Introduction to Cosmology

Big Bang Nucleosynthesis 141

end of

inflation

(^2520)
electroweak
symmetry breaking
quark hardon
transition
nucleosynthesis matter radiation
equality
e± annihilation recombination
15 10 5 0.4
temperature – log K
energy – log eV 20

• 25
  
  
  • 30
  
  
  
  

10000

10000

0.01

matter radiation

equality recombination

start of

structure

reionization oldest

quasar

oldest

galaxies

acceleration

begins

0.1 13700

2.725

1000

10

1000

1000

100

100

10 100

10 1 0.1

redshift – z

time – Myr

temperature – K

density – log kg m^3

• 20 – 10

– 14 – 16 – 18 – 20 – 22 – (^24) – 26
10 17.6

• 20

15 10 5 0

• 15 – 10 – 5
  
  
  • 3.6
  
  
  
  

0

0

scale – log a

time – log s

Figure6.5The ’complete’historyof the Universe.The scalesabovethe dashedline coverthe time fromthe end of inflationto the present,
thosebelowfromthe end of radiationdominanceto the present.Inputconstants(not completelyupdated):퐻 0 = 0 .71 kms−^1 Mpc−^1 ,훺휆= 0 .73,
푇 0 = 2 .275 K,푡 0 = 13 .7Gyr,and푔∗,푔∗푆fromFigure6.2.