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Title: Colloquium: Measuring the neutron star equation of state using x-ray timing

Journal Article · · Reviews of Modern Physics
 [1];  [2];  [3];  [4];  [5];  [6];  [7];  [8];  [9];  [10];  [11];  [12];  [10];  [13];  [14];  [6];  [15];  [1]
  1. Univ. of Amsterdam, Amsterdam (The Netherlands)
  2. Univ. of Southamption, Southampton (United Kingdom)
  3. Massachusetts Inst. of Technology (MIT), Cambridge, MA (United States)
  4. INAF/IASF Roma, Roma (Italy); INFN, Sezione di Roma Tor Vergata, Roma (Italy)
  5. Technische Univ. Darmstadt, Darmstadt (Germany), ExtreMe Matter Institute EMMI, GSI Helmholtzzentrum fur Schwerionenforschung GmbH, Darmstadt (Germany)
  6. INAF/OAR, Roma (Italy)
  7. Univ. of Illinois at Urbana-Champaign, Urbana, IL (United States)
  8. Univ. of Maryland, College Park, MD (United States)
  9. Univ. of Alberta, Edmonton, AB (Canada)
  10. Univ. of Arizona, Tucson, AZ (United States)
  11. Univ. of Leiden, Leiden (The Netherlands)
  12. Univ. of Turku, Piikkio (Finland)
  13. Technische Univ. Darmstadt, Darmstadt (Germany); ExtreMe Matter Institute EMMI, GSI Helmholtzzentrum fur Schwerionenforschung GmbH, Darmstadt (Germany)
  14. Univ. of Tennessee, Knoxville, TN (United States); Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States)
  15. Instituto de Ciencias del Espacio (IEEC-CSIC), Cerdanyola del Valles (Spain)

One of the primary science goals of the next generation of hard x-ray timing instruments is to determine the equation of state of 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 modeling. The flux observed from a hotspot on the neutron star surface offset from the rotational pole will be modulated by the star s rotation, and this periodic modulation at the spin frequency is called a pulsation. As the photons propagate through the curved spacetime of the star, information about mass and radius is encoded into the shape of the waveform (pulse profile) via special and general-relativistic effects. Using pulsations from known sources (which have hotspots that develop either during thermo- nuclear bursts or due to channeled accretion) it is possible to obtain tight constraints on mass and radius. The second technique involves characterizing the spin distribution of accreting neutron stars. A large collecting area enables highly sensitive searches for weak or intermittent pulsations (which yield spin) from the many accreting neutron stars whose spin rates are not yet known. The most rapidly rotating stars provide a clean constraint, since the limiting spin rate where the equatorial surface velocity is comparable to the local orbital velocity, at which mass shedding occurs, 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 quasiperiodic 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, and large-area x-ray timing instruments would provide much improved detection capability. In addition, an illustration is given of how these complementary x-ray timing techniques can be used to constrain the dense matter equation of state and the results that might be expected from a 10 m2 instrument are discussed. Also discussed are how the results from such a facility would compare to other astronomical investigations of neutron star properties.

Research Organization:
Oak Ridge National Laboratory (ORNL), Oak Ridge, TN (United States)
Sponsoring Organization:
USDOE
Grant/Contract Number:
AC05-00OR22725; PCIG09-GA-2011-291679; COST Action MP1304
OSTI ID:
1331087
Alternate ID(s):
OSTI ID: 1247243
Journal Information:
Reviews of Modern Physics, Vol. 88, Issue 2; ISSN 0034-6861
Publisher:
American Physical SocietyCopyright Statement
Country of Publication:
United States
Language:
English
Citation Metrics:
Cited by: 216 works
Citation information provided by
Web of Science

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Equation-of-state dependence of the gravitational-wave signal from the ring-down phase of neutron-star mergers text January 2012
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Propagation of thermonuclear flames on rapidly rotating neutron stars: extreme weather during type I X-ray bursts text January 2001
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Formation of Resonant Atomic Lines during Thermonuclear Flashes on Neutron Stars text January 2005
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Fierz-complete NJL model study. II. Toward the fixed-point and phase structure of hot and dense two-flavor QCD text January 2018
Exterior spacetime of relativistic stars in scalar-Gauss-Bonnet gravity journal August 2019
Precision of Mass and Radius Determination for Neutron Stars from the ATHENA Mission journal January 2020
Neutron Star Mass-Radius Constraints using Evolutionary Optimization text January 2016
Neutron Stars in the Laboratory text January 2016
From hadrons to quarks in neutron stars: a review text January 2017
GW170817: Observation of Gravitational Waves from a Binary Neutron Star Inspiral text January 2017
On parametrised cold dense matter equation of state inference text January 2018
A pitfall of piecewise-polytropic equation of state inference text January 2018
Constraints on the equation of state from the stability condition of neutron stars text January 2018
Neutron star pulse profiles in scalar-tensor theories of gravity text January 2018
Dense matter with eXTP text January 2018
Equation of state sensitivities when inferring neutron star and dense matter properties text January 2018
Effects of Compton scattering on the neutron star radius constraints in rotation-powered millisecond pulsars text January 2019
Effect of viscosity and thermal conductivity on the radial oscillation and relaxation of relativistic stars text January 2019
Isovector Effects in Neutron Stars, Radii and the GW170817 Constraint text January 2019
Neutron skins of atomic nuclei: per aspera ad astra text January 2019
Neutron Star Matter as a Relativistic Fermi Liquid text January 2019

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