Abstract
Pulsars are rapidly rotating compact cores left over from supernova explosions. They pour out pulsar winds containing relativistic magnetized particles which can form pulsar wind nebulae (PWNe) when shocked by ambient materials. These shocked particles emit synchrotron radiations with a power-law spectrum and linear polarization, making it possible to map the magnetic fields of PWNe. A PWN powered by a supersonically traveling pulsar can drive a bow shock in space. These bow-shock PWNe are ideals objects to study relativistic shocks and magnetohydrodynamics of pulsar winds. Previous studies suggest that the magnetic field configurations of PWNe may be related to space velocities of pulsars. To verify this hypothesis, we carried out radio observations of a PWN system IGR J11014−6103 which is traveling at a speed higher than 2000 km s−1, using the Australia Telescope Compact Array in 3 cm and 6 cm bands. In addition, radio observation can trace the integrated history of PWN systems since radio-emitting particles have a long synchrotron cooling time. I will present a preliminary 6 cm image of J11014 which shows a tail extending from the pulsar and it is much longer than the X-ray counterpart. Future works will also be discussed.
Anyone interested is welcome to attend.