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Acknowledgments 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 Pulsars 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- nova Remnant, Pulsar 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 glitch, 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 baryon 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 electron–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 magnetars, see neutron stars critical temperature, 156, 254, 255, 257 magnetic braking index, 11, 96, 98 magnetic
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