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Measuring the neutron star equation of state using X-ray timing

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arxiv 1602.01081 v1 pith:FTEOUKMJ submitted 2016-02-02 astro-ph.HE astro-ph.SRnucl-th

Anna L. Watts , Nils Andersson , Deepto Chakrabarty , Marco Feroci , Kai Hebeler , Gianluca Israel , Frederick K. Lamb , M. Coleman Miller
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Sharon Morsink Feryal Özel Alessandro Patruno Juri Poutanen Dimitrios Psaltis Achim Schwenk Andrew W. Steiner Luigi Stella Laura Tolos Michiel van der Klis
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classification astro-ph.HEastro-ph.SRnucl-th
keywords neutronstarsequationmatterradiusstarstatex-ray
verification ladder T0 review T1 audit T2 compute T3 formal
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abstract

One of the primary science goals of the next generation of hard X-ray timing instruments is to determine the equation of state of the matter at supranuclear densities inside neutron stars, by measuring the radius of neutron stars with different masses to accuracies of a few percent. Three main techniques can be used to achieve this goal. The first involves waveform modelling. The flux we observe from a hotspot on the neutron star surface offset from the rotational pole will be modulated by the star's rotation, giving rise to a pulsation. Information about mass and radius is encoded into the pulse profile via relativistic effects, and tight constraints on mass and radius can be obtained. The second technique involves characterising the spin distribution of accreting neutron stars. The most rapidly rotating stars provide a very clean constraint, since the mass-shedding limit is a function of mass and radius. However the overall spin distribution also provides a guide to the torque mechanisms in operation and the moment of inertia, both of which can depend sensitively on dense matter physics. The third technique is to search for quasi-periodic oscillations in X-ray flux associated with global seismic vibrations of magnetars (the most highly magnetized neutron stars), triggered by magnetic explosions. The vibrational frequencies depend on stellar parameters including the dense matter equation of state. We illustrate how these complementary X-ray timing techniques can be used to constrain the dense matter equation of state, and discuss the results that might be expected from a 10m$^2$ instrument. We also discuss how the results from such a facility would compare to other astronomical investigations of neutron star properties. [Modified for arXiv]

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Forward citations

Cited by 7 Pith papers

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