1. “GRAND UNIFICATION” in Neutron Stars Victoria Kaspi McGill University Montreal, Canada

2. Census of Non-Accretion Neutron Stars

3. Why the Diversity? Neutron stars close cousins of black holes Gravitational redshifts of ~0.3 WHY SO MUCH HAIR??? Wide variety of behaviours is totally unpredicted What could matter? – Mass – Magnetic field – Initial spin – Geometry – Composition? – Evolutionary history? John Wheeler: 1967(?) Surprised neutron stars Come with “bell and whistle”

4. In This Talk Focus on finding commonalities among the various types of objects Hopefully infer physical mechanisms behind observed behaviour Ultimately constrain fundamental physics – Behaviour of matter at high density, low temperature – Behaviour of matter in highest magnetic fields known in Universe

5. Radio Pulsars (aka Rotation-Powered Pulsars) Born hot in supernova explosions; cool slowly, thermal X-rays Non-thermal (and some thermal) emission powered by rotation, via magnetic braking Infer B from P, Pdot Relativistic particle winds that produce spectacular nebulae, all rotation- powered

6. P-Pdot Diagram Radio Pulsars: Stable Emission

7. Magnetars: AXPs and SGRs “Bad Boys”: young, volatile Spectacular X-ray/g-ray bursts Unusual glitches X-ray pulsations Lx >> spin-down luminosity Many arguments for power via enormous B field, as inferred from spin-down

8. P-Pdot Diagram SGRs, AXPs Radio Pulsars High-B Radio Pulsars

9. High-B Radio Pulsars: “Anomalous” X-rays? NameP (s)PdotB (G)D (kpc) J1119-6127 0.44.1e-124.1e138.4 J1718-3718 3.41.6e-127.4e134.9 J1734-3333 1.22.3e-125.2e137.4 J1814-1744 4.07.4e-135.5e139.8 J1819-1458 4.35.7e-135.0e133.6 J1846-0258 0.37.1e-124.8e136 J1847-0130 6.71.3e-129.3e138.4 (RRAT)

10. PSR J1846-0258 0.3 s pulsar in SNR Kes 75 B = 5e13 G Youngest known: 884 yr Bona fide rotation-powered: – Lx << Edot – Power-law X-ray spectrum – Pulsar wind nebula – Normal timing properties, including n=2.65 (Livingstone et al. 2006) No radio emission (Archibald et al. 2008 )

11. Magnetar-like Behavior in a Rotation-Powered Pulsar Gavriil et al., Science, 2008 20062000

12. Chandra Observations of Kes 75 200020062009 Ng, Gavriil, VK, et al, in prep.

13. Timing Anomaly in PSR J1846-0258 Pulsar had spin-up glitch (df/f~4e-6) followed by strong spin-down Net effect: large spin-down df/f = 5e-5 Similar to that in SGR (Thompson et al. 2000); also AXP 0142+61 (Gavriil et al., submitted); RRAT 1819-1458 (Lyne et al. 2009) Interesting glitch behaviour in magnetars! Livingstone, VK, Gavriil 2010 Chandra ToO Program: Look at High-B radio pulsars at glitch epochs

14. Change of Braking Index? Livingstone, VK, Gavriil et al., in prep.

15. Unification B Transition Objects (e.g. PSR J1846-0258)

16. Anonymous ApJ Review: Aug 12, 1999 “ I believe this paper contains neither substantive new observational nor theoretical results for publication in the Astrophysical Journal… It is not clear if the analogy between PSR J1814-1744 and 1E 2259+586 is valid. Because, first of all, PSR J1814-1744 is a radio pulsar, while 1E 2259+586 is radio-quiet pulsar, without considering their X-ray properties. … There is no solid evidence that this object is similar to that of AXP…” We have come very far.

17. Unification? Pons et al. 2007, Aguilera et al. 2008, Pons et al. 2009 Solid line prediction of model of B-decay heating crust and subsequent cooling: B decay delays cooling; highest B NSs stay hotter longer:``magneto-thermal evolution.”

18. Unification: One Very Rough and Incomplete Possibility Log Age Log B 2 6 4 108 8 12 14 Millisecond pulsars Magnetars Radio Pulsars RRATs “anti-magnetars” Isolated Neutron Stars (aka “going out on a limb”)