New Problems for a New Century

Yokohama March 6-8 2001

By Dr. Roger Blandford

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

Answer all Questions1. 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?

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 LEdd , <10-5 Lbondi

Cluster magnetic fields

Tsuboi

Linsky

Mukai

Mushotzky

KubotaMineshige

Brandt

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

KahnInoueIwasawa

Brandt, BollerNandra,ZdziarskiReeves,Yaqoob

Linsky

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

PetreAschenbachKamae

Koyama

BautzArnaud

RickerNousekFiore

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?

IyudinPetreAschenbach

Fiore

Nomoto

FabbianoIwasawaOhashiBohringer

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

TsurutaWeisskopf

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

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,BoehringerOhashiArnaudMitsuda

KawaiTanaka

Q8. How did the universe expand? New standard model

Flat universe

H0 ~ 60-70

0 ~ 0.3 frequency, luminosity function, substructure

a(t) High z clusters

Need standard candles, rods, beans Clusters SZ?

BoehringerHenryMitsuda

Udomprasert

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

MushotzkySwank

BrandtHasingerBarcons

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

StruederCashTakahashiKuniedaWhiteTurnerElvisPorterStahle