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Testing the Equation of State with Electromagnetic Observations

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The Physics and Astrophysics of Neutron Stars

Part of the book series: Astrophysics and Space Science Library ((ASSL,volume 457))

Abstract

Neutron stars are the densest, directly observable stellar objects in the universe and serve as unique astrophysical laboratories to study the behavior of matter under extreme physical conditions. This book chapter is devoted to describing how electromagnetic observations, particularly at X-ray, optical and radio wavelengths, can be used to measure the mass and radius of neutron stars and how this leads to constraints on the equation of state of ultra-dense matter. Having accurate theoretical models to describe the astrophysical data is essential in this effort. We will review different methods to constrain neutron star masses and radii, discuss the main observational results and theoretical developments achieved over the past decade, and provide an outlook of how further progress can be made with new and upcoming ground-based and space-based observatories.

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Notes

  1. 1.

    Initially the suggested method was using the assumption \(w=f_{\mathrm {c}}^{-1/4}\) and the observed curves \(K_{\mathrm {BB}}^{-1/4} - F_{\mathrm {BB}}\) were fitted with the model f c −  ones.

  2. 2.

    We note that the cooling-tail method is independent of distance: see Eq. (5.14).

  3. 3.

    The oscillations seen during the rise are thought to come from spreading of the burning front that is modulated by the neutron star spin period (e.g. Strohmayer et al. 1997), whereas the rapid variability seen during the cooling tails are thought to be associated with oscillatory behavior of the surface (“surface modes”; e.g. Muno et al. 2002; Piro and Bildsten 2005).

  4. 4.

    For reference, the pulsed fractions of other CCOs are ∼11% for RX J0822.0−4300 in SNR Puppis A, ∼9% for 1E 1207.4−5209 in SNR PKS 1209−51/52, and ∼64% for CXOU J185238.6+004020 in SNR Kes 79 (Gotthelf et al. 2013).

  5. 5.

    Although pile-up can be an issue when studying bursts with Athena (e.g. Keek et al. 2016).

  6. 6.

    http://xtreme.as.arizona.edu/NeutronStars

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Acknowledgements

The authors acknowledge support from NewCompStar COST Action MP1304. ND is supported by a Vidi grant from the Netherlands Organization for Scientific Research (NWO). VS is supported by Deutsche Forschungsgemeinschaft (DFG) grant WE 1312/51-1.

For the creation of Figure 5.1, the authors thank Morgane Fortin for providing unified EOSs and Feryal Ozel̈ for making her compilation of EOSs publicly available online.Footnote 6

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Correspondence to Nathalie Degenaar .

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Degenaar, N., Suleimanov, V.F. (2018). Testing the Equation of State with Electromagnetic Observations. In: Rezzolla, L., Pizzochero, P., Jones, D., Rea, N., Vidaña, I. (eds) The Physics and Astrophysics of Neutron Stars. Astrophysics and Space Science Library, vol 457. Springer, Cham. https://doi.org/10.1007/978-3-319-97616-7_5

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