The viable MOND theories from Section 7, although still mostly effective, have the great advantage of
proving that constructing relativistic MOND theories is possible, and that it is thus possible to calculate
from them the effects of gravitational lensing. But the non-uniqueness of the theories means that there is
not really a unique prediction for gravitational lensing, especially in heavily–time-dependent configurations,
or when the predictions of the theories for the expansion history of the universe deviate from the
concordance model. As we have seen, some theories also deviate slightly from classical MOND predictions
for dynamics of quasi-static systems, due to the presence of massive dark fields, and the same would of
course happen for gravitational lensing. However, at the zeroth order, and in static weak-field
configurations, we can make predictions for all theories whose expansion history would be similar to that
of CDM (see Section 9.1) and whose static weak-field limit is represented by a physical
metric56
with
in Eq. 73
(
obeying Eq. 17
). In this case, the way the light propagates on the
null geodesics of this metric is exactly the same in all these theories once
is known. What
differs from GR is only the relation between
and the underlying mass distribution of the
lens.
http://www.livingreviews.org/lrr-2012-10 |
Living Rev. Relativity 15, (2012), 10
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