The Long-stable Hard State of XTE J1752-223 and the Disk Truncation Dilemma

The degree to which the thin accretion disks of black hole X-ray binaries are truncated during hard spectral states remains a contentious open question in astrophysics. During its singular observed outburst $2009\mbox{--}2010$, binary XTE J1752-223 spent $\sim1$~month long-stable state at luminosity $\sim0.02\mbox{--}0.1~L_{\rm Edd}$. It was with 56 RXTE pointings this period, simultaneous Swift-XRT daily coverage first 10 days observations. Whilst reflection modeling has been extensively explored analysis these data, there is disagreement surrounding geometry disk and corona implied by features. We re-examine combined, high signal-to-noise, Swift observations, perform extensive latest relxill suite models, including newer density models. show that requires be within $\sim5~R_{\rm ISCO}$ state, whilst weaker constraints from thermal emission imply higher truncation ($R_{\rm in}=6\mbox{--}80~R_{\rm ISCO}$). also explore more complex coronal continuum allowing for two Comptonization components instead one, features still require only mildly disk. Finally we present full comparison our results previous found analyses same dataset.