'Pulsar wind' presentation slideshows

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Pulsar wind nebulae and their interaction with the environments

Pulsar wind nebulae and their interaction with the environments. Fangjun Lu ??? Institute of High Energy Physics Chinese Academy of Sciences. Most of the spin-down power of a pulsar is not released through direct radiation. (Li, Lu, & Li 2008, ApJ 682, 1166).

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Pulsar Wind Nebulae at High Energies

Pulsar Wind Nebulae at High Energies. Stephen C.-Y. Ng HKU. Outline. What are pulsar wind nebulae? Physical properties and evolution Why study PWNe ? Common TeV sources, particle accelerators Multiwavelength observations of PWNe Broadband SED Surprise from Fermi : Crab flaring.

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Nick Camus Niccolo Bucciantini Philip Hughes Maxim Lyutikov

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Pulsar Wind Nebulae and Relativistic Shocks

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Structure and Evolution

Structure and Evolution. of Pulsar Wind Nebulae. Take In:. Pulsars are born as reservoirs of tremendous rotational energy Their strong magnetic fields and rapid rotation rates promote loss of rotational energy through formation of a relativistic magnetized wind

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Pulsar Wind Nebulae

Pulsar Wind Nebulae. http://www.astroscu.unam.mx/neutrones/home.html. Rotating magnetosphere generates E X B wind - direct particle acceleration as well, yielding (e.g. Michel 1969; Cheng, Ho, & Ruderman 1986). The Pulsar Wind Zone. Magnetic polarity in

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e-EVN science projects (2006-2008)

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Colliding winds in pulsar binaries

Colliding winds in pulsar binaries. S.V.Bogovalov 1 , A.V.Koldoba 2 ,G.V.Ustugova 2 , D. Khangulyan 3 , F.Aharonian 3 1-National Nuclear Research University (Moscow) 2-Institute of applied mathematics RAN (Moscow) 3-Max-Planck-Institute for Nuclear Physics (Heidelberg). Candidates.

345 views • 25 slides

Pulsar Winds and Jets

Pulsar Winds and Jets. Pat Slane (Harvard-Smithsonian Center for Astrophysics). Outline. Pulsar Winds and Their Nebulae Jet/Torus Structure in PWNe Observations of Pulsar Jets - Jet sizes and luminosities - Curved jets and instabilities

382 views • 25 slides

Supernova Remnants

Supernova Remnants. and GLAST. Reverse Shock. PWN Shock. Forward Shock. Pulsar Termination Shock. Pulsar Wind. Unshocked Ejecta. Shocked Ejecta. Shocked ISM. PWN. ISM. SNRs: The (very) Basic Structure. Pulsar Wind - sweeps up ejecta; shock decelerates

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Ya.N. Istomin P.N. Lebedev Physical Institute, Moscow, Russia

Low frequency observation of both pulsar wind and magnetodipole radiation from switch on-off pulsars. Ya.N. Istomin P.N. Lebedev Physical Institute, Moscow, Russia. What is the reason of a neutron star spin down?

285 views • 15 slides

Norita Kawanaka Kunihito Ioka & Mihoko M. Nojiri (KEK, Japan) Rencontres de Moriond 04/02/09

Continuous Injection of High Energy Positrons from an Astrophysical Object: Can a Pulsar Account for the Cosmic Ray Electron/Positron Data?. Norita Kawanaka Kunihito Ioka & Mihoko M. Nojiri (KEK, Japan) Rencontres de Moriond 04/02/09. Positron Excess: PAMELA.

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Chandra View of Pulsar Wind Nebulae Torii submitted to ApJ

Chandra View of Pulsar Wind Nebulae Torii submitted to ApJ. Contents: 1. Introduction 2. PWN torus and spin-down luminosity 3. Discussion and application. Aya Bamba ISAS/JAXA -> DIAS (Oct.01). 1. Introduction. Chandra discovered torii and jets of pulsar wind nebulae !!.

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Jamie Holder VERITAS Collaboration Bartol Research Institute/ University of Delaware

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Jamie Holder VERITAS Collaboration Bartol Research Institute/ University of Delaware

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Model of Radio Emission from Spherically Symmetric Pulsar Wind Nebulae

ABSTRUCT

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3D Crab Model and comparison with Chandra result

Presented at The IAU 8 th Asian-pacific regional meeting Tokyo Japan July 2-5, 2002. Pulsar Wind Nebulae and Particle Acceleration in the Pulsar Magnetosphere Shibata, S., Tomatsuri, H., Shimanuki, M., Saito, K., Nakamura, Y., Mori, K.*

83 views • 1 slides