The double pulsar system: a unique laboratory for gravity

By Michael Kraemer, N. Wex. 2009

233 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Oceanography

View Paper: https://www.semanticscholar.org/paper/461124f4491e832e9f2c47a8a21683e9571cc11f

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Citations in the corpus

Stellar structure models in modified theories of gravity: Lessons and challenges (2019, background): “In this sense, precise future measurements of the moment of inertia could allow to constrain the value of Q∞ [373], which must also satisfy the stability condition for this model, which reads”
Doing Science with eLISA: Astrophysics and Cosmology in the Millihertz Regime (2012, result): “In that system, the orbital period derivative is consistent with GR at the 0.3 % level, and the Shapiro delay agrees to within 0.05 % with the predictions of GR (Kramer and Wex, 2009).”
Formation of Double Neutron Star Systems (2017, background): “…objects in relativistic orbits and radio pulsars being ultra stable clocks allows for unprecedented tests of gravitational theories in the strong-field regime (Damour & Taylor 1992; Stairs 2003; Kramer et al. 2006b; Kramer & Wex 2009; Damour 2009; Freire et al. 2012; Wex 2014; Kaspi & Kramer 2016).”
Approximate Universal Relations for Neutron Stars and Quark Stars (2016, background): “Of course, such precision is currently unnecessary, since not even the effect of the moment of inertia, and thus the dipole moment, on the orbital motion is currently within the level of observational precision [67, 91].”
PRECISE γ-RAY TIMING AND RADIO OBSERVATIONS OF 17 FERMI γ-RAY PULSARS (2010, background): “Precise timing measurements on radio pulsars have yielded many fundamental advances including the first indirect detection of energy loss due to gravitational radiation (Taylor et al. 1979) and confirmation of many effects predicted by General Relativity (Stairs 2003; Kramer & Wex 2009).”
Maximum mass, moment of inertia and compactness of relativistic stars (2016, background): “If the mass is observed with a much larger precision [as it is natural to expect from pulsar measurements in binary neutron-star systems (Kramer & Wex 2009)], then it is possible to define regions in the (M, R) plane that are compatible with such observations.”