Astroparticle Physics

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12.5 Mechanisms for Inflation 253One now needs to ask several further questions: “Whatcould cause such a vacuum energy density?”, “How and whydid inflation stop?”, “How does this solve any of the previouslymentioned problems?”, and “What are the observationalconsequences of inflation?”.12.5 Mechanisms for Inflation“Using the forces we know now, youcan’t make the universe we know now.”George SmootTo predict an accelerating scale factor, an equation of staterelating pressure P and energy density ϱ of the form P =wϱ with w
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Astroparticle Physics
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Prof. Dr. Claus GrupenUniversity of
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VIPrefaceand M.Sc. Mehmet T. Kurt (
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VIIIPrefaceOn top of that, the basi
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XTable of Contents5 Acceleration Me
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XIITable of Contents11 The Cosmic M
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11 Historical Introduction“Look i
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1.1 Discoveries in the 20th Century
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1.2 Discoveries of New Elementary P
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1.3 Start of the Satellite Era 11ex
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1.3 Start of the Satellite Era 13CO
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1.3 Start of the Satellite Era 1519
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1.4 Open Questions 171989) and at e
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1.5 Problems 191.5 Problems1. Work
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22 2 The Standard Model of Elementa
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}28 2 The Standard Model of Element
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353 Kinematics and Cross Sections
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3.1 Threshold Energies 373.1 Thresh
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3.2 Four-Vectors 39Example 3: Consi
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3.2 Four-Vectors 41Example 6: Muon
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3.2 Four-Vectors 43Because of E γ2
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3.3 Lorentz Transformation 45energi
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3.5 Problems 47If j is the particle
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494 Physics of Particleand Radiatio
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4.2 Interaction Processes Used for
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4.2 Interaction Processes Used for
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4.3 Principles of the Atmospheric A
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4.4 Special Aspects of Photon Detec
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4.6 Propagation and Interactions of
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4.8 Problems 61board of a satellite
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635 Acceleration Mechanisms“Physi
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5.2 Acceleration by Sunspot Pairs 6
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5.3 Shock Acceleration 67The ejecte
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5.5 Pulsars 69Since this accelerati
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5.6 Binaries 71one obtains, using E
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5.7 Energy Spectra of Primary Parti
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5.7 Energy Spectra of Primary Parti
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776 Primary Cosmic Rays“It will b
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6.1 Charged Component of Primary Co
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6.2 Neutrino Astronomy 87is only co
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6.2 Neutrino Astronomy 89ν e + e
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6.2 Neutrino Astronomy 91For an ass
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6.2 Neutrino Astronomy 93upward-goi
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6.2 Neutrino Astronomy 957 Be + p
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6.2 Neutrino Astronomy 97A reconstr
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6.2 Neutrino Astronomy 99nos (or in
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6.2 Neutrino Astronomy 101In the ho
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6.2 Neutrino Astronomy 103The exper
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6.2 Neutrino Astronomy 105muon spec
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6.2 Neutrino Astronomy 107The setup
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6.3 Gamma Astronomy 109All parts of
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6.3 Gamma Astronomy 111The energy s
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6.3 Gamma Astronomy 1136.3.3 Measur
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6.3 Gamma Astronomy 115v = c n = 29
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6.3 Gamma Astronomy 117The relation
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6.3 Gamma Astronomy 119Future space
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6.3 Gamma Astronomy 121γ -ray burs
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6.4 X-Ray Astronomy 123bursters all
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6.4 X-Ray Astronomy 125synchrotron
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6.4 X-Ray Astronomy 127In 1952 Wolt
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6.4 X-Ray Astronomy 129In 1959 the
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6.4 X-Ray Astronomy 131Measurements
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6.5 Gravitational-Wave Astronomy 13
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6.5 Gravitational-Wave Astronomy 13
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6.6 Problems 1373. Radiation exposu
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6.6 Problems 139the star and its te
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1417 Secondary Cosmic Rays“There
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7.1 Propagation in the Atmosphere 1
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7.1 Propagation in the Atmosphere 1
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7.2 Cosmic Rays at Sea Level 1477.2
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7.2 Cosmic Rays at Sea Level 149muo
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7.3 Cosmic Rays Underground 151N(ν
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7.3 Cosmic Rays Underground 153[ a
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7.3 Cosmic Rays Underground 155Fig.
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7.4 Extensive Air Showers 157hadron
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7.4 Extensive Air Showers 159precis
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7.4 Extensive Air Showers 161primar
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7.5 Nature and Origin of the Highes
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7.6 Problems 169‘Milky Way’ of
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1718 Cosmology“As far as the laws
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8.1 The Hubble Expansion 173isotrop
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8.2 The Isotropic and Homogeneous U
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8.3 The Friedmann Equation from New
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8.4 The Friedmann Equation from Gen
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8.4 The Friedmann Equation from Gen
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8.7 Nature of Solutions to the Frie
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8.7 Nature of Solutions to the Frie
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8.8 Experimental Evidence for the V
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8.9 Problems 189where E max is the
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1919 The Early Universe“Who cares
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9.2 Thermodynamics of the Early Uni
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9.3 Solving the Friedmann Equation
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9.3 Solving the Friedmann Equation
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9.4 Thermal History of the First Te
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9.5 The Baryon Asymmetry of the Uni
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9.6 Problems 211investigation of CP
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21310 Big Bang Nucleosynthesis“In
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10.2 Start of the BBN Era 215these
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10.3 The Neutron-to-Proton Ratio 21
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10.4 Neutrino Decoupling, Positron
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10.5 Synthesis of Light Nuclei 221i
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10.6 Detailed BBN 223Fig. 10.4Evolu
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10.6 Detailed BBN 225prediction for
Page 482: 10.7 Constraints on the Number of N
Page 486: 22911 The Cosmic MicrowaveBackgroun
Page 490: 11.2 Discovery and Basic Properties
Page 494: 11.3 Formation of the CMB 23311.3 F
Page 498: 11.4 CMB Anisotropies 235Once the p
Page 502: 11.5 The Monopole and Dipole Terms
Page 506: 11.6 Determination of Cosmological
Page 518: 24512 Inflation“Inflation hasn’
Page 522: 12.2 The Flatness Problem 247Althou
Page 526: 12.3 The Monopole Problem 249place
Page 530: 12.4 How Inflation Works 251the pre
Page 536: 254 12 Inflationexcitation of this
Page 540: 256 12 InflationFig. 12.3Schematic
Page 544: 258 12 Inflationinflationary period
Page 548: 260 12 Inflationdilutionof magnetic
Page 552: 262 12 InflationFig. 12.4Measuremen
Page 556: 264 12 InflationΩ gravity waves =
Page 560: 266 13 Dark Matterearly universedev
Page 564: 268 13 Dark Mattermass density54321
Page 568: 270 13 Dark Matterbrown dwarvesFig.
Page 572: 272 13 Dark MatterNACHOsultracold g
Page 576: 274 13 Dark Matterneutrinosas free
Page 580: 276 13 Dark Mattersupersymmetric ex
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278 13 Dark MatterIt is not totally
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280 13 Dark Mattertrue vacuumcosmol
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282 13 Dark Matterpropertiesof non-
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284 13 Dark MatterquintessenceBoome
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286 13 Dark Matter3. Derive the Fer
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288 14 Astrobiologyage of life on E
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290 14 Astrobiologybeen the result
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29315 Outlook“My goal is simple.
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15 Outlook 295also the cosmological
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15.1 Problems 29715.1 Problems1. It
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300 16 GlossaryMeasurement of exten
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302 16 GlossaryAn asymmetry created
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304 16 GlossarySensitive resistance
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306 16 GlossaryA Friedmann-Lemaîtr
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308 16 GlossaryThe cosmological con
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310 16 GlossaryThe apparent change
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312 16 GlossaryFermi-Dirac distribu
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314 16 GlossaryExtragalactic gamma-
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316 16 GlossaryHawking radiationHaw
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318 16 GlossaryNuclei of fixed char
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320 16 GlossaryTotal light emission
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322 16 GlossaryMpcMSW effectMtheory
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324 16 GlossaryOA Friedmann-Lemaît
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326 16 GlossaryRotating neutron sta
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328 16 GlossaryThe number of neutra
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330 16 GlossaryOr cascade. High-ene
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332 16 GlossaryPhenomenon of appare
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334 16 Glossarytime-reversal invari
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336 16 GlossaryXX bosonXMM-NewtonX-
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338 17 Solutionsv 2 = r 2 ω 2 = G
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340 17 SolutionsWithµ = 1.67 × 10
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342 17 Solutionsor2m e (E e + + m e
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344 17 Solutions2. The relative ene
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346 17 Solutions17.5 Chapter 51. a)
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348 17 Solutions17.6 Chapter 6Sect.
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350 17 Solutionsc) With the numbers
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352 17 SolutionsSolid angle: Ω =A4
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354 17 SolutionsThe solution of thi
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356 17 SolutionsSect. 6.51. E = GMm
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358 17 SolutionsN 1 (> 2GeV) = a∫
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360 17 Solutions2E kin = 3kT M µ =
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362 17 Solutions7. An observer in e
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364 17 SolutionsWith the ansatzR =
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366 17 Solutions(Solve for v ∗ :
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368 17 Solutions17.11 Chapter 111.
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370 17 Solutionsb) At last scatteri
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372 17 Solutions4.( ) 2R 0 t0 3= ,R
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374 17 SolutionsThe axion mass does
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376 17 Solutions100 kg kgW 0 = = 50
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378 17 SolutionsThis results inM pl
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381A Mathematical AppendixA.1 Selec
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A.1 Selected Formulae 383∫e x dx
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A.2 Mathematics for Angular Variati
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A.2 Mathematics for Angular Variati
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389B Results from Statistical Physi
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B.1 Statistical Mechanics Review 39
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B.2 Number and Energy Densities 397
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B.3 Equations of State 399which rel
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401C Definition of Equatorialand Ga
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403D Important Constants for Astrop
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405References“References are like
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407Further Reading“Education is t
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Further Reading 409Ulf Borgeest, Ka
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Further Reading 411M. A. Bucher, D.
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414 Photo Credits{20} ESA/XMM-Newto
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416 Indexanisotropy, 85, 86- cosmic
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418 Index- of hydrogen, 94, 222, 22
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420 Index- parameters, 243- - deter
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422 Indexeffective number of degree
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424 IndexFeynman diagram, 26, 98, 2
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426 IndexHarrison-Zel’dovich spec
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428 IndexKoshiba, M., 13kpc, 318, s
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430 Index- standard, see StandardMo
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432 Index- primary, energy spectrum
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434 Indexplanet, extrasolar, 18plan
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436 Indexrange- relation, energy-,
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438 Index- dark, 269- double, see b
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440 Indexuncertainty- principle, se
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