The Pulsar Wind Nebula of G11.2-0.3

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dc.creatorRoberts, M. S. E.
dc.creatorTam, C.
dc.creatorKaspi, V. M.
dc.creatorLyutikov, M.
dc.creatorGotthelf, E. V.
dc.creatorVasisht, G.
dc.creatorKawai, N.
dc.date2001-12-03
dc.date.accessioned2026-07-07T02:01:39Z
dc.date.available2026-07-07T02:01:39Z
dc.descriptionWe present high-resolution radio and X-ray studies of the composite supernova remnant G11.2-0.3. Using archival VLA data, we perform radio spectral tomography to measure for the first time the spectrum of the shell and plerion separately. We compare the radio morphology of each component to that observed in the hard and soft Chandra X-ray images. We measure the X-ray spectra of the shell and the emission in the interior and discuss the hypothesis that soft X-ray emission interior to the shell is the result of the expanding pulsar wind shocking with the supernova ejecta. We also see evidence for spatial variability in the hard X-ray emission near the pulsar, which we discuss in terms of ion mediated relativistic shocks.
dc.description4 pages, 2 figures, To appear in "Neutron Stars in Supernova Remnants" (ASP Conference Proceedings), eds P. O. Slane and B. M. Gaensler
dc.identifierhttps://arxiv.org/abs/astro-ph/0112053
dc.identifierhttp://arxiv.org/abs/astro-ph/0112053
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/3831
dc.subjectAstrophysics
dc.titleThe Pulsar Wind Nebula of G11.2-0.3
dc.typetext

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