  We present an analysis of X-ray, Ultraviolet and optical/near-IR photometric
data of the transitional millisecond pulsar binary XSSJ12270-4859, obtained at
different epochs after the transition to a rotation-powered radio pulsar state.
The observations, while confirming the large-amplitude orbital modulation found
in previous studies after the state change, also reveal an energy dependence of
the amplitudes as well as variations on time scale of months. The amplitude
variations are anti-correlated in the X-ray and the UV/optical bands. The
average X-ray spectrum is described by a power law with \Gamma index of 1.07(8)
without requiring an additional thermal component. The power law index \Gamma
varies from 1.2 to 1.0 between superior and inferior conjunction of the neutron
star. We interpret the observed X-ray behaviour in terms of synchrotron
radiation emitted in an extended intrabinary shock, located between the pulsar
and the donor star, which is eclipsed due to the companion orbital motion. The
G5 type donor dominates the UV/optical and near-IR emission and is similarly
found to be heated up to ? 6500K as in the disc state. The analysis of optical
light curves gives a binary inclination 46 < i < 65deg and a mass ratio 0.11 <
q <0.26. The donor mass is found to be 0.15 < M2 < 0.36Msun for a neutron star
mass of 1.4Msun. The variations in the amplitude of the orbital modulation are
interpreted in terms of small changes in the mass flow rate from the donor
star. The spectral energy distribution from radio to gamma-rays is composed by
multiple contributions that are different from those observed during the
accretion-powered state.
