X-rays from reconnection in pulsar winds

Details X-rays from reconnection in pulsar winds X-rays from reconnection in pulsar winds

Aug 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001icrc....6.2418k&link_type=abstract

Proceedings of the 27th International Cosmic Ray Conference. 07-15 August, 2001. Hamburg, Germany. Under the auspices of the Int

Physics

Scientific paper

The rotational energy of a pulsar is most likely carried away by a relativistic MHD wind. Near the equatorial plane, such a wind should exhibit a striped structure in which regions of opposite magnetic polarity are separated by cur-rent sheets. Using a recent model of the reconnection rate in these sheets, we estimate the synchrotron radiation which they emit. For sufficiently fast winds, this radiation is observed in a pulse/interpulse pattern. We compare our com-putations with observations of rotationally powered Xray and optical pulsars.

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