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New Problems for a New Century

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

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New Problems for a New Century

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

  2. X-rays in the 20th CenturyFinal 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? Tsuboi • 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 LEdd , <10-5 Lbondi • Cluster magnetic fields Linsky Mukai Kubota Mineshige Mushotzky Brandt

  5. Q2. How do cosmic plasmas really behave? Tanaka • 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 Linsky Kahn Inoue Iwasawa Brandt, Boller Nandra,Zdziarski Reeves,Yaqoob

  6. Q3. What is the structure of collisionless shocks? Linsky Petre Aschenbach Kamae • 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 ~ 106-7 K • GRBs • Sgr A East? Bautz Arnaud Ricker Nousek Fiore Koyama

  7. Q4. When and how were the elements made? Iyudin Petre Aschenbach • 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? Nomoto Fiore Fabbiano Iwasawa Ohashi Bohringer

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

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

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

  11. Q8. How did the universe expand? • New standard model • Flat universe • H0 ~ 60-70 • W0 ~ 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? Matsumoto • Intermediate black holes • Pop III stars • Could be W ~ 10-6 • X-ray binaries in Elliptical Globular Clusters • Fossils? • Quasars • AGN before or after galaxies? • Super - critical accretion? • Impact on Ionisation Mushotzky Swank Brandt Hasinger Barcons

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

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