  Over the last few years X-ray observations of broad-line radio galaxies
(BLRGs) by ASCA, RXTE and BeppoSAX have shown that these objects seem to
exhibit weaker X-ray reflection features (such as the iron K\alpha line) than
radio-quiet Seyferts. This has lead to speculation that the optically-thick
accretion disc in radio-loud active galactic nuclei (AGN) may be truncated to
an optically-thin flow in the inner regions of the source. Here, we propose
that the weak reflection features are a result of reprocessing in an ionized
accretion disc. This would alleviate the need for a change in accretion
geometry in these sources. Calculations of reflection spectra from an ionized
disc for situations expected in radio-loud AGN (high accretion rate,
moderate-to-high black hole mass) predict weak reprocessing features. This idea
was tested by fitting the ASCA spectrum of the bright BLRG 3C 120 with the
constant density ionized disc models of Ross & Fabian. A good fit was found
with an ionization parameter of \xi ~4000 erg cm s^{-1} and the reflection
fraction fixed at unity. If observations of BLRGs by XMM-Newton show evidence
for ionized reflection then this would support the idea that a high accretion
rate is likely required to launch powerful radio jets.
