The Meaning of Relativity: Four lectures delivered at Princeton University, May, 1921Einstein, Albert
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The Meaning of Relativity: Four lectures delivered at Princeton University, May, 1921
Einstein, Albert
Relativity (Physics)
3. A material particle, moving perpendicularly to the axis
of rotation inside a rotating hollow body, is deflected in
the sense of the rotation (Coriolis field). The centrifugal
action, mentioned above, inside a rotating hollow
body, also follows from the theory, as has been shown
by Thirring.[18]
[18]That the centrifugal action must be inseparably connected with the
existence of the Coriolis field may be recognized, even without calculation,
in the special case of a co-ordinate system rotating uniformly relatively to
an inertial system; our general co-variant equations naturally must apply
to such a case.
Although all of these effects are inaccessible to experiment,
because is so small, nevertheless they certainly exist according
to the general theory of relativity. We must see in them a
strong support for Mach's ideas as to the relativity of all inertial
actions. If we think these ideas consistently through to the end
we must expect the whole inertia, that is, the whole
-field, to
be determined by the matter of the universe, and not mainly by
the boundary conditions at infinity.
For a satisfactory conception of the -field of cosmical dimensions,
the fact seems to be of significance that the relative
velocity of the stars is small compared to the velocity of light.
It follows from this that, with a suitable choice of co-ordinates,
is nearly constant in the universe, at least, in that part of
the universe in which there is matter. The assumption appears
natural, moreover, that there are stars in all parts of the universe,
so that we may well assume that the inconstancy of depends
only upon the circumstance that matter is not distributed
continuously, but is concentrated in single celestial bodies and
systems of bodies. If we are willing to ignore these more local
[Pg 109]
non-uniformities of the density of matter and of the -field, in
order to learn something of the geometrical properties of the universe
as a whole, it appears natural to substitute for the actual
distribution of masses a continuous distribution, and furthermore
to assign to this distribution a uniform density . In this
imagined universe all points with space directions will be geometrically
equivalent; with respect to its space extension it will
have a constant curvature, and will be cylindrical with respect
to its -co-ordinate. The possibility seems to be particularly
satisfying that the universe is spatially bounded and thus, in
accordance with our assumption of the constancy of , is of
constant curvature, being either spherical or elliptical; for then
the boundary conditions at infinity which are so inconvenient
from the standpoint of the general theory of relativity, may be
replaced by the much more natural conditions for a closed surface.
According to what has been said, we are to put
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