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V. Kaspi (McGill University), M. Pivovaroff (Thermawave Inc.), G. Gaensler (MIT), N. Kawai (RIKEN), J. Arons (UC Berkeley), K. Tamura (RIKEN)
The Chandra X-ray Observatory has provided spectacular images of the two most famous young, energetic pulsars, the Crab and Vela. In particular, it has revealed a wealth of structure near the pulsar, including collimated outflows, bow shocks, and torii, with morphology correlated with the pulsar proper motion. These features currently defy explanation in conventional models of pulsar wind physics. Whether such properties are ubiquitous among young pulsars is simply not known. Here we present the results of a 20 ks observation of a third young, energetic radio pulsar PSR B1509-58, and its associated supernova remnant G320.4-1.2, obtained with the ACIS instrument aboard the Chandra X-ray Observatory. As with the other two pulsars, Chandra has revealed previously unresolved structure near the pulsar that strongly argues that such features are common to all pulsars. We will present preliminary spatial and spectral analyses of the pulsar and remnant, as well as discuss the nature of the proposed interaction of the pulsar with its surrounding supernova remnant.
This work is funded by the Smithsonian Astrophysical Observatory, NASA, NSF, and NSERC.
The author(s) of this abstract have provided an email address for comments about the abstract: vkaspi@physics.mcgill.ca