Acknowledgments

J. Arons: I have benefitted from many discussions with A. Spitkovsky, P. Chang, N. Bucciantini, E. Amato, R. Blandford, F. Coroniti, D. Backer and E. Quataert. My research efforts on these topics have been supported by NSF grant AST-0507813 and NASA grant NNG06G108G, both to the University of California, Berkeley; by the Department of Energy contract to the Stanford Linear Accelerator Center no. DE-AC3-76SF00515; and by the taxpayers of California. W. Becker: I’m grateful to the Heraeus-Foundation for financing the 363rd Heraeus-Seminar on Neutron Stars and which took place in May 2006 at the Physikzentrum in Bad Honnef. A selection of papers presented at this meet- ing and at the IAU Joined Discussion JD02 in Prague in August 2006 became the groundwork to produce this book. I’m further thankful to Joachim Trumper¨ and Harald Lesch for their help and support in organizing the Heraeus-Seminar and to Gunther¨ Hasinger as well as the MPE for additional financial support. Without the great organizational talent and help of Christa Ingram the meetings would not have been what they were. Thanks also for her help in producing this book. Christian Saedtler has spend many days in producing the index of this book. Sincere thanks to him for taking the time. All articles in this book were refereed. I am much obliged to all colleagues who helped in this process. Special thanks goes to Dr. Jaroslaw Dyks, Dr. Ulrich Geppert, Prof. Dr. Yashwant Gupta, Dr. John Kirk, Dr. Maura McLaughlin, Prof. Dr. Andreas Reisenegger and Prof. Dr. Bronislaw Rudak. K.S. Cheng: We are benefited from the useful conversions and suggestions from H.K. Chang, J.J. Jia, K. Hirotani, J. Takata, M. Ruderman, Anisia Tang, and L. Zhang. This work is partially supported by a RGC grant of Hong Kong Government under HKU7015/05P. U. Geppert: I gratefully acknowledge collaboration and discussions with W. Becker, F. Haberl, D. Page, J. Pons, K.-H. Radler,¨ M. Rheinhardt, and J. Trumper.¨ I am especially grateful to J. Pons and M. Rheinhardt for carefully reading this manuscript.

687 688 Acknowledgments

J. Grindlay and S. Bogdanov: We thank our collaborators on our various MSP papers as cited here. This work was supported in part by various Chandra grants, currently GO7-8033A. K. Hurley: This research has made use of data obtained from the High Energy Astrophysics Science Archive Research Center (HEASARC), provided by NASA’s Goddard Space Flight Center. O.C. de Jager and A. Djannati-Ata¨ı: The first author acknowledges support from the South African Department of Science & Technology and National Research Foundation Research Chair: Astrophysics & Space Science. Support from the GDRI-GREAT French, German, South African & Namibian multinational funding source is also acknowledged. The authors would like to thank members of the Super- Remnant, and Plerion working group of the H.E.S.S. collaboration for useful discussions. J.G. Kirk, Y. Lyubarsky, and J. Petri:´ Our work was supported by a grant from the G.I.F. the German-Israeli Foundation for Scientific Research and Development. M. Kramer: I am grateful to all my co-workers who contributed so significantly to this work. They are I.H. Stairs, R.N. Manchester, M.A. McLaughlin, A.G. Lyne, R.D. Ferdman, M. Burgay, D.R. Lorimer, A. Possenti, N. D’Amico, J.M. Sarkissian, G.B. Hobbs, J.E. Reynolds, P.C.C. Freire and F. Camilo. It is a pleasure to thank Thibault Damour and Norbert Wex for very useful discussions. The Parkes radio telescope is part of the Australia Telescope which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. The National Radio Astronomy Observatory is a facility of the U.S. National Science Foundation operated under cooperative agreement by Associated Universities, Inc. J.M.E Kuipers: I would like to thank my collaborators P.-K. Fung (Royal Netherlands Meteorological Institute, De Bilt, The Netherlands), and D. Khechinashvili (Abastumani Astrophysical Observatory, Georgia), and Dr. A. Jessner for their stimulating discussions. D.R. Lorimer: While the text is a significant update of an earlier article and presents my personal views on this topic, many of my opinions have been formed from the investigations and results of others. In particular, I wish to acknowledge numerous stimulating discussions and debates on pulsar statistics over the years with M. Bailes, Ed van den Heuvel, S. Johnston, R.N. Manchester, A.G. Lyne and J. Cordes. M. McLaughlin: Many thanks to J. Cordes, A.G. Lyne, N. Rea, D. Lorimer and M. Kramer for their contributions to the work described in my review. I am also grateful to WVU undergraduates D. Ludovici and G. Habib for their discoveries of new RRATs in the PMPS and PH survey and to WVU graduate student J. Boyles for his help processing new GBT data on the RRATs. I thank M. Burgay and J. Deneva for their assistance with new RRATs found in the PH and PALFA survey. None of this work would be possible without the observing assistance of the PMPS team. Many thanks also to all on the PH, DMB and PALFA survey teams. Acknowledgments 689

D. Page: The results presented in my paper are strongly indebted to my recent collaborators, M. Kuker,¨ U. Geppert, J.M. Lattimer, M. Prakash, S. Reddy, and A.W. Steiner, but the content and its errors are only the fault of the author. I also warmly acknowledge many discussions with Dima Yakovlev, either directly or through e-mail, whose impact on my work could not be overstated. Jillian A. Henderson is also warmly acknowledged for careful reading of this manuscript. This work was partially supported by a grant from UNAM’s DGAPA program PAPIIT, #IN-119306. R. Prix (for the LIGO Scientific Collaboration): The authors gratefully acknowl- edge the support of the United States National Science Foundation for the construction and operation of the LIGO Laboratory and the Particle Physics and Astronomy Research Council of the United Kingdom, the Max-Planck-Society and the State of Niedersachsen/Germany for support of the construction and operation of the GEO600 detector. The authors also gratefully acknowledge the support of the research by these agencies and by the Australian Research Council, the Natural Sci- ences and Engineering Research Council of Canada, the Council of Scientific and Industrial Research of India, the Department of Science and Technology of India, the Spanish Ministerio de Educacion y Ciencia, The National Aeronautics and Space Administration, the John Simon Guggenheim Foundation, the Alexander von Humboldt Foundation, the Leverhulme Trust, the David and Lucile Packard Founda- tion, the Research Corporation, and the Alfred P. Sloan Foundation. This document has been assigned LIGO Laboratory document number LIGO-P060039-05-Z. M. Ruderman: I am happy to thank A. Beloborodov, E.V. Gotthelf, J.P. Halpern, P. Jones, A. Lyne, J. Sauls, J. Trumper,¨ and colleagues at the Institute of Astronomy (Cambridge) and the Center for Astrophysics and Space Sciences (UCSD) for help- ful discussions and hospitality. I am especially grateful to U. Geppert for his excel- lent advice and criticism. S. Tsuruta: I acknowledge with special thanks the contributions by and valuable discussions with W. Becker, T. Takatsuka, R. Tamagaki, J. Sadino, A. Liebmann, M.A. Teter, A. Kobelsky, J. Thiel, H. Umeda, K. Nomoto, T. Tatsumi, W. Candler, and K. Fukumura. Thanks are due to K. Nomoto and T. Tatsumi for their hospitality during our visits to Tokyo University and Kyoto University. Our work for this paper has been supported in part by NASA grants NAG5-12079, AR3-4004A, and G02- 3097X. F. Weber, R. Negreiros, and P. Rosenfield: The material used in this review paper is based upon work supported by the National Science Foundation under Grant No. 0457329, and by the Research Corporation. V.E. Zavlin: I gratefully acknowledge the collaboration with George Pavlov and many other colleagues in studying neutron stars during the last 15 years. This work was supported in part by a NASA Associateship Award. Index

Alfven´ critical current, 416 flux tubes Alfven´ crossing time, 327 magnetic, 355–372 Alfven´ frequency, 327 Alfven´ pulse, 551 gamma-ray burst, 577 Alfven´ speed, 383 geodetic precession, 83, 84, 88 Alfven´ transit time, 395, 560 giant flare, 580 Alfven´ wave, 384, 385 , 367 Alfvenic´ front, 551 Crab-like glitches, 367–369 aligned rotator, 426 Vela-like glitches, 369–370 ATNF catalog, 4, 19 globular cluster pulsars, 119–125, 167–175 Goldreich–Julian charge loss rate, 441 resonances, 216, 220 Goldreich–Julian density, 425, 485, 505, 524, Bohm limit, 464 549 Bragg reflection, 602 gyro-radius, 431, 459 braking index, see magnetic braking index H-dibaryon matter, 223 braking model, see magnetic braking model Hall-cascade, 324 bremsstrahlung Hall-drift, 343–345 –ion bremsstrahlung, 261 heat flux vector, 347 n-n bremsstrahlung, 259 inverse Compton scattering, 433, 434 CCO, see central compact object central compact object, 111–115, 207, Klein–Nishina limit, 456, 476, 527, 532 596 L − E˙ relation, 125–137, 513 Chandrasekhar mass, 91 x Landau states, 533 Cherenkov imager, 631 Larmor frequency, 323 see color-superconductivity, superconductivity light cylinder, 99, 365, 376, 484, 485, 524, 549 conversion efficiency, 126–129, 477, 478, Lorentz factor, 427, 505 514 Lorentz force, 483 cooling curve vs. data, 117, 302, 307 Lorentz torque, 550, 551 Cooper pairing, 226–228, 254–257, 304, 309, 312–314 , see neutron stars critical temperature, 156, 254, 255, 257 magnetic braking index, 11, 96, 98 magnetic braking model, 96–98 death line, 382, 394, 397, 402, 527 magnetic field decay, 11 magnificent seven, 143, 144, 146 electron Compton wavelength, 527 distances, 150 exotic , 223 optical counterparts, 150

691 692 Index magnificent seven (Continued) cooling era, 101, 268–269, 271, proper motion, 150 285, 286, 298, 304, 309 surface temperature distribution, 152 neutrino emission, 101, 228, 258–262 timing properties, 146 processes, 258 mass–mass diagram, 82 neutrino emissivity, 102, 295, 301–302, 347 meson condensation, 222 neutrino luminosity, 273, 295, 297, 298, 301 millisecond pulsars, see pulsars nonstandard cooling, 302, 304, 308, 309, 312–314, 316 perturbation, 232 neutron stars photon cooling era, 268–269, 298, 309 accelerated cooling scenario, 101 photon luminosity, 168, 262, 272, 276, anti-aligned magnetized rotating NS, 557 296–298, 310 burst oscillations, 215 pion-mixed neutron stars, 315–316 structure, 234–238 proto , 230–231, 240, 325 composition, 216, 226, 299–301 quasi-stationary approximation, 329 cooling, 249 specific heat, 252–253 cooling curves, 115 standard cooling, 101, 102, 270, 279, 292, critical mass, 278, 281, 286 301 cross section, 300 cooling curves, 297, 302 density relation, 296 structure, 249–251, 299–301 dipolar equilibrium field, 331 temperature distribution, 121, 145, 154, 267, effective temperature, 267 283, 284, 345–351 equation of state, 145, 176–179, 215–242, temperature profile, 281–282, 342 281, 294, 299, 528 thermal emission, 115, 345, 394, 488, 534, fast cooling, 277–282, 302, 511 596 heat transport, 153, 264–265, 324, 343 thermal energy content, 252 heating mechanism, 101, 305 thermal evolution, 100–102, 241, 270, 279, -mixed neutron stars, 313 292, 306–316, 347 initial mass function, 87, 287 thermal relaxation in young NSs, 341 interior magnetic field, 337 thermal structure of the NS crust, 348 isolated neutron stars, 58, 59, 95–102, 117, thermoelectric instability, 339 143–163, 249, 321–352, 681 temperature and magnetic field surface objects distribution, 143 0531+21, 131, 135 magnetars, 12, 35, 104, 275, 321, 382, 525, 0833−45, 131, 135 577–589, 595–596 1E 1207.4−5209, 207, 310 magnetic energy content, 341 1E 1613−5055, 113 magnetic field, 284, 305, 321–352, 355–372 1RXS J214303.7+065419, 147, 150 stability of, 327 3C58, 274 changes in spinning down, 360–361 47 Tucanae, 27, 169, 170, 516 dipole field changes in spinning up, 4U0115+63, 618 361–363 4U0900−40, 618 field lines, 154 4U1538−58, 618 field strength, 336 4U1626−67, 618 geometry, 332 4U1636−53, 618 magnetized envelopes, 266–267 4U1822−37, 618 mass vs. central density, 219 1E 1207.4−5209, 111 mass–radius relationship, 218 1E 1613−5055, 111 masses, 217–219 B0540−69, 94 MHD instabilities, 325 B0656+14, 115, 200 minimal cooling, 270, 275, 312 B0833−45, 109 models, 217, 219, 371, 658 B1046−58, 109 moment of inertia, 48 B1055−52, 115, 200 net electric field, 234–238 B1509−58, 94 Index 693

B1706−44, 109, 198 B0656+14, 35, 38, 131, 135, 310, 513 B1821−24A, 124 X-ray spectrum, 116 B1919+21, 183 B0823+06 B1951+32, 109 pulse profile, 118 B1957+20, 121 B0823+26, 117, 131, 136, 311 B2334+61, 199 B0826−34, 28, 570–572 Cas−A, 111 B0833−45, see Vela pulsar CXOU J085201.4−461753, 111 B0943+10, 131, 136, 570 CXOU J185238.6+004020, 111 pulse profile, 386 CXOU J232327.8+584842, 111 B0950+08, 117, 131, 136, 203, 513 G347.3−0.5, 111 pulse profile, 118 Her X−1, 93 B1046−58, 131, 135, 311, 513 J0030+0451, 205 B1055−52, 131, 135, 274, 310, 513 J0205+6449, 184 B1133+16, 131, 136 J0437−4715, 120, 121, 205 B1257+12, 13, 132, 133 − J0538+2817, 199 B1259 63, 131, 135 − J1024−0719, 205 B1509 58, 131, 135, 311, 513 J1119−6127, 108, 196 B1534+12, 132, 133 − J1357−6429, 197 B1610 50, 131, 136, 513 − J1617−5055, 107 B1620 26, 13, 132, 133, 175 − J1811−1959, 107 B1706 44, 131, 135, 310, 513 − J2043+2740, 204 B1719 37, 131, 136 B1757−24, 131, 135 J2124−3358, 121, 205 B1800−21, 131, 135 J2229+6114, 109 B1821−24, 124, 132, 133, 169, 174, 513 Kes 79, 111 pulse profile, 122 PKS 1209−51/52, 111 B1823−13, 131, 135, 311 Pupis−A, 111 B1828−11, 153 RCW 103, 111 B1853+01, 131, 135, 513 RX J0822−4300, 111 B1855+09 RX J1713.7−3946, 111 pulse profile, 366 Sco X−1, 92 − B1919+21, 560 Vela Jr, 111 B1929+10, 117, 131, 136, 311, 461, 513 − B0021 72C, 132, 134 pulse profile, 118 − B0021 72D, 132, 134 B1931+24, 7, 30, 31, 67 − B0021 72E, 132, 133 intermittent nature, 67 − B0021 72F, 132, 133 period variation, 68 − B0021 72G, 132, 134 B1937+21, 34, 132, 133, 168, 215, 217, 513 − B0021 72H, 132, 134 pulse profile, 122, 366 − B0021 72I, 132, 134 B1951+32, 131, 135, 311, 513 − B0021 72J, 132, 134 B1953+29 B0021−72L, 132, 134 pulse profile, 366 B0021−72M, 132, 134 B1957+20, 132, 133, 168, 175, 215, 512 B0021−72N, 132, 134 pulse profile, 366 B0031−07, 35 B2224+65, 117, 131, 136, 311 drifting sub-pulses, 546 B2334+61, 131, 136, 311 B0355+54, 131, 135 black widow pulsar, see B1957+20 B0531+21, 105, see Crab pulsar Cen A, 618 pulse profile, 106 Cen X−1, 618 B0537−69, 513 Cir X−1, 618 B0540−69, 131, 135, 513 Crab nebula, 104, 401, 406, 423, 431, 618 B0628−28, 117, 131, 136, 311 magnetisation, 448 pulse profile, 118 shock radius, 442 B0633+17, see Geminga spectrum, 438 694 Index objects (Continued) J0628+09, 26 Crab pulsar, 96, 105, 184, 311, 483, 513, J0631+1036, 131, 136, 513 539, 618 J0633+1746, 131, 135 optical polarization, 509 J0633+1748, see Geminga phase averaged spectrum, 508 J0737−3039, 132, 133 phase resolved spectrum, 504, 507 J0737−3039A/B, 23, 76 photon index, 131, 440 mass–mass diagram, 82 polarization, 508 parameters, 80 pulse profile, 106, 594 pulse vs. orbital phase, 76 CTA 1, 274 J0751+1807, 132, 133 CXOU J061705.3+222127, 207 J0843−43, 49 CXOU J232327.8+584842, 311 J1012+5307, 132, 133 Cyg X−1, 618 J1024−0719, 132, 133 Cyg X−2, 618 J1057−5226, 539 Cyg X−3, 618 J1105−6107, 131, 135 G084.2−0.8, 311 J1119−6127, 131, 135 G093.3−6.9, 311 J1124−5916, 131, 135, 311 G127.1+0.5, 311 J1141−6545, 26 G226−29, 229 J1301−6305, 131, 135 G315.4−2.3, 311 J1317−5759, 48, 50 Geminga, 115, 131, 135, 200, 310, 513 J1326−6700, 27 compact X-ray nebula, 511 J1357−5759, 55 GRS 1915+105, 618 J1357−6429, 131, 135 GS1826−238, 618 J1420−6048, 131, 135 GX 1+4, 618 J1443−6040, 46, 47, 50 GX 5−1, 618 J1509−5850, 131, 136 Her X−1, 618 J1513−5908, 539 HESS J1825−137, 465 J1617−5055, 131, 135 J0024−7204O, 132, 133 pulse profile, 109 J0024−7204Q, 132, 133 J1655−40, 618 J0024−7204R, 132, 134 J1701−3006B, 132, 134 J0024−7204S, 132, 134 J1709−4429, 539 J0024−7204T, 132, 133 J1717−4054, 27 J0024−7204U, 132, 133 J1740−5340, 132, 134, 171 J0024−7204W, 132, 133, 171 Chandra image, 173 pulse profile, 172 J1744−1134, 132, 133 J0024−7204Y, 132, 134 J1744−28, 618 J0030+0451, 132, 133, 178 J1747−2958, 131, 135 pulse profile, 122, 178 J1748−2446ad, 27, 215, 217 J0034−0534, 132, 133 J1748−2446I, 27 J0108−1431, 131, 136 J1748−2446J, 27 J0154+61, 311 J1751−305, 618 J0205+6449, 131, 135, 274, 311 J1754−30, 51 J0218+4232, 34, 132, 133 J1808.4−3658, 618 pulse profile, 34, 122, 366 J1809−1917, 131, 135 spectrum, 538 J1809−1943, 22, 35, 36 J0437−4715, 132, 133, 169, 174, 177, 513, J1811−1925, 131, 135 635 J1811−1926, 513 bow-shock nebula, 123 J1819−1458, 46–48, 51, 55 pulse profile, 122, 177, 366 J1824−2425A, 124 X-ray spectrum, 123, 206 J1824−2425E, 124 J0537−6910, 131, 135 J1824−2425H, 124 J0538+2817, 131, 136, 310 J1824−2425I, 124 J0609+2130, 13 J1824−2425J, 124 Index 695

J1824−245H, 132, 133 J1911+00, 47, 48 J1826−14, 51 J1913+1333, 47, 48 J1832+0029, 69 RX J0002+6246, 310 period variation, 69 RX J0007.0+7302, 207, 274, 311 J1839−01, 46, 51 RX J0420.0−5022, 147, 150 J1840−0809, 45 pulse profile, 148 J1840−0815, 45 RX J0720.4−3125, 147, 150, 154, 274, 310 J1846−0258, 52, 131, 136, 513 phase residuals, 155 J1848−12, 52 spectrum, 149 J1906+0746, 15 RX J0806.4−4123, 147, 150 J1909−3744, 25 RX J0822−4300, 310 J1910−5959B, 132, 134 RX J1308.6+2127, 147, 150, 153 J1911+00, 46, 47, 53 pulse profile, 148 J1911−6000C, 132, 134, 175 RX J1605.3+3249, 147, 150 J1911−6000D, 132, 134 RX J1856.5−3754, 147, 150, 162, 285, 310 J1913+1333, 48, 53, 58 RX J7020.4−3125, 153 J1928+15, 64 Sco X−1, 618 J1930+1852, 131, 135 SGR0525−66, 578, 588 J1952+3252, 539 SGR1627−41, 578 J1953+1846A, 132, 133, 175 SGR1806−20, 578, 582, 584, 586, 587 J2019+2425 pulse profiles, 581 pulse profile, 366 SGR1900+14, 578, 579, 582, 618 J2021+3651, 131, 136 SMC X−1, 618 J2043+2740, 117, 131, 136, 311 Terzan 5, 26, 27, 174 J2124−3358, 132, 133, 178, 513 Vela pulsar, 109, 198, 274, 310, 483, 513, bow-shock nebula, 123 539 pulse profile, 122, 178 XTE J1739−285, 215 J2229+6114, 131, 135, 513 XTE J1810−197, 22, 35, 42 J2235+1506, 14 observatories J2322+2057 ACT, 625 pulse profile, 366 AGILE, 625, 627, 638, 639 M28, 174 ALFA, 25 X-ray image, 124 AMS, 638–640 M4, 175 ASCA, 95, 103, 168, 473, 487 M71, 175 ATNF, 4, 19 Magellanic cloud, 25 BeppoSAX, 95, 487 NGC 104, 125 CANGAROO, 635 NGC 4151, 618 CGRO, 487, 623 NGC 6397, 171 Chandra, 95, 103, 146, 151, 162, 167–169, NGC 6752, 175 487, 617 OAO1657−41, 618 CTA, 636 Procyon B, 229 EGRET, 398, 623, 624, 627, 638 PWN Vela X, 441 Einstein, 94, 103, 143, 292, 617 RCW 103, 108 EUVE, 95 RRATs EXOSAT, 95 J0848−43, 47, 48 GBT, 15 J1317−5759, 47, 48 Gen-X, 179 J1443−6040, 47, 48 GLAST, 398, 418, 419, 449, 625, 626, J1754−30, 47, 48 640–648 J1819−1458, 47, 48 H.E.S.S., 629, 634–635 J1826−14, 47, 48 HESS, 453, 455 J1839−01, 47, 48 IXO, 162, 179, 619 J1846−0258, 47, 48 LOFAR, 15 J1848−12, 47, 48 LTT, 636 696 Index observatories (Continued) striped wind, 408–411, 424, 429–432, MAGIC, 632–634 435 PALFA, 25 termination shock, 405, 412, 419, 424, 433, Parkes multi-beam survey, 15, 22 438–442, 511 RHESSI, 617 pulsars ROSAT, 95, 103, 144, 168, 169, 473, 3-D velocity, 1 487 anomalous X-ray pulsar, 20, 97, 595 RXTE, 95, 167, 168, 487 comparison SGR, 588 SKA, 15 AXP, see anomalous X-ray pulsar Spectrum-X, 617 birth rate, 10 UHURU, 292 braking hypothesis, 11 VERITAS, 625, 631–632 braking torque, 11 Very Long Baseline Interferometry, see CCO, seecentral compact object97 VLBI characteristic age, 20, 530 VLBI, 88, 293 CHR model, 492–494 Westerborg synthesis radio telescope, 15 cluster pulsar population, 27 XMM-Newton, 95, 103, 145, 148, 167, 176, cooling frequency, 512 487 Crab giant pulses, 33 XPOL, 163 Crab-like pulsars, 104–111 orbital decay, 88 CRZ model, 499–502 distribution, 2 P–P˙ diagram, 3, 21, 75, 97, 377, distributions in galactic z-distance, 24 528 distributions in galactocentric radius, 24 P–P˙ diagram double pulsars, 73–89 multiplicities, 403 evolution, 87 pair annihilation process, 262 drifting subpulses, 31 pairing, see Cooper pairing electrodynamics, 547–555 pattern circulation, 562 electrosphere, 385–388 pentaquark, 224 gamma-ray pulsar candidates, 645 photo disintegration, 300 gap models, 389–406 photo-neutrino process, 262 giant pulses, 33 plasma physics, 73–77, 555 globular cluster pulsars, 14, 119–125, polarimeter, 163, 542, 592–593 167–175 photo-electron tracking polarimeter, GRB, see gamma-ray burst 606–610 high energy emission, 483–520 scattering polarimeter, 605–606 high-energy emission post-Keplerian parameters, 79 models, 98 Poynting flux, 376, 379, 384, 404, 426 histogram of observed periods, 20 pulsar wind nebulae, 98, 379, 401, 423, 438, initial spin period, 11 453–480 intermittent pulsars, 67 cooling radius, 462–463 magnetosphere, 381, 382, 390, 399, 486 emission, 441 relativistic magnetosphere, 383 high energy emission, 483–520 MHD model, 378 inner wind, 408 millisecond pulsars, 119–125, 167–181, 516 jet-torus structure, 443, 447 population, 12 MHD model, 404–408 radiation, 537 jet, 447 radio-quiet MSP, 179 post-shock plasma, 443 X-ray emission, 169 proper motion in jets, 443 X-ray properties, 518 PWN shocks, 458, 461 mode changing, 27–30 sandwich magnetic field model, 413 null charge surfaces, 485 shock acceleration, 407, 413–418 outer gap model, 99, 484, 492–502 shock radius, 454, 462, 510–512, 518 geometry, 493 simple pulsar wind model, 510 period evolution, 11 Index 697

polar cap, 99, 365, 425, 485 quark deconfinement, 224 emission, 180 quark-hybrid star, 227 heating luminosity, 529 high energy emission, 523–542 radio intermittency, 7 radius, 548 radio sky background, 5 space-charge limited flow gap, 525 Rayleigh-Taylor instability, 447 temperature, 517 recent surveys, 25 vacuum gap, 525 relativistic cyclotron frequency, 565 polar gap, 484 relativistic wind, 78 breakdown, 557 , see RRAT model, 489–492 RRAT, 23, 40, 43, 47, 67 position angle, 37 population estimates, 61 propagation effects in ISM, 5 radio observations, 48 proper motion, 1, 36 recent discoveries, 63 pulse modulation, 31 results of Monte Carlo simulations, 62 pulse nulling, 6, 27–30, 70 rotational properties, 59 pulsed fraction, 108, 110, 118, 121, 179 single-pulse search, 45, 64 quasi periodic modulation, 30 spectral fits, 57 radial distribution, 8 spin-down luminosity, 48 radio emission geometry, 539 surface dipole magnetic field, 48 radio emission properties, 18 X-ray properties, 54 radio pulsars, 593–595 Schwarzschild radius, 185 Clemens and Rosen model, 558 Shapiro delay, 81 diocotron instability model, 561–572 SNR, see remnants drift wave models, 559 solar-system test, 88 drifting sub-pulses, 545–575 spectrum in cold plasma, 158 models of drifting sub-pulses, 555–561 strange dwarfs, 216, 229, 230 phenomenological Wright-model, 557 strange quark matter, 216, 228–230 Ruderman and Sutherland models, 556 experiments, 242 statistics, 1 surface properties, 229 rotation axis, 37 striped wind, see pulsar wind nebulae rotation-powered pulsars, 96–98, 111, strong-field gravity, 77 377 superconductivity, 254–257 selection effects in surveys, 5 color, 226 SGR, see soft gamma-ray repeater superdense matter, 215–242 size of emission beam, 6 superfluidity, 254–257, 303 slot cap supernova remnants, 103–115 high energy emission, 523–542 synchrotron cooling, 439, 454 slot gap model, 489–492 synchrotron limit, 459 soft gamma-ray repeater, 97, 577–589, 595 comparison AXP, 588 Thomson limit, 456, 464 general locations, 580 transient phenomena, 67 spatial distribution, 4 spin down rate, 19 URCA process, 222 spin down times, 371 direct URCA process, 258 standard magnetospheric models, 484–487 medium modified URCA process, 259 strength of dipole field, 20 modified URCA process, 258 vacuum models, 378 Vela-like pulsars, 109–111 vortex lines, 356, 358, 360, 361 X-ray emission, 593 X-ray luminosity vs. spin-down power, 514, X-ray binary, 597–599 515 X-ray Dim Isolated Neutron Stars , see XDIN PWN, see pulsar wind nebulae438 XDIN, 144–163, 596