Determining Neutron Star Properties by Fitting Oblate-Star Waveform Models to X-Ray Burst Oscillations

Miller, M. Coleman; Lamb, Frederick K.

doi:10.1088/0004-637x/808/1/31

Cited by 73 publications

(78 citation statements)

References 55 publications

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“…This range is consistent with previous findings (e.g., Hebeler et al , 2013). Besides, note that the knowledge of oblateness of a spinning compact star may be important to understand its physics, and to constrain its EoS models using various techniques (e.g., Miller & Lamb , 2015;Bauböck et al , 2013). The R p /R e value, which determines the oblateness, decreases with increasing spin rate.…”

Section: Properties Of Millisecond Pulsarssupporting

confidence: 90%

Millisecond radio pulsars with known masses: Parameter values and equation of state models

et al. 2017

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The recent fast growth of a population of millisecond pulsars with precisely measured mass provides an excellent opportunity to characterize these compact stars at an unprecedented level. This is because the stellar parameter values can be accurately computed for known mass and spin rate and an assumed equation of state (EoS) model. For each of the 16 such pulsars and for a set of EoS models from nucleonic, hyperonic, strange quark matter and hybrid classes, we numerically compute fast spinning stable stellar parameter values considering the full effect of general relativity. This first detailed catalogue of the computed parameter values of observed millisecond pulsars provides a testbed to probe the physics of compact stars, including their formation, evolution and EoS. We estimate uncertainties on these computed values from the uncertainty of the measured mass, which could be useful to quantitatively constrain EoS models. We note that the largest value of the central density ρ c in our catalogue is ∼ 5.8 times the nuclear saturation density ρ sat , which is much less than the expected maximum value 13ρ sat . We argue that the ρ c -values of at most a small fraction of compact stars could be much larger than 5.8ρ sat . Besides, we find that the constraints on EoS models from accurate radius measurements could be significantly biased for some of our pulsars, if stellar spinning configurations are not used to compute the theoretical radius values.

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Section: Properties Of Millisecond Pulsarssupporting

confidence: 90%

Millisecond radio pulsars with known masses: Parameter values and equation of state models

et al. 2017

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“…For example, the future PREX-II [116,117]) experiments aim to accurately measure the neutron skin thickness of heavy nuclei that correlates with the pressure/stiffness of neutron-rich matter at or below saturation density; modern computations based on chiral effective field theory [107] and quantum Monte Carlo methods [110] hold the promise of improving the uncertainty analysis in the nuclear EoS at 1-2 times the saturation density. Moreover, forthcoming results from NICER would provide complementary constraints on the NS radii [118,119] which could help serve as prior information for the analysis of GW data [120].…”

Section: Discussionmentioning

confidence: 99%

Studying strong phase transitions in neutron stars with gravitational waves

2020

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The composition of neutron stars at the extreme densities reached in their cores is currently unknown. Besides nuclear matter of normal neutrons and protons, the cores of neutron stars might harbor exotic matter such as deconfined quarks. In this paper we study strong hadron-quark phase transitions in the context of gravitational wave observations of inspiraling neutron stars. We consider upcoming detections of neutron star coalescences and model the neutron star equations of state with phase transitions through the Constant-Speed-of-Sound parametrization. We use the fact that neutron star binaries with one or more hadron-quark hybrid stars can exhibit qualitatively different tidal properties than binaries with hadronic stars of the same mass, and hierarchically model the masses and tidal properties of simulated populations of binary neutron star inspiral signals. We explore the parameter space of phase transitions and discuss under which conditions future observations of binary neutron star inspirals can identify this effect and constrain its properties, in particular the threshold density at which the transition happens and the strength of the transition. We find that if the detected population of binary neutron stars contains both hadronic and hybrid stars, the onset mass and strength of a sufficiently strong phase transition can be constrained with 50-100 detections. If the detected neutron stars are exclusively hadronic or hybrid, then it is possible to place lower or upper limits on the transition density and strength.

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“…Moreover, they encode information of the spacetime curvature around the star and thereby of the bulk properties of the star. One of the main goals of the ongoing Neutron star Interior Composition ExploreR (NICER) [15][16][17] mission, is to measure light curves from a number of sources with unprecedented time-resolution, constraining their masses and radii within 5−10% accuracy in optimal cases [18][19][20] (see also e.g. [21][22][23]).…”

Section: Introductionmentioning

confidence: 99%

Finite size effects on the light curves of slowly-rotating neutron stars

2019

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An important question when studying the light curves produced by hot spots on the surface of rotating neutron stars is, how might the shape of the light curve be affected by relaxing some of the simplifying assumptions that one would adopt on a first treatment of the problem, such as that of a point-like spot. In this work we explore the dependence of light curves on the size and shape of a single hot spot on the surface of slowly-rotating neutron stars. More specifically, we consider two different shapes for the hot spots (circular and annular) and examine the resulting light curves as functions of the opening angle of the hot spot (for both) and width (for the latter). We find that the point-like approximation can describe light curves reasonably well, if the opening angle of the hot spot is less than ∼ 5 • . Furthermore, we find that light curves from annular spots are almost the same as those of the full circular spot if the opening angle is less than ∼ 35 • independently of the hot spot's width.

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Determining Neutron Star Properties by Fitting Oblate-Star Waveform Models to X-Ray Burst Oscillations

Cited by 73 publications

References 55 publications

Millisecond radio pulsars with known masses: Parameter values and equation of state models

Millisecond radio pulsars with known masses: Parameter values and equation of state models

Studying strong phase transitions in neutron stars with gravitational waves

Finite size effects on the light curves of slowly-rotating neutron stars

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