 opacity17.1 electron scattering17.2 absorption due to free-free transitions17.3 bound-free transitions17.4 bound-bound transitions17.5 the negative hydrogen ion17.6 conduction17.7 molecular opacities17.8 opacity tables 18 nuclear energy production18.1 basic considerations18.2 nuclear cross sections18.3 thermonuclear reaction rates18.4 electron shielding18.5 the major nuclear burning stages18.5.1 hydrogen burning.18.5.2 helium burning18.5.3 carbon burning and beyond18.6 neutron-capture nucleosynthesis18.7 neutrinos part iv simple stellar models 19 polytropic gaseous spheres19.1 polytropic relations19.2 polytropic stellar models19.3 properties of the solutions19.4 application to stars19.5 radiation pressure and the polytrope n d 3.19.6 polytropic stellar models with fixed k19.7 chandrasekhar’s limiting mass19.8 isothermal spheres of an ideal gas19.9 gravitational and total energy for polytropes19.10 supermassive stars19.11 a collapsing polytrope 20 homology relations20.1 definitions and basic relations20.2 applications to simple material functions20.2.1 the case ? d 020.2.2 the case ? d ? d ‘ d 1; a d b d 020.2.3 the role of the equation of state20.3 homologous contraction 21 simple models in the u-v plane21.1 the u-v plane21.2 radiative envelope solutions21.3 fitting of a convective core21.4 fitting of an isothermal core 22 the zero-agemain sequence22.1 surface values22.2 interior solutions22.3 convective regions22.4 extreme values of m22.5 the eddington luminosity 23 other main sequences23.1 the helium main sequence.23.2 the carbon main sequence.23.3 generalized main sequences 24 the hayashi line24.1 luminosity of fully convectivemodels24.2 a simple description of the hayashi line24.3 the neighbourhood of the hayashi line and the forbidden region24.4 numerical results24.5 limitations for fully convectivemodels 25 stability considerations25.1 general remarks25.2 stability of the piston model25.2.1 dynamical stability25.2.2 inclusion of non-adiabatic effects25.3 stellar stability25.3.1 perturbation equations25.3.2 dynamical stability25.3.3 non-adiabatic effects25.3.4 the gravothermal specific heat25.3.5 secular stability behaviour of nuclear burning part v early stellar evolution 26 the onset of star formation26.1 the jeans criterion26.1.1 an infinite homogeneous medium.26.1.2 a plane-parallel layer in hydrostatic equilibrium26.2 instability in the spherical case26.3 fragmentation 27 the formation of protostars.27.1 free-fall collapse of a homogeneous sphere27.2 collapse onto a condensed object27.3 a collapse calculation27.4 the optically thin phase and the formation of a hydrostatic core27.5 core collapse27.6 evolution in the hertzsprung-russell diagram 28 pre-main-sequence contraction.28.1 homologous contraction of a gaseous sphere28.2 approach to the zero-age main sequence 29 from the initial to the present sun29.1 known solar data29.2 choosing the initial model29.3 a standard solar model29.4 results of helioseismology.29.5 solar neutrinos. 30 evolution on the main sequence30.1 change in the hydrogen content30.2 evolution in the hertzsprung-russell diagram30.3 timescales for central hydrogen burning30.4 complications connected with convection30.4.1 convective overshooting30.4.2 semiconvection30.5 the sch¨onberg-chandrasekhar limit30.5.1 a simple approach: the virial theorem and homology30.5.2 integrations for core and envelope.30.5.3 complete solutions for stars with isothermal cores part vi post-main-sequence evolution 31 evolution through helium burning: intermediate-mass stars31.1 crossing the hertzsprung gap31.2 central helium burning31.3 the cepheid phase.31.4 to loop or not to loop 31.5 after central helium burning 32 evolution through helium burning: massive stars32.1 semiconvection32.2 overshooting32.3 mass loss 33 evolution through helium burning: low-mass stars33.1 post-main-sequence evolution33.2 shell-source homology33.3 evolution along the red giant branch.33.4 the helium flash33.5 numerical results for the helium flash33.6 evolution after the helium flash.33.7 evolution from the zero-age horizontal branch part vii late phases of stellar evolution 34 evolution on the asymptotic giant branch34.1 nuclear shells on the asymptotic giant branch34.2 shell sources and their stability.34.3 thermal pulses of a shell source.34.4 the core-mass-luminosity relation for large core masses.34.5 nucleosynthesis on the agb34.6 mass loss on the agb34.7 a sample agb evolution34.8 super-agb stars.34.9 post-agb evolution 35 later phases of core evolution35.1 nuclear cycles35.2 evolution of the central region 36 final explosions and collapse36.1 the evolution of the co-core36.2 carbon ignition in degenerate cores36.2.1 the carbon flash36.2.2 nuclear statistical equilibrium36.2.3 hydrostatic and convective adjustment36.2.4 combustion fronts.36.2.5 carbon burning in accretingwhite dwarfs36.3 collapse of cores of massive stars36.3.1 simple collapse solutions36.3.2 the reflection of the infall36.3.3 effects of neutrinos36.3.4 electron-capture supernovae36.3.5 pair-creation instability36.4 the supernova-gamma-ray-burst connection part viii compact objects 37 white dwarfs37.1 chandrasekhar’s theory37.2 the corrected mechanical structure37.2.1 crystallization37.2.2 pycnonuclear reactions37.2.3 inverse ˇ decays37.2.4 nuclear equilibrium37.3 thermal properties and evolution of white dwarfs 38 neutron stars38.1 cold matter beyond neutron drip38.2 models of neutron stars39 black holes part ix pulsating stars 40 adiabatic spherical pulsations40.1 the eigenvalue problem.40.2 the homogeneous sphere40.3 pulsating polytropes 41 non-adiabatic spherical pulsations41.1 vibrational instability of the piston model41.2 the quasi-adiabatic approximation41.3 the energy integral41.3.1 the _ mechanism41.3.2 the ” mechanism41.4 stars driven by the _ mechanism: the instability strip41.5 stars driven by the ” mechanism. 42 non-radial stellar oscillations42.1 perturbations of the equilibrium model42.2 normal modes and dimensionless variables42.3 the eigenspectra42.4 stars showing non-radial oscillations part x stellar rotation 43 the mechanics of rotating stellar models43.1 uniformly rotating liquid bodies43.2 the roche model43.3 slowly rotating polytropes. 44 the thermodynamics of rotating stellar models44.1 conservative rotation.44.2 von zeipel’s theorem.44.3 meridional circulation44.4 the non-conservative case.44.5 the eddington-sweet timescale.44.6 meridional circulation in inhomogeneous stars 45 the angular-velocity distribution in stars45.1 viscosity45.2 dynamical stability45.3 secular stabilityreferencesindex
封面
书名:恒星结构与演化-第二版-(影印版)
作者:基彭汉
页数:604
定价:¥106.0
出版社:北京大学出版社
出版日期:2014-12-01
ISBN:9787301251751
PDF电子书大小:75MB 高清扫描完整版