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Post Info TOPIC: PSR J1141-6545

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Posts: 131433
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 RE: PSR J1141-6545 Permalink Title: PSR J1141-6545: a powerful laboratory of GR and tensor-scalar theories of gravity Authors: J. P. W. Verbiest, N. D. R. Bhat, M. Bailes Pulsars in close binary systems have provided some of the most stringent tests of strong-field gravity to date. The pulsar--white-dwarf binary system J1141-6545 is specifically interesting due to its gravitational asymmetry which makes it one of the most powerful probes of tensor-scalar theories of gravity. We give an overview of current gravitational tests provided by the J1141-6545 binary system and comment on how anomalous accelerations, geodetic precession and timing instabilities may be prevented from limiting future tests of gravity to come from this system. Read more (14kb, PDF) __________________

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Posts: 131433
Date:
 Permalink Title: Gravitational-radiation losses from the pulsar-white-dwarf binary PSR J1141-6545Authors: N. D. Ramesh Bhat, Matthew Bailes, Joris P. W. VerbiestPulsars in close binary orbit around another neutron star or a massive white dwarf make ideal laboratories for testing the predictions of gravitational radiation and self-gravitational effects. We report new timing measurements of the pulsar-white-dwarf binary PSR J1141-6545, providing strong evidence that such asymmetric systems have gravitational wave losses that are consistent with general relativity. The orbit is found to be decaying at a rate of 1.04 ±0.06 times the general relativistic prediction and the Shapiro delay is consistent with the orbital inclination angle derived from scintillation measurements. The system provides a unique test-bed for tensor-scalar theories of gravity; our current measurements place stringent constraints in the theory space, with a limit of \alpha_0²  < 2.1 \times 10^{-5} for weakly non-linear coupling and an asymptotic limit of \alpha_0²  < 3.4 \times 10^{-6} for strongly non-linear coupling, where \alpha_0 is the linear coupling strength of matter to an underlying scalar field. This asymptotic limit is nearly three times smaller than the Cassini bound (\alpha_0²  ~ 10^{-5}). Read more (26kb, PDF) __________________
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