A Refined Analytic Oblate--Schwarzschild Model for Thermal X-Ray Pulse Profiles of Rotating Neutron Stars
Abstract
Thermal X-ray pulse profiles constrain neutron-star masses and radii through the effects of gravitational light bending and rotation on surface emission. The precision anticipated from the enhanced X-ray Timing and Polarimetry (eXTP) mission motivates more accurate analytic light-bending formulae that retain the efficiency needed for repeated model evaluations. We derive a refined analytic flux expression within the oblate--Schwarzschild (OS) approximation that combines bending, propagation-delay, and lensing approximations with a spheroidal surface. We compare its profiles with numerical Schwarzschild and second-order Hartle--Thorne ray tracing on the same spheroidal surfaces. The comparisons use a selected two-spot configuration at 300 Hz with isotropic blackbody emission and three choices for surface eccentricity: a freely specified value, the Maclaurin relation for a uniformly rotating Newtonian fluid, and a fit to rotating-neutron-star surfaces. Across these cases, the refined OS profiles have RMS flux differences of 1.76−1.98% relative to the Hartle--Thorne reference, compared with 6.50−21.39% for the spherical Schwarzschild-plus-Doppler (S+D) model. All differences are normalized to the phase-averaged reference flux. The corresponding differences between Schwarzschild and Hartle--Thorne ray tracing remain below 1.1%. These comparisons separate errors in analytic photon transfer from the effects of surface deformation and the rotating exterior spacetime. For the configurations examined, accounting for oblateness substantially improves agreement with ray tracing. The model retains the speed of an analytic calculation while making the physical origin of profile changes explicit.
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BibTeX
@misc{yang2026refined,
title = {{A Refined Analytic Oblate--Schwarzschild Model for Thermal X-Ray Pulse Profiles of Rotating Neutron Stars}},
author = {Xi Yang and Tong Zhao and Renxin Xu},
howpublished = {arXiv},
year = {2026},
month = oct,
doi = {10.48550/arxiv.2610.02653},
eprint = {2610.02653},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2610.02653},
note = {CC BY-NC-ND 4.0},
}
RIS
TY - UNPB
TI - A Refined Analytic Oblate--Schwarzschild Model for Thermal X-Ray Pulse Profiles of Rotating Neutron Stars
AU - Xi Yang
AU - Tong Zhao
AU - Renxin Xu
PY - 2026
DA - 2026/10/02
PB - arXiv
DO - 10.48550/arxiv.2610.02653
UR - https://arxiv.org/abs/2610.02653
AB - Thermal X-ray pulse profiles constrain neutron-star masses and radii through the effects of gravitational light bending and rotation on surface emission. The precision anticipated from the enhanced X-ray Timing and Polarimetry (eXTP) mission motivates more accurate analytic light-bending formulae that retain the efficiency needed for repeated model evaluations. We derive a refined analytic flux expression within the oblate--Schwarzschild (OS) approximation that combines bending, propagation-delay, and lensing approximations with a spheroidal surface. We compare its profiles with numerical Schwarzschild and second-order Hartle--Thorne ray tracing on the same spheroidal surfaces. The comparisons use a selected two-spot configuration at 300 Hz with isotropic blackbody emission and three choices for surface eccentricity: a freely specified value, the Maclaurin relation for a uniformly rotating Newtonian fluid, and a fit to rotating-neutron-star surfaces. Across these cases, the refined OS profiles have RMS flux differences of 1.76−1.98% relative to the Hartle--Thorne reference, compared with 6.50−21.39% for the spherical Schwarzschild-plus-Doppler (S+D) model. All differences are normalized to the phase-averaged reference flux. The corresponding differences between Schwarzschild and Hartle--Thorne ray tracing remain below 1.1%. These comparisons separate errors in analytic photon transfer from the effects of surface deformation and the rotating exterior spacetime. For the configurations examined, accounting for oblateness substantially improves agreement with ray tracing. The model retains the speed of an analytic calculation while making the physical origin of profile changes explicit.
ER -