1. APP Introduction to Astro-Particle Physics
Maarten de Jong

2. What is APP? Cosmology Particle physics Astrophysics
This course will have a particle physics approach.

3. Chapter 1 Chapter 2, 3, 6 Chapter 11 Chapter 12, 13, 14 Chapter 15
Free download of this book available at publisher.
Chapter 1
Chapter 2, 3, 6
Chapter 11
Chapter 12, 13, 14
Chapter 15

4. useful coordinates http://www.nikhef.nl E-mail
URL

5. What is (cosmic) matter made of?

6. !

7. q n p q beam of particles scattering off target protons
Mass spectrum of hadrons
point like particles
number of events
extended charge
distribution q

8. quark-parton model ↓ standard model of particles and fields
1960’s → today
quark-parton model ↓
standard model of particles and fields

9. particles q e m t –1 ne nm nt 0 u c t +⅔ d s b –⅓ particle flavour
leptons
quarks

10. fermions
spin ½ particle

11. interactions interaction mediator spin/parity strong gluon (g) 1– E-M
photon (g)
weak
W±, Z0
1–, 1+
gravity
graviton? 2+

12. bosons
spin 1, 2, … particle

13. mediator of E-M interaction mass-less ‘particle’
photon
mediator of E-M interaction
mass-less ‘particle’

14. photon astronomy Crab nebula broadband feature1’
radio eV optical eV X-rays eV gamma rays 1012 eV
broadband feature

15. Planck constant
speed of light
Wavelength:
Energy of ‘particle’

16. Mass of elementary particles?

17. quarks leptons bosons Z t b W t c s m nt d u e nm Mass [eV/c2] ne
atmospheric n oscillations
mg < eV
solar n oscillations

18. origin of mass?
Higgs search
discovery

19. interactions (II) strong E-M weak gravity 1 10-2 10-7 10-39 nucleus
atom ?
planets stars

20. conservation rules energy-momentum charge lepton number (e,m,t)
baryon (qqq) number …

21. Radio-active decay
2-body decay?

22. Radio-active decay (II)
observed energy spectrum
of e±
Number of events
Energy not conserved?

23. Postulate of an invisible particle
Zürich, Dec. 1930
Dear radioactive ladies and gentlemen,
I may have found a solution to the energy crisis in radioactive decays.
… the existence of electrically neutral particles
–which I call neutrons– in the atomic nucleus.
The measured spectrum can be understood if
such a neutral particle escapes together with the
electron such that the total energy is conserved.
I admit that this idea is unlikely because the
neutrons –if they exist– would have been found
already.
W. Pauli

24. Fermi: Weak interaction
Pauli (1930):
not detected
Fermi: Weak interaction e W– d u d d u u n p
Feynman diagram

25. Fundamental forces
Energy

26. Atomic Mass Unit
Energy ratio:

27. Chemical energy
1.5 Volt
E-M interaction: a = 1/137

28. Nuclear energy
Strong interaction: as ≈ 1

29. Gravitational energy
A = 4pr2 r dr
4p r r2dr

30. Stellar implosion
Å = m p e- n
fm = m

31. Stellar implosion (II)
Gravitational force is accumulative: ?
¶ Weak field approximation!

32. Energy barrier

33. Solar luminosity
Luminosity
Age
chemical

34. hydrogen burning
detected!

35. Solar luminosity (II)
Luminosity
Age
nuclear

36. Milky Way
Luminosity
Age
observed
He has cosmological origin