LEADER 05282nam 2200649Ia 450 001 9910143076703321 005 20200520144314.0 010 $a1-282-11852-8 010 $a9786612118524 010 $a3-527-62736-7 010 $a3-527-62737-5 035 $a(CKB)1000000000774666 035 $a(EBL)482320 035 $a(OCoLC)441886927 035 $a(SSID)ssj0000158747 035 $a(PQKBManifestationID)11153939 035 $a(PQKBTitleCode)TC0000158747 035 $a(PQKBWorkID)10151584 035 $a(PQKB)11294714 035 $a(MiAaPQ)EBC482320 035 $a(Au-PeEL)EBL482320 035 $a(CaPaEBR)ebr10313723 035 $a(CaONFJC)MIL211852 035 $a(PPN)163475016 035 $a(EXLCZ)991000000000774666 100 $a20080630d2009 uy 0 101 0 $aeng 135 $aur|n|---||||| 181 $ctxt 182 $cc 183 $acr 200 10$aFrom first light to reionization$b[electronic resource] $ethe end of the Dark Ages /$fMassimo Stiavelli 210 $aWeinheim $cWiley-VCH$dc2009 215 $a1 online resource (232 p.) 300 $aDescription based upon print version of record. 311 $a3-527-40705-7 320 $aIncludes bibliographical references and index. 327 $aFrom First Light to Reionization; Preface; Preface; Contents; 1 Introduction; 1.1 First Light and Reionization; 1.2 The Cosmological Framework; 1.3 Organization of this Book; 1.4 Key Observations in this Field; Part 1 Theory; 2 The First Stars; 2.1 Overview; 2.1.1 First Light; 2.1.2 Forming the First Stars; 2.1.3 The Legacy of the First Stars; 2.2 Before the First Stars; 2.2.1 Recombination and Residual Ionization Fraction; 2.2.2 The Formation of Molecular Hydrogen; 2.2.3 Cooling Functions; 2.3 Forming the First Stars; 2.3.1 Perturbations in the Early Universe 327 $a2.3.2 Collapse of Perturbations in the Early Universe2.3.3 Cooling and the Jeans Instability; 2.3.4 Properties of the First Stars; 2.3.5 Remnants and Signatures of a Population III; 2.4 Primordial HII Regions; 2.5 What if Dark Matter is not Cold?; 2.6 Hints for Further Study; 3 The First Star Clusters and Galaxies; 3.1 Overview; 3.2 Subsequent Generations of Stars; 3.2.1 Second-Generation Population III Stars; 3.2.2 Population III Stars Forming in Self-Shielding Halos; 3.2.3 Late Population III Star Formation by Atomic-Hydrogen Cooling in Massive Halos 327 $a3.2.4 Termination of the First Stars Phase3.3 Containing Gas in the Halos of Population III Stars; 3.3.1 Ionization Heating and Gas Temperature; 3.3.2 The Escape of Gas Heated by Ionization; 3.3.3 The Escape of Gas Following a Supernova Explosion; 3.3.4 Population II.5; 3.4 The First Star Clusters; 3.4.1 Clusters of Population III Stars and of Metal-Poor Stars; 3.4.2 The Origin of Globular Clusters; 3.5 The First Galaxies; 3.6 The First Active Galactic Nuclei; 3.6.1 Population III Black Holes; 3.6.2 Black-Hole Mergers; 3.6.3 The Highest-Redshift QSOs; 3.6.4 Direct Collapse to Black Holes 327 $a3.7 Low-Metallicity HII Regions3.8 Numerical Techniques and Their Limitations; 3.8.1 Collisionless Dynamics; 3.8.2 Collisionless Dynamics: Particle-Mesh Codes; 3.8.3 Collisionless Dynamics: Treecodes; 3.8.4 Gas Dynamics; 3.8.5 Gas Dynamics: Smooth Particle Hydrodynamics; 3.8.6 Gas Dynamics: Eulerian Codes; 3.8.7 Improving Resolution Through Mesh Refinement; 3.8.8 Radiative Transfer; 3.9 Hints for Further Study; 4 Cosmic Reionization; 4.1 Overview; 4.2 The Properties of the Sources of Reionization; 4.2.1 The Surface Brightness of Reionization Sources; 4.2.2 Reionization in a Hydrogen-Only IGM 327 $a4.2.3 Reionization in a Hydrogen-Helium IGM4.2.4 Results for a Homogeneous IGM; 4.2.5 Mean Metallicity at Reionization; 4.3 Adding Realism to the Calculations; 4.3.1 Escape of Ionizing Photons; 4.3.2 Clumpy IGM; 4.3.3 Two-Parameter Models; 4.4 Luminosity Function of Ionizing Sources; 4.4.1 Detecting Lyman ? from Ionizing Sources; 4.5 Reionization by Population III Stars; 4.6 How Is the Intergalactic Medium Enriched?; 4.7 Reheating of the Intergalactic Medium; 4.8 Keeping the Intergalactic Medium Ionized; 4.9 Hints for Further Study; Part 2 Observational Techniques and their Results 327 $a5 Studying the Epoch of Reionization of Hydrogen 330 $aThis up-to-date and concise account of a critical period of the early universe directly links the latest theories and experiments. Targeted at cosmological problems rather than specific methods, it begins with an introduction reviewing the early universe and looks at why reionization is important. The process of reionization analyzes simple analytical considerations and compares existing observations, while a further chapter describes some of the issues regarding the transition from Population III to Population II stars, as well as the constraints that can be derived from WMAP. Further chapter 606 $aBeginning 606 $aCosmology 615 0$aBeginning. 615 0$aCosmology. 676 $a523.1 700 $aStiavelli$b Massimo$0874106 801 0$bMiAaPQ 801 1$bMiAaPQ 801 2$bMiAaPQ 906 $aBOOK 912 $a9910143076703321 996 $aFrom first light to reionization$91951583 997 $aUNINA