This is an image of the central region of the Vela supernova remnant,
showing emission created by ``winds'' from the active dead star (a pulsar) at the heart of
the remnant.
This image is in so-called ``polarised
emission'', where we measure the tendency for the radio waves to oscillate
in a preferred direction. In Vela, the preferred direction is caused
by a strong magnetic field.
The ``cracks'' in the image
are regions where the preferred direction of oscillation is scrambled by
visps of intervening material.
ATCA 21cm continuum image by D. Bock, R. Sault,
A. Green and D. Milne.
Original: Bob Sault (1-Jan-2003)
Modified: Bob Sault (1-Jan-2003)
