By Blackwood O. H., Osgood T. H., Ruark A. E. et. al.
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Extra resources for An Outline of Atomic Physics. 3rd edition, 2nd printing
Futamase: New derivation of a third post-Newtonian equation of motion for relativistic compact binaries without ambiguity, Phys. Rev. D 68, 121501(R), (2003). 22. L. Blanchet, T. Damour, G. Esposito-Far`ese: Dimensional regularization of the third post-Newtonian dynamics of point particles in harmonic coordinates, Phys. Rev. D 69, 124007 (2004). 23. M. E. Pati, C. M. Will: Post-Newtonian gravitational radiation and equations of motion via direct integration of the relaxed Einstein equations. II.
A rather tall order which will be a challenge to meet. The phenomenological approach to pulsar tests has the advantage that it can conﬁrm or invalidate a speciﬁc theory of gravity without making assumptions about other theories. Moreover, as General Relativity has no free parameters, any test of its predictions is a potentially lethal test. From this point of view, it is remarkable that GR has passed with ﬂying colours all the pulsar tests if has been submitted to. [See, notably, Fig. ] As argued above, these tests have probed strong-ﬁeld aspects of gravity which had not been probed by solar-system (or cosmological) tests.
3. Solar-system and binary-pulsar constraints on the two-parameter family of tensor–mono-scalar theories T1 (α0 , β0 ). Figure taken from . 26 27 However, this could be achieved only at the cost of allowing some combination of the two scalar ﬁelds to carry a negative energy ﬂux. 3 × 10−5 but γ ¯ Cassini = 0. Otherwise, we systematic eﬀects, we use σγ 2 would get unreasonably strong 1σ limits on α0 because tensor–scalar theories predict that γ¯ must be negative, see Eqs. (60) and (61). Binary Systems as Test-Beds of Gravity Theories 37 In Fig.