1. 130 ix 05ICFA High Energy Astro-Particle Physics International Conference on Future Accelerators Daegu, Korea Roger D. Blandford KIPAC Stanford University

2. 230 ix 05ICFA The Scope of Astro-Particle Physics *Cosmology –Physics of the Early Universe, inflation, baryo/leptogenesis… –Dark Matter/Dark Energy *Physics of Extreme Environments –Neutron Stars - Pulsars, Magnetars… –Black Holes - Quasars, Gamma-ray Bursts… *High Energy Particles –Cosmic Rays - UHE Protons, VHE Gamma rays, UHE ’s… –Cosmic Accelerators - Shock Fronts, Electromagnetic Inductors…

3. 330 ix 05ICFA The Scope of Astro-Particle Physics *Cosmology –Physics of the Early Universe, inflation, baryo/leptogenesis… –Dark Matter/Dark Energy *Physics of Extreme Environments –Neutron Stars - Pulsars, Magnetars… –Black Holes - Quasars, Gamma-ray Bursts… *High Energy Particles –Cosmic Rays - UHE Protons, VHE Gamma rays, UHE ’s… –Cosmic Accelerators - Shock Fronts, Electromagnetic Inductors…

4. 430 ix 05ICFA General Relativity *General Relativity (Einstein 1915) –Singular “simple” theory of classical gravity –G=8  T –Many, more elaborate alternatives Scalar tensor, bimetric, extra dimensions, PPN… *Experimental Program –Classical tests Redshift, Mercury. Light deflection –Modern tests Shapiro delay, gravitational radiation, EP, inverse square law... GR/AE vindicated at level from 10 -2 to 10 -4 !

5. 530 ix 05ICFA Cosmology *Einstein 1916 –G+  g=8  T - Cosmological Constant Vacuum energy: P=-  *Friedmann 1922 a(t) is scale factor ( =1 now) B Const. measures curvature =0 when flat.

6. 630 ix 05ICFA Historically,  was taken very seriously *Lemaitre 1927 –Basic equations, relativistic growth of perturbations *Eddington 1933 –The universe is much bigger than particles; therefore there must a cosmological lengthscale -  -1/2 –“I would as soon think of reverting to Newtonian theory as of dropping the cosmical constant” –“To drop the cosmical constant would knock the bottom out of space” *Bondi 1948 –  CDM Universe

7. 730 ix 05ICFA Simple World Models  only – r const – a ~ exp t – De Sitter Universe *Matter only –  ~ a -3 –a ~ t 2/3 –Einstein - De Sitter Universe –Deceleration *Matter plus  –Singular “simple” theory –a ~ (sinh t) 2/3 –  CDM universe –Deceleration -> acceleration t

8. 830 ix 05ICFA Cosmological Observations *Kinematical –Cannot measure time accurately –Instead measure d(a), where –Observe objects of known size eg density fluctuations –at recombination when a ~ 10 -3

9. 930 ix 05ICFA Microwave Background Observations Hinshaw et al WMAP *Measure spectrum of temperature fluctuations –Derive from scale-invariant initial conditions => inflation? *Calculate linear size of peak; angle => distance Universe Flat to ~ 2 percent

10. 1030 ix 05ICFA Cosmological Observations *Kinematical –Cannot measure time accurately –Instead measure d(a), where –Observe objects of known size eg density fluctuations –at recombination when a ~ 10 -3 –Observe objects of known power eg supernovae –For a > 0.3 Perlmutter

11. 1130 ix 05ICFA Cosmological Observations *Dynamical –Newtonian physics in Universe expanding at rate given by a(t) –Measure CMB fluctuation spectrum –Clusters of galaxies –Growth of structure Compare with CMB X-rays +Lensing Nuclear Physics Tegmark et al

12. 1230 ix 05ICFA  CDM Dynamics *Positive perturbations grow –Gravity vs expansion –Initial conditions when a~0.001 from CMB observations –Fluctuation spectrum has “simple,” scale-free form Linear perturbations evolve with time according to: –Extend into nonlinear phase using simulations –many uncertainties on short scales

13. 1330 ix 05ICFA Standard Model of the Universe *   = const =0.7nJm -3 =6 x 10 -28 kg m -3  Equivalent to: 0.4 mG, 40 K, 1meV, 100 , 3THz m  ~m SUSY 2 /m P Extra dimensions… *  DM = 0.25nJm -3 Supersymmetric particle? *   = 0.05nJm -3 *Flat spatial geometry All contemporary data consistent with  CDM to 10-20%

14. 1430 ix 05ICFA How do we study DE/DM at 1% level? *What physics must we explain? *CMB observations will improve *Kinematic Tests –Distance to supernovae –Baryon oscillations –… *Dynamical Tests –Weak gravitational lensing –Counting clusters of galaxies –… *Only careful, well-planned projects will be up to the task Eisenstein et al In US, a task force is making choices

15. 1530 ix 05ICFA Extreme Conditions *SGR 1806-20 Magnetar Explosion Dec 27 2004 *Highly Magnetized Neutron Star in our Galaxy *Released large fraction of magnetic energy in electromagnetic bomb –M ` 3 x 10 30 kg: R ~ 10km; giant nucleus –B ~ 10 11 T, E~10 41 J ~30 B QED, 15MeV cyclotron energy –E ~ 10 40 J in ~ 1s –Afterglow in radio and X-rays –Still fading 300  s risetime

16. 1630 ix 05ICFA Extreme Physics *Cold nuclear matter at several times nuclear density –Many body effects dominant –Composition still unknown Neutrons, hyperons, quarks, strange stars… Superconductivity, superfluidity –M(R), cooling etc *QED in supercritical fields –Novel, though uncontroversial effects –Largely unexplored Plenty of new effects! *Ultrarelativistic shock waves, pair plasma physics –Accelerators increasingly used to perform HED experiments

17. 1730 ix 05ICFA Cosmic Particle Acceleration *Naturally occuring accelerators produce UHE CR: –E ~ ZeV = 10 12 GeV –E CM ~ PeV; Higher energy collisions on our past light cone –I ~ 1 EA = 10 18 A *How do they work? Shock Fronts Black Holes Jets Chandra X-ray Observatory

18. 1830 ix 05ICFA TeV  -ray Astronomy *H.E.S.S. (VERITAS) *Atmospheric Cerenkov emission in stereo *Particle physics techniques *Observe up to 30 TeV *Combine with GLAST in 2007 *How are GCR accelerated *Test Lorentz Invariance on cosmological scale ASCA 1-3 keV > 1 TeV

19. 1930 ix 05ICFA Summary *Astro-Particle Physics remains a very exciting area *Fundamental problems –Dark Energy - astronomical observation plus pure thought –Dark Matter – below, on and above ground –Inflation - CMB polarization *Outstanding astro-engineering puzzles –How do shocks and Zevatrons work? –What causes magnetars and gamma ray bursts to explode? –What is a neutron star? *Tremendous discovery potential for new physics –Baryogenesis and leptogenesis –Black hole observations as tests of strong field gravitation –Strong field QED