1. Neutrino Ocillations and Astroparticle Physics (3)
John Carr
Centre de Physique des Particules de Marseille (IN2P3/CNRS)
Pisa, 8 May 2002
 Introduction to Cosmology and High Energy Astronomy
- expansion of the universe
- some astronomy
- some cosmology
- big bang nucleosynthesis
- cosmic microwave background radiation
- SuperNova Type 1a
- Energy composition of universe

2. Expansion of Universe v= H r H ~ 70 km/sec / Mpc Velocity of galaxy
Edwin Hubble
Mt. Wilson
100 Inch
Telescope
Velocity of galaxy
proportional to distance:
v= H r
H ~ 70 km/sec / Mpc

3. Astronomy Scales 1 pc = 3 light years = 3 1016 km Nearest Stars
Nearest Galaxies
Nearest Galaxy Clusters
4.5 pc
450 kpc
150 Mpc

4. Galaxies Spiral (Milky Way) Solar Mass: M = 2 1033g
1kpc
1kpc
~ 10% mass
Solar Mass: M = g
Typical stars mass 1-10 M
Typical Galaxies M
100kpc

5. Milky Way Galaxy
Magnetic field
 few G

6. Cosmic Accelerators: Hillas Plot
Crab Pulsar
E  Z B L  B
Z: Charge of particle
B: Magnetic field
L: Size of object
: Lorentz factor
of shock wave
M87, AGN
Centurus A
GRB (artist)
3C47
Vela SNR L

7. Active Galactic Nuclei
Radio Images
Visible light

8. QUASARS & MICROQUASARS
QUASAR MICROQUASAR
QUASAR MICROQUASAR
Central black hole
M M
distant galaxies local galaxy

9. QUASARS & MICROQUASARS

10. Gamma-Ray Burst Story
Gamma Ray Burst were first detected by the Vela satellites that were developed in the sixties to monitor nuclear test ban treaties.
1st GRB

11. Gamma Ray Bursts : present knowledge
~1-2 / day, duration 10ms - 100s,
isotropic distribution in sky,
at extra galactic distances.
Count rate in unit of 1000 counts s-1
Now evidence
of GRB association
with supernova
sec
ANTARES will dump all data in  100 secs of gamma ray burst warning signal

12. Multi-Messengers to see Whole Universe
Distant universe
invisible in
high energy photons
need neutrinos
Quasar
formation
period

13. Evolution of the Universe
Consider a particle on surface of sphere which expands with universe:
r : radius of sphere
Mass inside sphere is: (4/3) r3 
Potential energy of particle: -(4/3)r3  G/r
Kinetic energy: r2/2
so total energy: r2/2 -(4/3)r3  G/r = E
 : mass density in universe . .
Sphere evolves with time, write r(t) = a(t) x
remember H = v/r = a/a .
Then get Freidmann equation: H2 = (8/3) G  - K/a2
where K = -2E
Evolution of universe depends on value of K
if K < 0, energy E > 0 expansion continues for ever
if K > 0, energy E < 0 eventually universe contracts
K = 0 critical value

14. Matter Density and Curvature of the Universe
Freidmann eqn: H2 = (8/3) G  - K/a2
With K = 0
Freidmann equation: H2 = (8/3) G 
define critical density: c = (3/8)H2/G
define density fraction:  =  / c
Same K comes into the spatial line element in General Relativity:
If K = 0, geometry is Euclidean - flat, if K = 0, geometry curved
equivalently if  = 0 universe is flat
 > 0 curvature positive, universe is closed
 < 0 curvature negative, universe is open

15. Cosmological Constant
Einstein did not know about the expansion of the universe and
add a ad-hoc term to make universe static
Freidmann equation becomes:
H2 = (8/3) G  - K/a2 +  /3
where  is cosmological constant
Theory no longer needs it, but experiment seems to indicate its presence
Conventional to treat it as another contribution to the density fraction
(t) =  matter(t) + 
 =  matter 

16. Future of Universe

17. Origin of Elements formed in: Big Bang Nucleo-synthesis Hot Stars
Supernova Explosions
Cosmic Ray Interactions

18. Big Bang T (K) ~ 1010/t½ (s) temperature of universe 1010 K 3000 K
Equilibrium n/p ends
Nucleosynthesis begins
1010 K
Neutral hydrogen forms
universe transparent to light
fossil photon radiation frozen
temperature of universe
3000 K
nuclei
atoms
100 s
3 105 y
time after big bang

19. Particle Physics after Big Bang
time since Big Bang

20. First Minute after Big Bang
Production rates = Annihilation rates
 equilibrium of particles and no nuclei formed
N (neutron)
N (proton)
= e m/kT
(m = 1.3 MeV)
In equilibrium:
When temperature falls below 1010 K (1 MeV) reactions cease

21. Nucleosynthesis starts
Deuterium necessary to start nucleosynthesis
Helium formed from deuterium
( Difficult to continue because no stable mass 5, 8 nuclei)

22. Nucleosynthesis development
helium-4
deuterium
helium-3
tritium
(free neutrons decay)
Be, Li low levels

23. Element Production in Stars
PP cycle : cold stars
CNO cycle : hot stars

24. Heavy Element Production in Supernova
CNO cycle : hot stars
rp process : supernova explosions
rp process
protons
stable nuclei
neutrons
Nuclear cross-sections not well known: need accelerator measurements

25. Nucleosynthesis rate gives baryon density
Measured abundance of He, D
 Fraction of baryons < 5%
Must have
non-baryonic particle dark matter
 = Nb/N , baryon number fraction

26. End of Opaque Universe
After recombination universe becomes transparent.
See photons as Cosmic Microwave Background Radiation redshifted by 1000 to 2.7K

27. Penzas and Wilson Discovery of Cosmic Microwave Background

28. Cosmic Microwave Background Radiation

29. Cosmic Microwave Background Radiation
temperature variation
-30
-35
-40
-45
-50
-55
-60
 (degrees)
 (degrees)
Analyse angular distribution to see typical variation scale

30. Measure Scale of CMBR Fluctuations

31. CMBR Data Analysis location of first peak: Wtotal ~ 1
amplitude of other peaks sensitive to Wbaryon

32. Supernova Type 1a
Implosion
of core of
red giant
Expansion of matter
shock wave  0.5 c
Explosion of star
Supernova
Supernova Remnant
SNIa occurs at Chandrasekar mass, 1.4 Msun  ‘Standard Candle’
measure brightness  distance: B = L / 4pd2
measure host galaxy redshift  get recession velocity
test Hubble’s Law: v = H d, at large distances

33. SuperNovae observed in our galaxy
Date Remnant Observed
352 BC Chinese
185 AD SNR Chinese
369 ? Chinese
Chinese
SNR Chinese
437 ?
827 ?
902 ?
SN Arabic, ...
Crab Chinese,..
C Chinese,..
1203 ?
1230 ?
Tycho Tycho Brahe
Kepler Johannes Kepler
Cas A not seen ?

34. SuperNovae Remnants Crab Vela Kepler Tycho Cas A Cygnus Crab Tycho
Soleil
Vela
Cas A
Cygnus Loop
Kepler
SN1006
Tycho
Cas A
SN1006
SN1054 (Crab)
SN1680 (CasA)
Cygnus
SN1006

35. Supernova in Large Magellenic Cloud

36. Distant Supernova

37. Life of big star ( > 1,4 M)
End in Supernovae of type Ib, Ic et II

39. Life of big star ( < 1,4 M)

40. La nébuleuse de la Lyre

41. Type Ia supernovae
SNe Ia sont which accrete matter from neighbour star in binary system When the mass achieves the Chandrasekhar mass (~1.4 M) star collapses to neutron star in supernova explosion.
Red Giant
Flow of
matter
White Dwarf
 Always same mass so always same luminosity
Standard Candle for measuring universe expansion

42. Reference
Image
Subtraction

43. Expansion with Supernova Ia
Acceleration of
universe expansion
effective magnitude  brightness  distance
non-linear v = H(t) d
redshift  recession velocity

45. In 1998, two teams: High-Z Supernovae and Supernovae Cosmology Project simultaneously annouce non-zero cosmological constant:
WL = 0,72 ± 0,23
WM = 0,28 ± 0,09

46. So what does it mean?
( due to E. Copeland, a theorist)

47. Supernova at z1.7

48. Future Project: SNAP  2500 SNe Ia per year with z < 1.7
Study Equation of state w=pw/w - -

49. Understanding Nature of Dark Energy

50. Evidence for Matter Density Combined Data
Cosmic Microwave Background Radiation, Supernova 1a, Galaxy clusters and BBN
tot = total  critical
critical density
for flat universe
critical= 3H2/8GN
H = h km/s/Mpc
M = matter  critical

51. Matter/Energy in the Universe
Wtotal = WM + WL 1
matter dark energy
Matter:
WM = Wb + W + WCDM  0.4
baryons neutrinos cold dark matter
Baryonic matter :
Wb ~ 0.05
stars, gas, brown dwarfs, white dwarfs
Neutrinos:
W ~ 0.003
if M(n) ~ 0.1 eV as from oscillations
Cold Dark Matter :
WCDM  0.3
WIMPS/neutralinos, axions