Astronomy and Astrophysics – Astronomy
Scientific paper
Nov 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...322..288n&link_type=abstract
Astrophysical Journal v.322, p.288
Astronomy and Astrophysics
Astronomy
2
Gravitation, Pulsars, Stars: Binaries
Scientific paper
If the post-Newtonian gravitational equations of motion exhibit a "preferred inertial frame," a possible observational consequence is that orbital systems whose center of mass moves relative to the preferred frame will have semisecular time variation in the orbital periods - the semisecular period being the period of precession of orbital periastron location. A contribution to the binary pulsar PSR 1913+16 orbital period rate of change above the level of observational accuracy would result for a parameterized post-Newtonian (PPN) coeffient α1 exceeding 5 x 10-9 ∣(mp + mc)/(mpM - mc)∣ , where mp is the pulsar mass and mc is the companion mass. Such a contribution would destroy agreement with the observed period rate of change and the calculated rate of change due to gravitational radiation reaction in general relativity. The fast precession rate of the binary pulsar system's periastron (4.2 arc degrees yr-1) should permit distinguishing this α1 effect from the secular gravitational radiation reaction effect.
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