Free Access

Fig. 1


Cartoon representing a density map of the physical scenario: an inhomogeneous stellar wind interacts with the relativistic pulsar wind. The shocked stellar wind and the shocked pulsar wind are separated by a contact discontinuity. The distances are not to scale. The simulations presented in this paper only considered a stellar wind with one clump centered at the axis joinning the two stars.

Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.

Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.

Initial download of the metrics may take a while.