  Vela Jr. (RX J0852.0$-$4622) is one of just a few known supernova remnants
(SNRs) with a resolved shell across the whole electromagnetic spectrum from
radio to very-high-energy ($>100$ GeV; VHE) gamma-rays. Its proximity and large
size allow for detailed spatially resolved observations of the source making
Vela Jr. one of the primary sources used for the study of particle acceleration
and emission mechanisms in SNRs. High-resolution X-ray observations reveal a
steepening of the spectrum toward the interior of the remnant. In this study we
aim for a self-consistent radiation model of Vela Jr. which at the same time
would explain the broadband emission from the source and its intensity
distribution. We solve the full particle transport equation combined with the
high-resolution 1D hydrodynamic simulations (using Pluto code) and subsequently
calculate the radiation from the remnant. The equations are solved in the test
particle regime. We test two models for the magnetic field profile downstream
of the shock: damped magnetic field which accounts for the damping of strong
magnetic turbulence downstream, and transported magnetic field. Neither of
these scenarios can fully explain the observed radial dependence of the X-ray
spectrum under spherical symmetry. We show, however, that the softening of the
spectrum and the X-ray intensity profile can be explained under the assumption
that the emission is enhanced within a cone.
