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Pulsar wind nebulae of runaway massive stars

Abstract : A significant fraction of massive stars move at speed through the interstellar medium of galaxies. After their death as core-collapse supernovae, a possible final evolutionary state is that of a fast-rotating magnetized neutron star, shaping its circumstellar medium into a pulsar wind nebula. Understanding the properties of pulsar wind nebulae requires knowledge of the evolutionary history of their massive progenitors. Using two-dimensional magnetohydrodynamical simulations, we demonstrate that, in the context of a runaway high-mass red-supergiant supernova progenitor, the morphology of its subsequent pulsar wind nebula is strongly affected by the wind of the defunct progenitor star pre-shaping the stellar surroundings throughout its entire past life. In particular, pulsar wind nebulae of obscured runaway massive stars harbour asymmetries as a function of the morphology of the progenitor's wind-blown cavity, inducing projected asymmetric up-down synchrotron emission.
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Submitted on : Monday, July 4, 2022 - 3:02:53 PM
Last modification on : Friday, August 5, 2022 - 11:57:59 AM

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D. M. -A. Meyer, Z. Meliani. Pulsar wind nebulae of runaway massive stars. Monthly Notices of the Royal Astronomical Society: Letters, 2022, 515, pp.L29-L33. ⟨10.1093/mnrasl/slac062⟩. ⟨insu-03713225⟩



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