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Preface; Contents; 1 Radio Properties of Pulsar Wind Nebulae; 1.1 Introduction; 1.2 Background Information; 1.2.1 Pulsars; 1.2.2 Pulsar Wind Nebulae; 1.2.2.1 Early Evolution of PWNe; 1.2.2.2 Mature PWNe: Interaction with the Reverse Shock; 1.2.2.3 Late PWN Evolution; 1.3 Radio Emission from Pulsar Wind Nebulae; 1.3.1 Synchrotron Emission from PWNe; 1.3.2 Radio Spectra of PWNe; 1.3.3 Spectral Breaks in PWNe; 1.4 Magnetic Fields in PWNe; 1.4.1 Magnetic Fields in Young PWNe; 1.4.2 Magnetic Fields in Evolved PWNe; References; 2 Optical and Infrared Observations of Pulsar Wind Nebulae
2.1 Introduction2.2 Properties and Evolution of PWNe; 2.2.1 Basic Properties; 2.2.2 PWN Evolution; 2.3 Optical and Infrared Emission from PWNe; 2.3.1 Non-thermal Emission from the PWN; 2.3.2 Emission from Shocked SN Ejecta; 2.3.3 Emission from SN-Formed Dust; 2.4 Summary; References; 3 Pulsar Wind Nebulae Viewed Through the Gamma-Ray Eye; 3.1 Introduction; 3.2 Unidentified Sources and PWNe; 3.3 The HE to VHE Connection; 3.4 Demography of the Gamma-Ray PWNe; 3.4.1 Few Young and Energetic Nebulae; 3.4.2 A Large Population of Old and (Re)Tired Nebula; 3.5 Pulsar Wind Nebulae Flares
3.6 Magnetar Wind Nebulae: MWNe3.7 Conclusion; References; 4 Observational Links Between Fermi-LAT Pulsars and Their Nebulae; 4.1 Introduction; 4.2 High-Energy Pulsars and Their Relativistic Winds; 4.3 Beyond the Wind: The Pulsar Wind Nebulae; 4.4 Connecting Pulsars and PWNe; 4.4.1 Distribution of LAT Pulsars and TeV PWNe in the Galaxy; 4.4.2 Energetics; 4.5 New Type of Pulsars and Pulsar Wind Nebula; 4.6 Prospects and Conclusions; References; 5 Prospects for Pulsar Wind Nebulae Observations with γ-Ray Astronomy Facilities: Cherenkov Telescope Array and Satellites
5.1 Introduction: An Overview of the Next ``gamma'' Decade5.2 The Future of VHE Astronomy: CTA; 5.3 The Impact of CTA on the Physics of PWN; 5.3.1 CTA Galactic Plane Survey: A Key Science Program; 5.3.2 CTA Energy Dependent Morphology and PWN Identification; 5.3.3 CTA, Crab, and Its Flares; 5.4 Space-Borne Detectors; 5.4.1 Improvement in Angular Resolutionand Polarimetric Capabilities; 5.4.2 Combining the Compton and the Pair-Production Detection Technique; 5.4.2.1 e-ASTROGAM; 5.4.2.2 ComPair; 5.5 The Importance of the MeVâ#x80;#x93;GeV Range for the Physics of PWN; 5.6 Summary; References
6 Crab Observational Status: Nebulae, Pulsations, and Flares6.1 Introduction; 6.2 Crab Pulsar; 6.2.1 The Rotational Frequency; 6.2.2 Pulse Profile; 6.2.3 Polarization; 6.2.4 Giant Pulses; 6.2.5 Spectral Measurements; 6.2.6 Lessons from the Crab Pulsar Observations; 6.3 Crab Nebula; 6.3.1 The "Halo'' and the Cage; 6.3.2 Morphological Measurements; 6.3.3 Spectral Measurements; 6.3.4 The Gamma-Ray Flares; 6.3.5 Polarization Measurements; 6.3.6 Lessons on the Crab Nebula; References; 7 Pulsar Striped Winds; 7.1 Introduction; 7.1.1 General Picture; 7.1.2 Problems; 7.2 MHD Picture: Striped Winds
2.1 Introduction2.2 Properties and Evolution of PWNe; 2.2.1 Basic Properties; 2.2.2 PWN Evolution; 2.3 Optical and Infrared Emission from PWNe; 2.3.1 Non-thermal Emission from the PWN; 2.3.2 Emission from Shocked SN Ejecta; 2.3.3 Emission from SN-Formed Dust; 2.4 Summary; References; 3 Pulsar Wind Nebulae Viewed Through the Gamma-Ray Eye; 3.1 Introduction; 3.2 Unidentified Sources and PWNe; 3.3 The HE to VHE Connection; 3.4 Demography of the Gamma-Ray PWNe; 3.4.1 Few Young and Energetic Nebulae; 3.4.2 A Large Population of Old and (Re)Tired Nebula; 3.5 Pulsar Wind Nebulae Flares
3.6 Magnetar Wind Nebulae: MWNe3.7 Conclusion; References; 4 Observational Links Between Fermi-LAT Pulsars and Their Nebulae; 4.1 Introduction; 4.2 High-Energy Pulsars and Their Relativistic Winds; 4.3 Beyond the Wind: The Pulsar Wind Nebulae; 4.4 Connecting Pulsars and PWNe; 4.4.1 Distribution of LAT Pulsars and TeV PWNe in the Galaxy; 4.4.2 Energetics; 4.5 New Type of Pulsars and Pulsar Wind Nebula; 4.6 Prospects and Conclusions; References; 5 Prospects for Pulsar Wind Nebulae Observations with γ-Ray Astronomy Facilities: Cherenkov Telescope Array and Satellites
5.1 Introduction: An Overview of the Next ``gamma'' Decade5.2 The Future of VHE Astronomy: CTA; 5.3 The Impact of CTA on the Physics of PWN; 5.3.1 CTA Galactic Plane Survey: A Key Science Program; 5.3.2 CTA Energy Dependent Morphology and PWN Identification; 5.3.3 CTA, Crab, and Its Flares; 5.4 Space-Borne Detectors; 5.4.1 Improvement in Angular Resolutionand Polarimetric Capabilities; 5.4.2 Combining the Compton and the Pair-Production Detection Technique; 5.4.2.1 e-ASTROGAM; 5.4.2.2 ComPair; 5.5 The Importance of the MeVâ#x80;#x93;GeV Range for the Physics of PWN; 5.6 Summary; References
6 Crab Observational Status: Nebulae, Pulsations, and Flares6.1 Introduction; 6.2 Crab Pulsar; 6.2.1 The Rotational Frequency; 6.2.2 Pulse Profile; 6.2.3 Polarization; 6.2.4 Giant Pulses; 6.2.5 Spectral Measurements; 6.2.6 Lessons from the Crab Pulsar Observations; 6.3 Crab Nebula; 6.3.1 The "Halo'' and the Cage; 6.3.2 Morphological Measurements; 6.3.3 Spectral Measurements; 6.3.4 The Gamma-Ray Flares; 6.3.5 Polarization Measurements; 6.3.6 Lessons on the Crab Nebula; References; 7 Pulsar Striped Winds; 7.1 Introduction; 7.1.1 General Picture; 7.1.2 Problems; 7.2 MHD Picture: Striped Winds