The X‐Ray Structure and Spectrum of the Pulsar Wind Nebula Surrounding PSR B1853+01 in W44 | Zendy

Robert Petre | Zendy; K. D. Küntz | Zendy; R. L. Shelton | Zendy

AI Assistant Blog Pricing

Home ZAIA Blog

Open Access

The X‐Ray Structure and Spectrum of the Pulsar Wind Nebula Surrounding PSR B1853+01 in W44

Author(s) -

Robert Petre,

K. D. Küntz,

R. L. Shelton

Publication year - 2002

Publication title -

the astrophysical journal

Language(s) - English

Resource type - Journals

SCImago Journal Rank - 2.376

H-Index - 489

eISSN - 1538-4357

pISSN - 0004-637X

DOI - 10.1086/342672

Subject(s) - pulsar wind nebula , physics , pulsar , astrophysics , nebula , supernova remnant , spectral index , acis , emission nebula , flux (metallurgy) , astronomy , supernova , spectral line , stars , materials science , metallurgy

We present the result of a Chandra ACIS observation of the pulsar PSRB1853+01 and its associated pulsar wind nebula (PWN), embedded within thesupernova remnant W44. A hard band ACIS map cleanly distinguishes the PWN fromthe thermal emission of W44. The nebula is extended in the north-southdirection, with an extent about half that of the radio emission. Morphologicaldifferences between the X-ray and radio images are apparent. Spectral fittingreveals a clear difference in spectral index between the hard emission from PSRB1853+01 (Gamma ~ 1.4) and the extended nebula (Gamma ~ 2.2). The more accuratevalues for the X-ray flux and spectral index are used refine estimates for PWNparameters, including magnetic field strength, the average Lorentz factor,gamma, of the particles in the wind, the magnetization parameter, sigma, andthe ratio k of electrons to other particles.Comment: 10 pages, 3 figures, accepted by Ap

The content you want is available to Zendy users.

Already have an account? Click here to sign in.

Having issues? You can contact us here

Accelerating Research