{"product_id":"astrophysics-isbn-9781119623557","title":"Astrophysics","description":"\u003cb\u003eASTROPHYSICS\u003c\/b\u003e \u003cp\u003e\u003cb\u003eThis is a balanced textbook presenting the theory and observations of stars and their evolution—a cornerstone of Astrophysics.\u003c\/b\u003e \u003c\/p\u003e\u003cp\u003e\u003ci\u003eAstrophysics: Decoding the Stars\u003c\/i\u003e is a companion volume to \u003ci\u003eAstrophysics: Decoding the Cosmos\u003c\/i\u003e from astrophysics teacher and researcher, Professor Judith Irwin. The text presents an accessible, student-friendly guide to the key theories and principles of stars, emphasizing the close connection between observation and theory.  \u003c\/p\u003e\u003cp\u003eTo aid in reader comprehension, the text includes online resources and problems at the end of each chapter. Many highlighted boxes summarize key concepts or point to example stars that can be seen with the naked eye. The text focuses on physical concepts, but it also refers to the results of numerical models using online resources. \u003c\/p\u003e\u003cp\u003eSample topics covered in \u003ci\u003eAstrophysics: Decoding the Stars\u003c\/i\u003e include: \u003c\/p\u003e\u003cul\u003e\n\u003cli\u003eThe Sun, gaseous and radiative processes\u003c\/li\u003e \u003cli\u003eStellar interiors, energy transport mechanisms, stellar cores and nuclear energy generation, the global energy budget, timescales, and stability\u003c\/li\u003e \u003cli\u003eObservational constraints, variable stars, and star formation from molecular clouds to the ZAMS\u003c\/li\u003e \u003cli\u003eEvolutionary tracks on the HR diagram for stars of different masses, and how stars end their lives\u003c\/li\u003e \u003cli\u003eStellar remnants — white dwarfs, neutron stars and pulsars, and black holes\u003c\/li\u003e\n\u003c\/ul\u003e \u003cp\u003e\u003ci\u003eAstrophysics: Decoding the Stars\u003c\/i\u003e is a highly useful textbook resource for second- to fourth-year undergraduate students pursuing an Astrophysics program, along with Physics undergraduates who have opted to take stellar structure and evolution as part of their program. It will also be useful for new graduate students who want a solid grounding in stellar astrophysics. \u003c\/p\u003e\u003cp\u003ePreface xi\u003c\/p\u003e \u003cp\u003eAcknowledgements xiii\u003c\/p\u003e \u003cp\u003eIntroduction xv\u003c\/p\u003e \u003cp\u003eI. 1 The Simple Physical Star xvii\u003c\/p\u003e \u003cp\u003eI. 2 The Dominance of Gravity for Stars xviii\u003c\/p\u003e \u003cp\u003eI. 3 The Numerical and Analytical Star xxii\u003c\/p\u003e \u003cp\u003eI. 4 The Theoretical and Observational Star xxiii\u003c\/p\u003e \u003cp\u003eProblems xxvi\u003c\/p\u003e \u003cp\u003e\u003cb\u003eChapter 1: The Closest Star 1\u003c\/b\u003e\u003c\/p\u003e \u003cp\u003e1.1 The Sun – First among Equals 2\u003c\/p\u003e \u003cp\u003e1.2 The Solar Atmosphere 4\u003c\/p\u003e \u003cp\u003e1.2.1 Physical Overview 4\u003c\/p\u003e \u003cp\u003e1.2.2 The Photosphere 8\u003c\/p\u003e \u003cp\u003e1.2.3 The Chromosphere 10\u003c\/p\u003e \u003cp\u003e1.2.4 The Transition Region 12\u003c\/p\u003e \u003cp\u003e1.2.5 The Corona 15\u003c\/p\u003e \u003cp\u003e1.2.6 Energy Source for Heating the Solar Atmosphere 17\u003c\/p\u003e \u003cp\u003e1.3 The Solar Interior 18\u003c\/p\u003e \u003cp\u003e1.3.1 The Standard Solar Model (SSM) 18\u003c\/p\u003e \u003cp\u003e1.3.2 Solar Rotation 21\u003c\/p\u003e \u003cp\u003e1.4 The Magnetic Sun 23\u003c\/p\u003e \u003cp\u003eProblems 27\u003c\/p\u003e \u003cp\u003e\u003cb\u003eChapter 2: The Gaseous and Radiative Star – The Basics 29\u003c\/b\u003e\u003c\/p\u003e \u003cp\u003e2.1 The Gaseous Star 29\u003c\/p\u003e \u003cp\u003e2.1.1 The Ideal Gas 29\u003c\/p\u003e \u003cp\u003e2.1.2 Abundances and Metallicity 31\u003c\/p\u003e \u003cp\u003e2.1.3 The Maxwell- Boltzmann Velocity Distribution and Gas Temperature 33\u003c\/p\u003e \u003cp\u003e2.1.4 The Mean Molecular Weight 34\u003c\/p\u003e \u003cp\u003e2.1.5 Fractional Ionization 35\u003c\/p\u003e \u003cp\u003e2.1.6 Pressure of a Partially Ionized Ideal Gas 38\u003c\/p\u003e \u003cp\u003e2.1.7 Degrees of Freedom, Adiabatic Index and Specific Heats 38\u003c\/p\u003e \u003cp\u003e2.1.8 Adiabatic and Isothermal Gases 41\u003c\/p\u003e \u003cp\u003e2.1.9 Gas Motions and the Doppler Shift 43\u003c\/p\u003e \u003cp\u003e2.2 The Radiative Star 44\u003c\/p\u003e \u003cp\u003e2.3 Stellar Opacities 46\u003c\/p\u003e \u003cp\u003eProblems 49\u003c\/p\u003e \u003cp\u003e\u003cb\u003eChapter 3: The Observed Star – Finding the Essential Parameters 53\u003c\/b\u003e\u003c\/p\u003e \u003cp\u003e3.1 Temperature and Spectral Type 54\u003c\/p\u003e \u003cp\u003e3.2 Luminosity and Luminosity Class 59\u003c\/p\u003e \u003cp\u003e3.3 Chemical Composition 62\u003c\/p\u003e \u003cp\u003e3.4 Mass 64\u003c\/p\u003e \u003cp\u003e3.4.1 Visual Binaries 67\u003c\/p\u003e \u003cp\u003e3.4.2 Spectroscopic Binaries 68\u003c\/p\u003e \u003cp\u003e3.5 Radius 71\u003c\/p\u003e \u003cp\u003e3.5.1 Eclipsing Binaries 72\u003c\/p\u003e \u003cp\u003e3.6 Rotation and Winds 75\u003c\/p\u003e \u003cp\u003eProblems 78\u003c\/p\u003e \u003cp\u003e\u003cb\u003eChapter 4: The Shining Star – Interiors 81\u003c\/b\u003e\u003c\/p\u003e \u003cp\u003e4.1 Energy Transport in Stars 82\u003c\/p\u003e \u003cp\u003e4.2 Radiative Transport 82\u003c\/p\u003e \u003cp\u003e4.2.1 The Rosseland Mean Opacity 83\u003c\/p\u003e \u003cp\u003e4.2.2 Analytical Forms for the Mean Opacities 85\u003c\/p\u003e \u003cp\u003e4.2.3 The Equation of Radiative Transport 88\u003c\/p\u003e \u003cp\u003e4.3 Convective Transport 90\u003c\/p\u003e \u003cp\u003e4.3.1 Condition for Convective Instability 90\u003c\/p\u003e \u003cp\u003e4.3.2 Mixing Length Theory 95\u003c\/p\u003e \u003cp\u003e4.3.3 Real Convection 99\u003c\/p\u003e \u003cp\u003e4.4 Conductive Energy Transport in Dense Regions 103\u003c\/p\u003e \u003cp\u003eProblems 105\u003c\/p\u003e \u003cp\u003e\u003cb\u003eChapter 5: The Burning Star – Cores 109\u003c\/b\u003e\u003c\/p\u003e \u003cp\u003e5.1 Classical and Quantum Approaches 110\u003c\/p\u003e \u003cp\u003e5.2 Energy Generation Rate 112\u003c\/p\u003e \u003cp\u003e5.3 Energy Release and Binding Energy 113\u003c\/p\u003e \u003cp\u003e5.4 Main Sequence Reactions 116\u003c\/p\u003e \u003cp\u003e5.4.1 The PP-chain 117\u003c\/p\u003e \u003cp\u003e5.4.2 The CNO Cycle 119\u003c\/p\u003e \u003cp\u003e5.5 Reactions after the Main Sequence 121\u003c\/p\u003e \u003cp\u003e5.5.1 The Triple-α Process – Helium Burning 122\u003c\/p\u003e \u003cp\u003e5.5.2 Additional and Higher Temperature Reactions 123\u003c\/p\u003e \u003cp\u003eProblems 125\u003c\/p\u003e \u003cp\u003e\u003cb\u003eChapter 6: The Modelled Star 127\u003c\/b\u003e\u003c\/p\u003e \u003cp\u003e6.1 The Equations of Stellar Structure 127\u003c\/p\u003e \u003cp\u003e6.1.1 Conservation of Mass 128\u003c\/p\u003e \u003cp\u003e6.1.2 Hydrostatic Equilibrium 129\u003c\/p\u003e \u003cp\u003e6.1.3 Energy Conservation 129\u003c\/p\u003e \u003cp\u003e6.1.4 Energy Transport 130\u003c\/p\u003e \u003cp\u003e6.1.5 Constitutive Relations 130\u003c\/p\u003e \u003cp\u003e6.1.6 Boundary Conditions 131\u003c\/p\u003e \u003cp\u003e6.2 Solving the Equations of Stellar Structure 132\u003c\/p\u003e \u003cp\u003e6.2.1 Numerical Solutions 132\u003c\/p\u003e \u003cp\u003e6.2.2 Conceptual and Analytical Approaches 133\u003c\/p\u003e \u003cp\u003e6.3 The Vogt-Russell Theorem, Mass-Luminosity Relation and Mass-Radius Relation 137\u003c\/p\u003e \u003cp\u003eProblems 146\u003c\/p\u003e \u003cp\u003e\u003cb\u003eChapter 7: The Quasistatic Star – Energies, Timescales and Limits 149\u003c\/b\u003e\u003c\/p\u003e \u003cp\u003e7.1 The Virial Theorem 150\u003c\/p\u003e \u003cp\u003e7.2 Timescales 154\u003c\/p\u003e \u003cp\u003e7.2.1 The Dynamical Timescale 154\u003c\/p\u003e \u003cp\u003e7.2.2 The Thermal (Kelvin-Helmholtz) Timescale 155\u003c\/p\u003e \u003cp\u003e7.2.3 The Nuclear Timescale 156\u003c\/p\u003e \u003cp\u003e7.3 Stability 157\u003c\/p\u003e \u003cp\u003e7.3.1 Stability against Perturbations 158\u003c\/p\u003e \u003cp\u003e7.3.2 Secular Evolution of the Sun along the Main Sequence 158\u003c\/p\u003e \u003cp\u003e7.4 The Minimum and Maximum Stable Stars 159\u003c\/p\u003e \u003cp\u003e7.4.1 The Lowest-Mass Stars 159\u003c\/p\u003e \u003cp\u003e7.4.2 The Highest-Mass Stars 160\u003c\/p\u003e \u003cp\u003e7.5 A Main Sequence Primer 164\u003c\/p\u003e \u003cp\u003eProblems 166\u003c\/p\u003e \u003cp\u003e\u003cb\u003eChapter 8: The Forming and Ageing Star – Evolution to and from the Main Sequence 169\u003c\/b\u003e\u003c\/p\u003e \u003cp\u003e8.1 The Forming Star 169\u003c\/p\u003e \u003cp\u003e8.1.1 The Jeans Criterion and Free-Fall Timescale 170\u003c\/p\u003e \u003cp\u003e8.1.2 Real Star Formation 172\u003c\/p\u003e \u003cp\u003e8.1.3 Protostars 173\u003c\/p\u003e \u003cp\u003e8.1.4 From Protostar to the Zams 177\u003c\/p\u003e \u003cp\u003e8.1.5 Number, Mass and Luminosity Functions 182\u003c\/p\u003e \u003cp\u003e8.2 The Ageing Star 185\u003c\/p\u003e \u003cp\u003e8.2.1 Post-Main-Sequence Evolution of a 1 M  Star 186\u003c\/p\u003e \u003cp\u003e8.2.2 Post-Main-Sequence Evolution of Stars of Different Mass 193\u003c\/p\u003e \u003cp\u003e8.2.3 Connecting Theory with Observations 200\u003c\/p\u003e \u003cp\u003eProblems 206\u003c\/p\u003e \u003cp\u003e\u003cb\u003eChapter 9: The Variable Star – Pulsation 209\u003c\/b\u003e\u003c\/p\u003e \u003cp\u003e9.1 Pulsation 211\u003c\/p\u003e \u003cp\u003e9.2 Asteroseismology 215\u003c\/p\u003e \u003cp\u003e9.3 Radial Pulsation 222\u003c\/p\u003e \u003cp\u003e9.4 The Drivers – The Kappa Mechanism 225\u003c\/p\u003e \u003cp\u003e9.5 Period-Luminosity Relations 227\u003c\/p\u003e \u003cp\u003eProblems 232\u003c\/p\u003e \u003cp\u003e\u003cb\u003eChapter 10: The Dying Star and Its Remnant 233\u003c\/b\u003e\u003c\/p\u003e \u003cp\u003e10.1 Planetary Nebulae 234\u003c\/p\u003e \u003cp\u003e10.2 White Dwarfs – Stellar Cinders 236\u003c\/p\u003e \u003cp\u003e10.2.1 The Mass-Radius Relation for White Dwarfs 237\u003c\/p\u003e \u003cp\u003e10.2.2 The Cooling Curve – A Cosmic Clock 242\u003c\/p\u003e \u003cp\u003e10.3 Supernovae 244\u003c\/p\u003e \u003cp\u003e10.3.1 Core-Collapse Supernovae 248\u003c\/p\u003e \u003cp\u003e10.3.2 Thermonuclear Supernovae 251\u003c\/p\u003e \u003cp\u003e10.4 The Densest Remnants – Neutron Stars and Pulsars 254\u003c\/p\u003e \u003cp\u003e10.4.1 The Mass-Radius Relation for Neutron Stars 256\u003c\/p\u003e \u003cp\u003e10.4.2 Stellar Beacons – Pulsars 257\u003c\/p\u003e \u003cp\u003e10.4.3 The PṖ Relation and Characteristic Age 264\u003c\/p\u003e \u003cp\u003e10.5 The Ultimate Stellar Remnants – Black Holes 266\u003c\/p\u003e \u003cp\u003e10.5.1 Observational Evidence 269\u003c\/p\u003e \u003cp\u003eProblems 272\u003c\/p\u003e \u003cp\u003e\u003cb\u003eChapter 11: A Stellar Invitational 275\u003c\/b\u003e\u003c\/p\u003e \u003cp\u003eAppendix A: Physical and Astronomical Data 279\u003c\/p\u003e \u003cp\u003eAppendix B: The Solar Atmosphere 283\u003c\/p\u003e \u003cp\u003eAppendix C: The Standard Solar Model 287\u003c\/p\u003e \u003cp\u003eAppendix D: Taylor Expansions for the Center of a Star 293\u003c\/p\u003e \u003cp\u003eAppendix E: Chandrasekhar’s Argument for a Declining Pressure Distribution in a Star 295\u003c\/p\u003e \u003cp\u003eAppendix F: Stellar Data 297\u003c\/p\u003e \u003cp\u003eBibliography 301\u003c\/p\u003e \u003cp\u003eIndex 323 \u003c\/p\u003e  \u003cp\u003e\u003cb\u003eProfessor Judith Irwin\u003c\/b\u003e teaches undergraduate and graduate physics, astro-physics, and astronomy in the Department of Physics, Engineering Physics and Astronomy at Queen’s University, Canada. Her research focuses on gaseous halos of spiral galaxies.   \u003c\/p\u003e\u003cp\u003e\u003cb\u003eThis is a balanced textbook presenting the theory and observations of stars and their evolution—a cornerstone of Astrophysics.\u003c\/b\u003e \u003c\/p\u003e\u003cp\u003e\u003ci\u003eAstrophysics: Decoding the Stars\u003c\/i\u003e is a companion volume to \u003ci\u003eAstrophysics: Decoding the Cosmos\u003c\/i\u003e from astrophysics teacher and researcher, Professor Judith Irwin. The text presents an accessible, student-friendly guide to the key theories and principles of stars, emphasizing the close connection between observation and theory.  \u003c\/p\u003e\u003cp\u003eTo aid in reader comprehension, the text includes online resources and problems at the end of each chapter. Many highlighted boxes summarize key concepts or point to example stars that can be seen with the naked eye. The text focuses on physical concepts, but it also refers to the results of numerical models using online resources. \u003c\/p\u003e\u003cp\u003eSample topics covered in \u003ci\u003eAstrophysics: Decoding the Stars\u003c\/i\u003e include: \u003c\/p\u003e\u003cul\u003e\n\u003cli\u003eThe Sun, gaseous and radiative processes\u003c\/li\u003e \u003cli\u003eStellar interiors, energy transport mechanisms, stellar cores and nuclear energy generation, the global energy budget, timescales, and stability\u003c\/li\u003e \u003cli\u003eObservational constraints, variable stars, and star formation from molecular clouds to the ZAMS\u003c\/li\u003e \u003cli\u003eEvolutionary tracks on the HR diagram for stars of different masses, and how stars end their lives\u003c\/li\u003e \u003cli\u003eStellar remnants — white dwarfs, neutron stars and pulsars, and black holes\u003c\/li\u003e\n\u003c\/ul\u003e \u003cp\u003e\u003ci\u003eAstrophysics: Decoding the Stars\u003c\/i\u003e is a highly useful textbook resource for second- to fourth-year undergraduate students pursuing an Astrophysics program, along with Physics undergraduates who have opted to take stellar structure and evolution as part of their program. It will also be useful for new graduate students who want a solid grounding in stellar astrophysics.\u003c\/p\u003e","brand":"Wiley","offers":[{"title":"Default Title","offer_id":47988770504933,"sku":"NP9781119623557","price":62.0,"currency_code":"USD","in_stock":false}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/1842\/7735\/files\/9781119623557.jpg?v=1761781524","url":"https:\/\/k12savings.com\/products\/astrophysics-isbn-9781119623557","provider":"K12savings","version":"1.0","type":"link"}