Colloquium: Measuring the neutron star equation of state using x-ray timing
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 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.more »
- Authors:
-
- Univ. of Amsterdam, Amsterdam (The Netherlands)
- Univ. of Southamption, Southampton (United Kingdom)
- Massachusetts Inst. of Technology (MIT), Cambridge, MA (United States)
- INAF/IASF Roma, Roma (Italy); INFN, Sezione di Roma Tor Vergata, Roma (Italy)
- Technische Univ. Darmstadt, Darmstadt (Germany), ExtreMe Matter Institute EMMI, GSI Helmholtzzentrum fur Schwerionenforschung GmbH, Darmstadt (Germany)
- INAF/OAR, Roma (Italy)
- Univ. of Illinois at Urbana-Champaign, Urbana, IL (United States)
- Univ. of Maryland, College Park, MD (United States)
- Univ. of Alberta, Edmonton, AB (Canada)
- Univ. of Arizona, Tucson, AZ (United States)
- Univ. of Leiden, Leiden (The Netherlands)
- Univ. of Turku, Piikkio (Finland)
- Technische Univ. Darmstadt, Darmstadt (Germany); ExtreMe Matter Institute EMMI, GSI Helmholtzzentrum fur Schwerionenforschung GmbH, Darmstadt (Germany)
- Univ. of Tennessee, Knoxville, TN (United States); Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States)
- Instituto de Ciencias del Espacio (IEEC-CSIC), Cerdanyola del Valles (Spain)
- Publication Date:
- Research Org.:
- Oak Ridge National Laboratory (ORNL), Oak Ridge, TN (United States)
- Sponsoring Org.:
- USDOE
- OSTI Identifier:
- 1331087
- Alternate Identifier(s):
- OSTI ID: 1247243
- Grant/Contract Number:
- AC05-00OR22725; PCIG09-GA-2011-291679; COST Action MP1304
- Resource Type:
- Accepted Manuscript
- Journal Name:
- Reviews of Modern Physics
- Additional Journal Information:
- Journal Volume: 88; Journal Issue: 2; Journal ID: ISSN 0034-6861
- Publisher:
- American Physical Society
- Country of Publication:
- United States
- Language:
- English
- Subject:
- 46 INSTRUMENTATION RELATED TO NUCLEAR SCIENCE AND TECHNOLOGY
Citation Formats
Watts, Anna L., Andersson, Nils, Chakrabarty, Deepto, Feroci, Marco, Hebeler, Kai, Israel, Gianluca, Lamb, Frederick K., Miller, M. Coleman, Morsink, Sharon, Ozel, Feryal, Patruno, Alessandro, Poutanen, Juri, Psaltis, Dimitrios, Schwenk, Achim, Steiner, Andrew W., Stella, Luigi, Tolos, Laura, and van der Klis, Michiel. Colloquium: Measuring the neutron star equation of state using x-ray timing. United States: N. p., 2016.
Web. doi:10.1103/RevModPhys.88.021001.
Watts, Anna L., Andersson, Nils, Chakrabarty, Deepto, Feroci, Marco, Hebeler, Kai, Israel, Gianluca, Lamb, Frederick K., Miller, M. Coleman, Morsink, Sharon, Ozel, Feryal, Patruno, Alessandro, Poutanen, Juri, Psaltis, Dimitrios, Schwenk, Achim, Steiner, Andrew W., Stella, Luigi, Tolos, Laura, & van der Klis, Michiel. Colloquium: Measuring the neutron star equation of state using x-ray timing. United States. https://doi.org/10.1103/RevModPhys.88.021001
Watts, Anna L., Andersson, Nils, Chakrabarty, Deepto, Feroci, Marco, Hebeler, Kai, Israel, Gianluca, Lamb, Frederick K., Miller, M. Coleman, Morsink, Sharon, Ozel, Feryal, Patruno, Alessandro, Poutanen, Juri, Psaltis, Dimitrios, Schwenk, Achim, Steiner, Andrew W., Stella, Luigi, Tolos, Laura, and van der Klis, Michiel. Wed .
"Colloquium: Measuring the neutron star equation of state using x-ray timing". United States. https://doi.org/10.1103/RevModPhys.88.021001. https://www.osti.gov/servlets/purl/1331087.
@article{osti_1331087,
title = {Colloquium: Measuring the neutron star equation of state using x-ray timing},
author = {Watts, Anna L. and Andersson, Nils and Chakrabarty, Deepto and Feroci, Marco and Hebeler, Kai and Israel, Gianluca and Lamb, Frederick K. and Miller, M. Coleman and Morsink, Sharon and Ozel, Feryal and Patruno, Alessandro and Poutanen, Juri and Psaltis, Dimitrios and Schwenk, Achim and Steiner, Andrew W. and Stella, Luigi and Tolos, Laura and van der Klis, Michiel},
abstractNote = {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.},
doi = {10.1103/RevModPhys.88.021001},
journal = {Reviews of Modern Physics},
number = 2,
volume = 88,
place = {United States},
year = {Wed Apr 13 00:00:00 EDT 2016},
month = {Wed Apr 13 00:00:00 EDT 2016}
}
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