New Problems for a New Century

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

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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
• lt10-8 LEdd , lt10-5 Lbondi
• Cluster magnetic fields

Tsuboi
Linsky
Mukai
Kubota Mineshige
Mushotzky
Brandt
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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
Linsky
Kahn Inoue Iwasawa
Brandt, Boller Nandra,Zdziarski Reeves,Yaqoob
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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 106-7 K
• GRBs
• Sgr A East?

Linsky Petre Aschenbach Kamae
Bautz Arnaud
Ricker Nousek Fiore
Koyama
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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
Nomoto
Fiore
Fabbiano Iwasawa
Ohashi
Bohringer
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Q5. How does matter behave at high density?

• 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

Tsuruta Weisskopf
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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
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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
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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
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Q9. What were the first structures in the
universe?

• 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

Matsumoto
Mushotzky Swank
Brandt Hasinger Barcons
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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