Astroparticle Physics

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8.7 Nature of Solutions to the Friedmann Equation 185One can then define the critical density ϱ c byϱ c = 3H 2(8.33)8πGand express the energy density ϱ by giving the ratio Ω,Ω parameterΩ = ϱ ϱ c. (8.34)Using this with H = Ṙ/R, (8.32) becomesk = R 2 (Ω − 1)H 2 . (8.35)So, if Ω
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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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Page 350: 7.4 Extensive Air Showers 161primar
Page 354: 7.5 Nature and Origin of the Highes
Page 366: 7.6 Problems 169‘Milky Way’ of
Page 370: 1718 Cosmology“As far as the laws
Page 374: 8.1 The Hubble Expansion 173isotrop
Page 378: 8.2 The Isotropic and Homogeneous U
Page 382: 8.3 The Friedmann Equation from New
Page 386: 8.4 The Friedmann Equation from Gen
Page 390: 8.4 The Friedmann Equation from Gen
Page 394: 8.7 Nature of Solutions to the Frie
Page 400: 186 8 Cosmology8.8 Experimental Evi
Page 404: 188 8 Cosmology24Ω m,0 ,Ω Λ,00.2
Page 408: 190 8 CosmologyGM 2R > 3 2 kT M µ
Page 412: 192 9 The Early UniverseSchwarzschi
Page 416: 194 9 The Early Universe9.2.1 Energ
Page 420: 196 9 The Early Universeyears), it
Page 424: 198 9 The Early Universeg ∗ = 28
Page 428: 200 9 The Early Universewhich relat
Page 432: 202 9 The Early Universe9.3.1 Digre
Page 436: 204 9 The Early UniverseTable 9.2Th
Page 440: 206 9 The Early Universebaryogenesi
Page 444: 208 9 The Early Universenet baryon
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210 9 The Early Universebaryon-numb
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212 9 The Early Universeϱ = π 230
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214 10 Big Bang Nucleosynthesisbary
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216 10 Big Bang Nucleosynthesis10.3
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218 10 Big Bang NucleosynthesisIgno
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220 10 Big Bang Nucleosynthesisquic
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222 10 Big Bang Nucleosynthesisfine
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224 10 Big Bang Nucleosynthesisdeut
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226 10 Big Bang Nucleosynthesis10.7
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228 10 Big Bang Nucleosynthesishad
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230 11 The Cosmic Microwave Backgro
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246 12 Inflation12.1 The Horizon Pr
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248 12 InflationΩ at the Planck ti
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250 12 Inflationcausally isolated r
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252 12 InflationOne can now ask wha
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254 12 Inflationexcitation of this
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256 12 InflationFig. 12.3Schematic
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258 12 Inflationinflationary period
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260 12 Inflationdilutionof magnetic
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262 12 InflationFig. 12.4Measuremen
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264 12 InflationΩ gravity waves =
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266 13 Dark Matterearly universedev
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268 13 Dark Mattermass density54321
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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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