Astroparticle Physics

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12.2 The Flatness Problem 247Although this is now known to hold to within around 2%, ithas been clear for many years that Ω is at least constrainedto roughly 0.2
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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
Page 470: 10.5 Synthesis of Light Nuclei 221i
Page 474: 10.6 Detailed BBN 223Fig. 10.4Evolu
Page 478: 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 524: 248 12 InflationΩ at the Planck ti
Page 528: 250 12 Inflationcausally isolated r
Page 532: 252 12 InflationOne can now ask wha
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.
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272 13 Dark MatterNACHOsultracold g
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274 13 Dark Matterneutrinosas free
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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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