2008/06/30 by D. A. Leahy, Denis A. Leahy, Sharon M. Morsink +2 · 52 citations
Earth and Planetary Sciences · Physics and Astronomy · #Accretion (finance) #Astrophysical Phenomena and Observations #Astrophysics #Black-body radiation #Equation of state #High-pressure geophysics and materials #Isotropy #Light curve #Neutron star #Nuclear physics #Optics #Physics #Pulsar #Pulsars and Gravitational Waves Research #RADIUS #Radiation #Star (game theory) #astro-ph
paper · pdf · doi:10.1088/0004-637x/691/2/1235
published in The Astrophysical Journal 691(2), 1235-1242 (IOP Publishing) · 8 pages, 5 figures. Accepted by ApJ. Changes suggested by referee included
arxiv created 2008/09/29 · openalex publication_date 2009/02/01 · arxiv updated 2011/02/11 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
The accretion-powered (non–X-ray burst) pulsations of XTE J1814−338 are modeled to determine neutron star parameters and their uncertainties. The model is a rotating circular hot spot and includes: (1) an isotropic blackbody spectral component; (2) an anisotropic Comptonized spectral component; (3) relativistic time delays and light bending; and (4) the oblate shape of the star due to rotation. This model is the simplest possible model that is consistent with the data. The resulting best-fit parameters of the model favor stiff equations of state (EOS), as can be seen from the 3σ allowed regions in the mass–radius diagram. We analyzed all data combined from a 23 day period of the 2003 outburst, and separately analyzed data from two days of the outburst. The allowed mass–radius regions for both cases only allow EOS that are stiffer than the EOS of Akmal and colleagues, consistent with the large mass that has been inferred for the pulsar NGC 6440B. The stiff EOS inferred by this analysis is not compatible with the soft EOS inferred from a similar analysis of SAX J1808.