Editing Gaussian gravitational constant (section)

===Units and dimensions===
{{mvar|k}} is given as a unit-less fraction of the order of 1.7%, but it can be considered equivalent to the square root of the [[gravitational constant]],<ref>{{cite book  | last1 = U.S. Naval Observatory | first1=Nautical Almanac Office | last2 = H.M. Nautical Almanac Office | title = Explanatory Supplement to the Astronomical Ephemeris and the American Ephemeris and Nautical Almanac | publisher = H.M. Stationery Office |location=London | year = 1961 | page = 493}}</ref> in which case it has the [[Units of measurement|units]] of au<sup>{{frac|3|2}}</sup>⋅d<sup>−1</sup>⋅{{solar mass}}<sup>−{{frac|1|2}}</sup>,<ref name="Clemence65"/>  where
:au is the [[distance]] for which {{mvar|k}} takes its value as defined by Gauss—the distance of the [[Perturbation (astronomy)|unperturbed]] [[circular orbit]] of a hypothetical, massless body whose [[orbital period]] is {{math|{{sfrac|2π|''k''}}}} days,<ref name="Herrick65"/>
:d is the [[mean solar day]] (86,400 seconds),
:{{solar mass}} is the [[mass]] of the [[solar mass|Sun]].
Therefore, the [[Dimensional analysis|dimensions]] of {{mvar|k}} are<ref>{{cite book|last1 = Brouwer|first1 = Dirk|last2 = Clemence|first2 = Gerald M.| title = Methods of Celestial Mechanics|url = https://archive.org/details/methodsofcelesti00brou|url-access = registration|publisher = Academic Press |location=New York and London|date=1961|page=[https://archive.org/details/methodsofcelesti00brou/page/58 58]}}</ref>
:length<sup>{{frac|3|2}}</sup> time<sup>−1</sup> mass<sup>−{{frac|1|2}}</sup> or {{math|L<sup>{{frac|3|2}}</sup> T<sup>−1</sup> M<sup>−{{frac|1|2}}</sup>}}.

In spite of this {{mvar|k}} is known to much greater accuracy than {{mvar|G}} (or the square root of {{mvar|G}}).
The absolute value of {{mvar|G}} is known to an accuracy of about 10<sup>−4</sup>, but the product {{math|''G''{{solar mass}}}} (the gravitational parameter of the Sun) is known to an accuracy better than 10<sup>−10</sup>.