2013/05/31 by Dimitrios Psaltis, Feryal Özel, Feryal Ozel · 3 citations
Earth and Planetary Sciences · Physics and Astronomy · #Asteroseismology #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Atomic physics #Classical mechanics #Computational physics #Detector #Doppler effect #Geophysics and Gravity Measurements #Moment (physics) #Neutron #Neutron star #Nuclear physics #Optics #Physics #Pulsars and Gravitational Waves Research #Pulse (music) #Quadrupole #Quantum electrodynamics #Spin (aerodynamics) #Spinning #Stars #astro-ph.HE
paper · pdf · doi:10.1088/0004-637x/792/2/87
to appear in the Astrophysical Journal; typos corrected
openalex publication_date 2014/08/20 · arxiv created 2014/09/18 · arxiv updated 2015/06/16 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We present a new numerical algorithm for the calculation of pulse profiles from spinning neutron stars in the Hartle–Thorne approximation. Our approach allows us to formally take into account the effects of Doppler shifts and aberration, of frame dragging, as well as of the oblateness of the stellar surface and of its quadrupole moment. We confirm an earlier result that neglecting the oblateness of the neutron-star surface leads to ≃ 5%–30% errors in the calculated profiles and further show that neglecting the quadrupole moment of its spacetime leads to ≃ 1%–5% errors at a spin frequency of ≃ 600 Hz. We discuss the implications of our results for the measurements of neutron-star masses and radii with upcoming X-ray missions, such as NASA's NICER and ESA's LOFT.