The Neutron Star Zoo. Stephen C.-Y. Ng ( 吳志勇 ) HKU
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1 The Neutron Star Zoo Stephen C.-Y. Ng ( 吳志勇 ) HKU
2 Overview Introduction to neutron stars Different classes of neutron stars: Radio Pulsars MSPs Magnetars DINS CCOs Unification 6/12/2017 NAOC Stephen Ng
3 Evolution of Massive Stars Brooks/Cole Thomson Learning 6/12/2017 NAOC Stephen Ng
4 Extreme Physics Densest star: M 1.4 M, R 10 km 6/12/2017 NAOC Stephen Ng
5 Neutron Star 10km 6/12/2017 NAOC
6 Neutron Star 10km or 466,000 X 6/12/2017 NAOC Stephen Ng
7 Extreme Physics Densest star: M 1.4 M, R 10 km r~10 14 g/cm 3 World Population: /12/2017 NAOC Stephen Ng
8 Large Nucleus Nuclear density: g/(10-13 cm) 3 A=294 A= /12/2017 NAOC Stephen Ng
9 Extreme Physics Densest star: M 1.4 M, R 10 km Strongest magnetic fields in the Universe 10 4 G 0.5G G 6/12/2017 Stephen Ng
10 Extreme Physics Densest star: M 1.4 M, R 10 km Strongest magnetic fields in the Universe Test of strong gravity and strong magnetism 6/12/2017 NAOC Stephen Ng
11 Gravitational Waves 6/12/2017 NAOC Stephen Ng
12 New Elements 6/12/2017 NAOC Stephen Ng
13 6/12/2017 Stephen Ng
14 6/12/2017 Stephen Ng
15 Radio Pulsars Neutron star was predicted by Baade and Zwicky in 1934 In 1967 (33 years later!) Jocelyn Bell discovered pulsed radio signal with period of 1.3s. LGM-1 6/12/2017 NAOC Stephen Ng
16 LGM-1 6/12/2017 NAOC Stephen Ng
17 Her PhD supervisor, Antony Hewish, awarded Nobel Prize in 1974 due to the discovery 6/12/2017 NAOC Stephen Ng
18 Pulsar = Rotating NS? Light crossing time 1.4ms 400km compact object Stable clocks: rotation, pulsation, binary Break-up period Ω 2 R GM R 2 ; Ω2 Gρ Rules out white dwarfs, as P > 1s. Black hole has no structure, accretion not periodic P ሶ > 0 rules out pulsation Rotating NS is the only choice 6/12/2017 NAOC Stephen Ng
19 Pulsars Rotating neutron stars Stable clocks 6/12/2017 NAOC Stephen Ng
20 Radio Pulsars known in our Galaxy Period: s Broadband emission: radio, optical, X-rays, -rays =L / Ė < 1% Powered by rotation, spin down steadily 6/12/2017 NAOC Stephen Ng
21 Radio Pulsars known in our Galaxy Period: s Broadband emission: radio, optical, X-rays, -rays =L / Ė < 1% Powered by rotation, spin down steadily 6/12/2017 NAOC Stephen Ng
22 Observational Properties Observable P t = P 0 + ሶ Pt ሷ Pt 2 + Characteristic age τ c = P 2 ሶ P Spin-down power ሶ E = d dt 1 2 Iω2 = Iωω ሶ = 4π 2 I Pሶ P 3 Surface dipole field B = P ሶ P 1/2 G 6/12/2017 NAOC Stephen Ng
23 P- ሶ P Diagram 6/12/2017 NAOC Stephen Ng
24 P- ሶ P Diagram 6/12/2017 Stephen Ng
25 Pulsar Winds Where does pulsar rotational energy go? E ሶ > erg/s < 10% in radiation (mostly -rays) > 90% in pulsar winds 6/12/2017 NAOC Stephen Ng
26 Pulsar Winds 6/12/2017 NAOC D. Page Stephen Ng
27 Pulsar Wind Nebula 6/12/2017 NAOC Stephen Ng
28 Ng et al. (2010) G ATCA X-ray + Radio Radio ATNF/CSIRO Kargaltsev et al. (2008); Ng et al. (2010) 6/12/2017 NAOC Stephen Ng
29 The Frying Pan 2000 km/s Longest pulsar tail > 20pc 6/12/2017 NAOC Ng et al. (2012)
30 PSR J /12/2017 NAOC Ng et al. (2017)
31 The Snail (G ) Temim et al (2009) Ma, Ng et al. (2015) 6/12/2017 NAOC Stephen Ng
32 Hand of God (MSH 15-52) 6/12/2017 NAOC Stephen Ng
33 Hand of God (MSH 15-52) 6/12/2017 NAOC Stephen Ng Leung, Ng et al., in prep.
34 Hand of God (MSH 15-52) Leung, Ng et al., in prep. 6/12/2017 NAOC Stephen Ng
35 Classes of Neutron Stars Radio Pulsars MSPs Magnetars DINS CCOs 6/12/2017 NAOC Stephen Ng
36 P- ሶ P Diagram 6/12/2017 Stephen Ng
37 P- ሶ P Diagram 6/12/2017 Stephen Ng
38 Classes of Neutron Stars Radio Pulsars MSPs Magnetars DINS CCOs 6/12/2017 NAOC Stephen Ng
39 Millisecond Pulsars Period: a few ms First discovered in 1982 by Becker et al. (PSR B ) Unification: old objects recycled via accretion 6/12/2017 NAOC NASA/Dana Berry
40 P- ሶ P Diagram 6/12/2017 Stephen Ng
41 Detecting Gravitational Waves Pulsar Timing Array 6/12/2017 NAOC D. Champion Stephen Ng
42 Gamma-ray Pulsars CGRO / EGRET 9 years 6 pulsars 1 possible MSP Fermi / LAT Since pulsars 93 MSPs more coming 6/12/2017 NAOC Stephen Ng
43 Fermi Pulsars Caraveo (2014) 6/12/2017 NAOC
44 Gamma-ray Pulsars 6/12/2017 NAOC Caraveo (2014)
45 Aliu et al. (2008) B-field at Light Cylinder B lc = R R lc 3 Bs R = 10km R lc = cp 2π 6/12/2017 NAOC Stephen Ng
46 Gamma-ray Pulsars 6/12/2017 Caraveo (2014)
47 PSR B First MSP discovered Highest B lc =10 6 G, even higher than the Crab Non-thermal X-ray emission, giant pulses Aligned gamma-ray and radio pulses 6/12/2017 NAOC Stephen Ng Ng et al. (2014)
48 PSR B First MSP discovered Highest B lc =10 6 G, even higher than the Crab Non-thermal X-ray emission, giant pulses Aligned gamma-ray and radio pulses co-located emission region new emission mechanism 6/12/2017 NAOC Stephen Ng
49 High-B lc MSPs 6/12/2017 NAOC Ng et al. (2014)
50 Classes of Neutron Stars Radio Pulsars MSPs Magnetars DINS CCOs 6/12/2017 NAOC Stephen Ng
51 P- ሶ P Diagram 6/12/2017 Stephen Ng
52 Magnetars: Extreme Pulsars First discovered in 1990s 23 confirmed (4 detected in radio) Extremely strong B G > B QED High temperature, L Eሶ => powered by B-field decay Violent outbursts 6/12/2017 NAOC John Rowe Animations
53 Magnetars 0-10s 0-10Myr >10Myr Magnetar Radio pulsar Kouveliotou et al. (2003) 6/12/2017 NAOC Stephen Ng
54 Chandra X-ray Observatory 1E ESA/Tiengo et al. 6/12/2017 NAOC Ng et al. (2011) Stephen Ng
55 Swift J /12/2017 Scholz, Ng et al. (2012)
56 SGR /12/2017 NAOC Stephen Ng Mong & Ng (2017)
57 1E : Anti-Glitch 6/12/2017 Archibald, Kaspi, Ng et al. (2013, Nature)
58 1E : Delayed Torque Variation 1700 days 1700 days Delayed torque variation 100 days 6/12/2017 Archibald, Kaspi, Ng et al. (2015)
59 Magnetar Timing Properties Outbursts not always associated with glitches Pulse profiles 6/12/2017 NAOC Stephen Ng
60 Magnetar Timing Properties Outbursts not always associated with glitches Pulse profiles 6/12/2017 NAOC Stephen Ng
61 Magnetars: Extreme Pulsars First discovered in 1990s 23 confirmed (4 detected in radio) Extremely strong B G > B QED High temperature, L Eሶ => powered by B-field decay Violent outbursts Unification? 6/12/2017 NAOC John Rowe Animations
62 Unification Magnetar-like outbursts from a high-b radio pulsar Low-field magnetar: SGR , J Radio emitting magnetars Surface temperature Magneto-thermal evolution 6/12/2017 NAOC Stephen Ng
63 High-B Radio Pulsars 6/12/2017 Stephen Ng
64 High-B Radio Pulsars Strong B-fields as magnetars But similar behavior as normal radio pulsars Radio to -ray pulsations Rotation-powered Transition objects, key to understand magnetars (Ng & Kaspi 2011 for a review) 6/12/2017 NAOC Stephen Ng
65 Young High-B PSRs PSR J P = 0.33s B = G Age = 728yr PSR J P = 0.41s B = G Age = 1610yr PSR B P = 0.15s B = G Age = 1700yr 6/12/2017 NAOC Stephen Ng
66 Magnetar-Like Outbursts PSR J /12/2017 NAOC Gavriil et al. (2008)
67 PSR J / Kes Ng et al. (2008); Livingstone, Ng et al. (2011)
68 PSR J /G XMM-Newton 6/12/2017 NAOC 10 Ng et al. (2012)
69 PSR J /G XMM-Newton Göğüş et al NAOC 10 Ng et al. (2012)
70 Hand of God (MSH 15-52) PSR B B=1.5x10 13 G Hu, Ng, et al. (2017) 6/12/2017 NAOC
71 Thermal Luminosity 6/12/2017 Hu, Ng, et al. (2017)
72 Surface Temperature Mong & Ng (2017) 6/12/2017 NAOC Stephen Ng
73 Unification Magnetar-like outbursts from a high-b radio pulsar Low-field magnetar: SGR , J Radio emitting magnetars Surface temperature Magneto-thermal evolution Toroidal B-field 6/12/2017 NAOC Stephen Ng
74 Classes of Neutron Stars Radio Pulsars MSPs Magnetars DINS CCOs 6/12/2017 NAOC Stephen Ng
75 Dim Isolated Neutron Stars The Magnificent Seven INS / DINS / XDINS / NTEINS Nearby, thermally emitting isolated neutron stars P 10s B=1-3x10 13 G < 1kpc No radio emission 6/12/2017 NAOC
76 P- ሶ P Diagram 6/12/2017 Stephen Ng
77 Unification Old pulsars born with strong B-fields Radio beam missing us Relatively high surface temperature Nearby, otherwise undetected due to interstellar absorption 6/12/2017 NAOC Stephen Ng
78 Classes of Neutron Stars Radio Pulsars MSPs Magnetars DINS CCOs 6/12/2017 NAOC Stephen Ng
79 Central Compact Objects 7 known, found near the center of SNRs => young objects No radio, IR, optical emission, no PWN Thermal X-rays, high T, small R First CCO 6/12/2017 NAOC NASA/CXC/SAO/D.Patnaude et al.
80 Anti-Magnetars? Only 3 CCOs have pulsations detected Periods: s B-field: (3-10) G 6/12/2017 NAOC Stephen Ng
81 P- ሶ P Diagram 6/12/2017 Stephen Ng
82 Anti-Magnetars? Only 3 CCOs have pulsations detected Periods: s B-field (3-10)x10 10 G CCOs as Anti-magnetars born with weak B? buried by fallback? Why no radio emission? 6/12/2017 NAOC Stephen Ng
83 Hunting for CCOs X-ray surveys: all pulsars coincident with supernova remnants (Bogdanov, Ng, & Kaspi 2014) all weak-field radio pulsars in the Galactic plane (Luo, Ng, et al. 2015) 6/12/2017 NAOC Luo, Ng, et al. (2015) Stephen Ng
84 P- ሶ P Diagram 6/12/2017 Stephen Ng
85 Grand Unification of NS Log B 14 Magnetars CCOs (anti-magnetars) Radio Pulsars Isolated Neutron Stars /12/2017 NAOC Millisecond pulsars Kaspi (2010) Stephen Ng Log Age
86 Binary Pulsars Gamma-ray binaries PSR B J / MT /12/2017 NAOC Stephen Ng
87 Binary Pulsars Gamma-ray binaries PSR B J / MT /12/2017 NAOC Stephen Ng Ho, Ng, et al. (2017)
88 Future FAST Hard X-ray Modulation Telescope (HXMT) 慧眼 Neutron star Interior Composition ExploreR (NICER) erosita Large Observatory for X-ray Timing (LOFT) Square Kilometre Array (SKA) 6/12/2017 NAOC Stephen Ng
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