1. New Problems for a New Century Yokohama March 6-8 2001 By Dr. Roger Blandford

2. X-rays in the 20 th Century Final Exam Time allowed: one decade Students are allowed and encouraged to collaborate; However, you must write up your own answers Calculators may be used You may find it useful to consult observations in other parts of the electromagnetic spectrum You should attempt all the questions NO CHEATING

3. Answer all Questions 1. How do cosmic magnetic fields really behave? 2. How do cosmic plasmas really behave? 3. What is the structure of collisionless shocks? 4. When and how were the elements made? 5. How does matter behave at high density? 6. Is general relativity correct? 7. What is the nature of dark matter? 8. How did the universe expand? 9. What were the first structures in the universe? 10. How do you do X-ray astronomy from the ground?

4. Q1.How do cosmic magnetic fields really behave? MHD ("go with the flow"; "push-pull") – Protostars – Brown Dwarfs – A stars – O stars – Magnetic CVs – Disk torque and dissipation – Disk Hole interaction - Jets – Disk Flows – Outflows from compact objects " <10 -8 L Edd, <10 -5 L bondi – Cluster magnetic fields Tsuboi Linsky Mukai Mushotzky Kubota Mineshige Brandt

5. Q2. How do cosmic plasmas really behave? Galactic ridge emission Seen in bulge 3 cmpt, reconnection collective e-i equilibration also SNRs, ADAFs Stellar Coronae Accretion Disk Coronae XRB spectra AGN spectra Fe K reverberation Warm absorbers Tanaka Kahn Inoue Iwasawa Brandt, Boller Nandra,Zdziarski Reeves,Yaqoob Linsky

6. Q3. What is the structure of collisionless shocks? Where are the O star wind shocks? Where are SNR shocks? Cas A shocks Particles accelerated at shock fronts, B where? 1-100 TeV electrons? Protons Where are the cluster shocks IGM T ~ 10 6-7 K GRBs Sgr A East? Linsky Petre Aschenbach Kamae Koyama Bautz Arnaud Ricker Nousek Fiore

7. Q4. When and how were the elements made? SNR abundances Mass cut -M(NS) Off center He explosion? Mg not O, S not with S - explosion models Gamma rays Hypernovae Mass loss in progenitor wind GRBs Origin of r-process? Galaxies [Fe/H ] ~ 5 Clusters homogeneous? Iyudin Petre Aschenbach Fiore Nomoto Fabbiano Iwasawa Ohashi Bohringer

8. Q5. How does matter behave at high density? Neutron star EoS cf Heavy Ion Collider Need g,  Cooling T(t) - nonthermal contribution? Magnetars (AXP) Test QED above critical field High radiation density physics GRBs cf Early Universe Tsuruta Weisskopf

9. Q6. Is general relativity correct? Test Kerr metric 50 masses measured spins Lense-Thirring Precession Bardeen-Petterson effect Cosmology 2nd/resumed inflation or new dynamics Yaqoob

10. Q7. What is the Nature of Dark Matter? Clusters Potentials Reconciled with lenses X-ray fundamental plane Double beta models SZ Groups Ellipticals monolithic collapse or mergers Decays? Bautz, Boehringer Ohashi Arnaud Mitsuda Kawai Tanaka

11. Q8. How did the universe expand? New standard model Flat universe H 0 ~ 60-70  0 ~ 0.3 frequency, luminosity function, substructure a(t) High z clusters Need standard candles, rods, beans Clusters SZ? Boehringer Henry Mitsuda Udomprasert

12. Q9. What were the first structures in the universe? Intermediate black holes Pop III stars Could be  ~ 10 -6 X-ray binaries in Elliptical Globular Clusters Fossils? Quasars AGN before or after galaxies? Super - critical accretion? Impact on Ionisation Matsumoto Mushotzky Swank Brandt Hasinger Barcons

13. Q.10 How do you do X-ray astronomy from the ground? Instrument / mirror development " Interferometry " Polarimetry (including circular) " High Energy Density Experiments " Numerical Simulation – MHD – Galaxy Formation " Laboratory Astrophysics Strueder Cash Takahashi Kunieda White Turner Elvis Porter Stahle