Yinghan Mao, Nanjing University, China, and University of Amsterdam, The Netherlands — July 29, 2026

Pulse profile modeling (PPM) is a relativistic ray-tracing technique that enables neutron star mass and radius measurements, providing key constraints on the equation of state of dense matter. While successfully applied to rotation-powered millisecond pulsars, its application to accreting millisecond X-ray pulsars (AMXPs) remains challenging due to complex accretion environments. In this talk, I will introduce the PPM framework and review recent developments in adapting these models for AMXPs, including my work on modeling disk occultation. I will then present recent studies of two AMXPs, SAX J1808.4−3658 and J144459.2−604207, using NICER timing and IXPE polarimetric observations. Finally, I will discuss future directions for advancing PPM models and the opportunity offered by next-generation X-ray missions such as eXTP.