Modeling Phase-resolved Observations of the Surfaces of Magnetic Neutron Stars.pdf

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Modeling Phase-resolved Observations of the Surfaces of Magnetic Neutron Stars.pdf

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Modeling Phase-resolved Observations of the Surfaces of Magnetic Neutron Stars

a r X i v : 0 7 1 0 .1 6 6 3 v 1 [ a s t r o - p h ] 9 O c t 2 0 0 7 Modeling Phase-resolved Observations of the Surfaces of Magnetic Neutron Stars Wynn C. G. Ho ? and Kaya Mori ? ? Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA, 02138, USA ? Department of Astronomy and Astrophysics, University of Toronto, 50 St. George Street, Toronto, Ontario, M5S 3H4, Canada Abstract. Recent observations by XMM-Newton detected rotational pulsations in the total brightness and spectrum of several neutron stars. To properly interpret the data, accurate modeling of neutron star emission is necessary. Detailed analysis of the shape and strength of the rotational variations allows a measurement of the surface composition and magnetic field, as well as constrains the nuclear equation of state. We discuss our models of the spectra and light curves of two of the most observed neutron stars, RX J1856.5?3754 and 1E 1207.4?5209, and discuss some implications of our results and the direction of future work. Keywords: stars: atmospheres - stars: magnetic fields - stars: neutron - stars: rotation - X-rays: stars PACS: 97.60.Jd; 26.60.Kp; 95.30.Gv; 95.75.-z; 95.85.Nv; 97.10.-q INTRODUCTION Thermal radiation from the surface of neutron stars (NSs) can provide invaluable information on the physical prop- erties and evolution of NSs. NS properties, such as the mass M and radius R, in turn depend on the poorly constrained physics of the stellar interior, such as the nuclear equation of state (EOS) and quark and super- fluid/superconducting properties at supra-nuclear densi- ties. Many NSs are also known to possess strong mag- netic fields (B ～ 1012 ? 1013 G), with some well above the quantum critical value (B ? BQ ≡ 4.4×10 13 G). The observed thermal radiation originates in a thin at- mospheric layer (with scale height ～ 1 cm) that cov- ers the stellar surface. To properly interpret the obser- vations of NS surface emission and to provide accurate constraints on t