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The coevolution of T Tauri stars and their surrounding protoplanetary disksdictates the timescales of planet formation. In this paper, we presentmagnetospheric accretion and inner disk wall model fits to NUV-NIR spectra ofnine classical T Tauri stars in Orion OB1b as part of the Outflows and Disksaround Young Stars: Synergies for the Exploration of ULLYSES Spectra (ODYSSEUS)Survey. Using NUV-optical spectra from the Hubble UV Legacy Library of YoungStars as Essential Standards (ULLYSES) Director's Discretionary Program andoptical-NIR spectra from the PENELLOPE VLT Large Programme, we find that theaccretion rates of these targets are relatively high for the region'sintermediate age of 5.0 Myr; rates range from $0.5-17.2 \times 10^{-8}$M$_{\odot}$/yr, with a median value of $1.2\times 10^{-8}$ M$_{\odot}$/yr. TheNIR excesses can be fit with 1200-1800 K inner disk walls located at 0.05-0.10AU from the host stars. We discuss the significance of the choice in extinctionlaw, as the measured accretion rate depends strongly on the adopted extinctionvalue. This analysis will be extended to the complete sample of T Tauri starsbeing observed through ULLYSES to characterize accretion and inner disks instar-forming regions of different ages and stellar populations.

Towards a comprehensive view of accretion, inner disks, and extinction in classical T Tauri stars: an ODYSSEUS study of the Orion OB1b association