1. Double feature: Yuri Levin, Leiden 1. The theory of fast oscillations during magnetar giant flares 2. Measuring gravitational waves using Pulsar Timing Arrays

2. Part 1. NEUTRON STARS: core: n (superfluid) p (supercond.) e crust 20 km spin=0.01-716 Hz km B

3. Physics preliminaries: magnetic fields in non-resistive media B Field lines : 1. Are frozen into the medium 2. Possess tension and pressure ~B 2 Alfven waves!

4. Magnetars: ultra-magnetic neutron stars. B~10 15 Gauss Duncan & Thompson 92 Usov 94 Thompson et al 94-06 crust Slowly rotating, with X-ray emission powered by magnetic energy Some magnetars also release flares 3 Giant flares: 1979, 1998, 2004 Mazetz, Hurley, etc.

5. Discovery of Quasi-Periodic Oscillations (Israel et al 2005)

6. Strohmayer & Watts 06

7. Oscilations at several frequencies: 18, 30, 40, 90, 625, etc., Hz. Israel et al 05 Barat et al 83 Watts & Strohmayer 06 Strohmayer & Watts 06 Interpretation 0: torsional vibration of the neutron star crust (starquake!) Three caveats: Duncan, et al 98-06 18 Hz does not work QPOs highly intermittent Physics does not work Key issue: high B-field

8. L. 06, L. 07, MNRAS also Glampedakis et 06 1.Magnetically coupling to the core on 0.01-0.1 second timescale. Pure crustal modes don’t exist. 2.Alfven continuum in the core. Initial crustal modes decay in <second What happens then? Torsional vibration of the whole star crust Normal-mode analysis: global torsional mode most likely doesn’t exist

9. 1.Magnetically coupling to the core on 0.01-0.1 second timescale. Pure crustal modes don’t exist. 2.Alfven continuum in the core. Initial crustal displacements decay in <second What happens then? Crust-core dynamics: Normal-mode analysis: global torsional mode likely don’t exist Resonant absorption, cf. solar corona (Ionson 78, Hollweg 87, Steinolfson 85, etc…..) crust Resonant Layer

10. Initial-value problem: toy model, zero friction 10000 small oscillators, 0.01g 1 kg

11. Zoom in on the residual:

12. Energies of small oscillators Power spectrum: 2 Oscillations !!! But: edges of the continuum

13. Phases of small oscillators: Special Point!

14. Initial-value problem: inflected spectrum 10000 small oscillators, 0.01g 1 kg

15. The real magnetar (simulated)!

17. Dynamical spectrum (simulations)

19. Dynamical spectrum theory

20. Asteroseismology? Low-frequency QPOs (18Hz) probe Alfven speed in the core. For B=10 G, need to decouple 90% of the core material from the wave. Neutron superfluidity! 15

21. Conclusions: main features of Quasi-Periodic Oscillations 1.Steady QPOs---special points of the Alfven continuum, 2.Intermittent QPOs everywhere, but enhanced near crustal frequencies. 3.Qualitative agreement between theory and observations 4.Powerful probe of the Alfven speed in the interior of magnetars 5. Open issue: magnetosphere

22. Part 2 Measuring gravitational waves using Pulsar Timing Arrays.

23. Galaxy formation: Universe becomes matter-dominated at z=10000. Gravitational instability becomes effective. Small halos collapse first, small galaxies form first Smaler galaxies merge to form large spirals and ellipticals. White & Rees 78

24. Snijders & van der Werf 06 Komossa et al 02 (Chandra) Merging Galaxies Merging SBHs?

25. Evidence for mergers? Milosavljevic & Merritt 01 Graham 04 Mass deficit at the center But: simulations do not agree with observations: McDermitt et al. 06 (Sauron)

26. Q: What to do? A: Measure gravitational waves!

27. LISA: the ESA/NASA space mission to detect gravitational waves. Binary black hole mergers Out to z=3 is one of the main targets Launch date 1915+..

28. Detection Amplitude for SBH mergers at z=1. Unprecedented test of GR as dynamical theory of spacetime!

29. Measuring gravitational-wave background with a Pulsar Timing Array. millisecond pulsar Earth arrival on Earth departure from pulsar gravitational wave frequency shift

30. Millisecond pulsars: Excellent clocks. Current precision 1 microsecond, projected precision ~100-200 ns. Intrinsic noise unknown and uncorrelated. GW noise uknown but correlated. Thus need to look for correlations between different pulsars. Many systematic effects with correlations: local noisy clocks, ephemeris errors, etc. However, GW signature is unique! 2 Pulsar Timing Arrays: Australia (20 pulsars) Manchester Europe (~20) Kramer+ Stappers

31. John Rowe animation/ATNF, CSIRO

32. Contributions to timing residuals: Gravitational waves!! Pulsar timing noises Quadratic spindowns Variations in the ISM Clock noises Earth ephemeris errors Changes of equipment Human errors Optimistic esimate: ~5000 timing residuals from all pulsars. Our work so far

33. Gravitational waves (theory): Phinney 01 Jaffe & Backer 03 Wyithe & Loeb 03 S(f)=A f -p

34. Current algorithm = const·[6x log(x)-x+2], x=cos(ab) Jenet et al. 05 ab pulsar a pulsar b GW Look for correlation of this form! But: statistical significance? Parameter extraction?

35. Leiden+CITA effort: Gravitational-Wave signal extraction van Haasteren, L., McDonald (CITA), Lu (CITA), soon tbs Bayesian approach: Parametrize simultaneously GW background and pulsar noises (42 parameters) Parametrize quadratic spindowns (60 parameters) derive P(parameters|data), where data=5000 timing residuals marginalize numerically over pulsar noises and analytically over the spindowns

36. Advantages No loss of information-optimal detection Measures the amplitude AND the slope of GWB Natural treatment of known systematic errors Allows unevenly sampled data

37. Markov Chain simulation: Pulsar noises 100 ns.

39. Conclusions part 2: SBH binaries predicted but not yet observed Gravitational-wave detection by LISA and Pulsar-Timing Arrays is likely within 1-1.5 decade.

40. accretion ashes H+He ashes X-ray flux time 1 sec THERMONUCLEAR BOMB ! He Type-I x-ray bursts. Spitkovsky, L., Ushomirsky 02 Spitkovsky & L., in prep Amsterdam, SRON, NASA, MIT,..

42. Analogy to hurricanes

43. deflagration front heat fuel FLAMES heat propagation reaction speed speed of the flame rise time of the burst Heat propagation: 1. microscopic conduction: too slow, 10 m/sec 2. turbulence from buoyant convection (Fryxell, Woosley): highly uncertain; only upper limit works probably irrelevant! Niemayer 2000

44. HEAT PROPAGATION hot cold 30m 3m 3 km Rossby radius Kelvin-Helmholtz stable!! Baroclinic: unstable but weak. Heat conduction a la Niemeier, but across a huge interface!

45. ROSSBY RADIUS Scale where potential = kinetic energy Rossby radius a R is a typical size of synoptic motions on Earth: ~1000 km, on NS ~ 1km

46. TWO - LAYER SHALLOW-WATER MODEL 22 h 2 (x) 11 h 1 (x) Q(T) Heat Q(T): Temperature -- height: Two sets of coupled shallow-water equations in 1 1/2 D. Include mass and momentum transport across layers and interlayer friction

48. Burst QPOs from ocean Rossby waves? + QPO coherence, + QPOs in the tail - Typically, waves go too fast. - Not clear how to excite them. - What happens during the burst rise (i.e., spreading hot spot)? Heyl 2004, Lee 2005, Piro & Bildsten 2005, Narayan & Cooper 2007

49. Conclusions: 1.Good prospects to understand magnetar QPOs and to learn about neutron-star interior 2. Good prospects to understand type-I burst deflagration, but QPO behaviour, etc., very difficult to understand

50. Precession of radio pulsars. Theory: radio pulsars cannot precess slowly pinned superfluid vortices Fast precession: 1/100 of NS spin Observations: Shaham 1977 Spin period 0.5 seconds Precession period 500 days Pulsar PSR B1828 Shaham’s nightmare!! Stairs et al 2000 No strong pinning in the crust? Link & Cutler 03 Jones 98

51. What about the core? Earth: Chandler wobble Crust precesses Core doesn’t L. & D’Angelo 04 Neutron star: B enforces co-precession between the crust and core plasma n-superfluid does not participate in precession: MUTUAL FRICTION damps precession!

52. Mutual friction in neutron stars n, p supercurrent: entrainment of p in n Magnetization of n-superfluid vortex B Superconductivity: Type II: Precession excluded! Link 03;-important result Type I: Precession damped in 10-100 yr p n B Sauls & Alpar 88 L. & D’Angelo 04 Probe of strong n-p forces! e

53. Spitkovsky

54. Formation of a neutron star: Burrows, Livne, et al. 2006