ABSTRACT:
Pulsars steadily loose their rotational energy via a magnetized
relativistic wind. The confinement of this wind by the surrounding
supernova ejecta or the interstellar medium generates a luminous
nebula of synchrotron emission called a pulsar wind nebula (PWN). I
will give a general introduction into structure and evolution of
pulsar wind nebulae and discuss examples of PWNe located inside and
outside of their host supernova remnant. I will then give an
overview of the PWN G63.7+1.1 and describe our planned JCMT
observations, with which we hope to detect molecular material
shocked by the expanding PWN.
Participating Organizations: