The Impact of Errors in the Shape Function of Rotating Neutron Stars in the Oblate Schwarzschild Approximation

@misc{ngo2026impact,
  title = {{The Impact of Errors in the Shape Function of Rotating Neutron Stars in the Oblate Schwarzschild Approximation}},
  author = {John Ming Ngo and Charlee Amason and Sharon M. Morsink},
  howpublished = {arXiv},
  year = {2026},
  month = oct,
  doi = {10.48550/arxiv.2608.27744},
  eprint = {2608.27744},
  archivePrefix = {arXiv},
  url = {https://arxiv.org/abs/2608.27744},
  note = {CC BY-SA 4.0},
}

TY  - UNPB
TI  - The Impact of Errors in the Shape Function of Rotating Neutron Stars in the Oblate Schwarzschild Approximation
AU  - John Ming Ngo
AU  - Charlee Amason
AU  - Sharon M. Morsink
PY  - 2026
DA  - 2026/10/16
PB  - arXiv
DO  - 10.48550/arxiv.2608.27744
UR  - https://arxiv.org/abs/2608.27744
AB  - Measurements of thermal X-ray flux emitted by neutron stars can constrain their radii and the equation of state of cold dense matter. Accurate flux modeling of rapidly rotating neutron stars requires an approximation for their oblate surface shape, usually given by a shape function. We examine the accuracy of five shape functions by comparing them against numerical relativistic stellar surfaces for seven representative equations of state over a broad range of compactness and spin. We characterize their errors in the surface radius and their derivative with respect to colatitude, test the extent of quasi-universality, and propagate these errors into the differential solid angle dΩ, a geometric factor underlying the observed flux, under the oblate Schwarzschild approximation. We find that the shape functions produce distinct error patterns associated with their forms and parameter ranges. These errors remain structured in compactness, spin, and colatitude. Simple polynomial corrections substantially reduce the radius errors of several shape functions, with most corrected errors within approximately 0.5%. We show that errors in dΩ may be understood as coming from an area contribution, which scales with twice the relative radius error, and a projection contribution controlled primarily by the error in the surface derivative. The projection contribution grows towards the limb, where small surface errors can produce much larger local errors in dΩ. We provide a set of guidelines for the construction of improved quasi-universal shape functions that can be used in future radius estimation efforts. Our recommendations include that both the shape and its derivative be modeled accurately, that more accurate predictions of the polar radius be developed, and that the shape function be calibrated over the same compactness-spin range that is to be tested.
ER  -