Abstract:
In the binary radio pulsar system J0737-3039 the faster pulsar A is
eclipsed once per orbit while the slower pulsar B shows orbital-dependent
variations of intensity. This gives us an exceptional opportunity to study
inner magnetospheres of neutron stars and their winds. We construct a
model of eclipses which reproduces the observed light curve up to
intricate details and proves the long standing assumption of dipolar
magnetic fields of neutron stars. In addition, interaction of pulsar B
magnetosphere with pulsar A wind produces orbital variations of observed B
intensity.