出版社：SISSA, Scuola Internazionale Superiore di Studi Avanzati
摘要：The main goal of our present work is to provide, for the first time, a simple computational tool
that can be used to compute the brightness, the spectral index, the polarization, the time variability
and the spectrum of the non-thermal light (both synchrotron and inverse Compton, IC) associated
with the plasma dynamics resulting from given relativistic magnetohydrodynamics(RMHD) simulations.
The proposed method is quite general, and can be applied to any scheme for RMHD and
to all non-thermal emitting sources, e.g. the pulsar wind nebulae (PWNe), and in particular to
the Crab Nebula (CN) as in the present proceeding. It is here analyzed in detail only the linear
optical and X-ray polarization that characterizes the PWNe synchrotron emission in order to infer
information on the inner bulk flow structure, to provide a direct investigation of the magnetic
field configuration, in particular the presence and the strength of a poloidal component, and to
understand the origin of some emitting features, such as the knot, whose origins are still uncertain.
Future work will be necessary to obtain polarization maps in the hard X- and gamma-rays
to compare with the actual observations by Integral/IBIS [7]. The complete investigation of the
dynamics and synchrotron emission can be found in [5]. In [22] the inverse Compton radiation
is treated to disentangle the different contributions to radiation from the magnetic field and the
particle energy distribution function, and to search for a possible hadronic component in the emitting
PWN, and thus for the presence of ions in the wind. If hadronic radiation was found in a
PWN, young supernova remnants would provide a natural birth-place of the cosmic-rays around
the knee.
