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measured the equation of time and the ir-
regular motion of the sun; and allowed for
this in his calculations by supposing that
the centre, about which the sun moves uni-
formly, is situated a little distance from the
fixed earth. He called this point the excentric .
The line from the earth to the ”excentric”
was called the line of apses . A circle hav-
ing this centre was called the equant , and
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