English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

Hydrodynamical simulations are presented of a pulsar wind emitted by asupersonically moving pulsar. The pulsar moves through the interstellar mediumor, in the more interesting case, through the supernova remnant created at itsbirth event. In both cases there exists a three-fold structure consisting ofthe wind termination shock, contact discontinuity and a bow shock bounding thepulsar wind nebula. Using hydrodynamical simulations we study the behaviour ofthe pulsar wind nebula inside a supernova remnant, and in particular theinteraction with the outer shell of swept up interstellar matter and the blastwave surrounding the remnant. This interaction occurs when the pulsar breaksout of the supernova remnant. We assume the remnant is in the Sedov stage ofits evolution. Just before break-through, the Mach number associated with thepulsar motion equals ${\cal M}_{\rm psr} = 7/\sqrt{5}$, {\em independent} ofthe supernova explosion energy and pulsar velocity. The bow shock structure isshown to survive this break-through event.Comment: 7 pages, 9 figures, submitted to A&

Interaction of high-velocity pulsars with supernova remnant shells