Editing Celestial mechanics (section)

==Reference frame==
{{expand-section|date=September 2023}}
Problems in celestial mechanics are often posed in simplifying reference frames, such as the '''synodic reference frame'''<!-- redirects here --> applied to the [[three-body problem]], where the origin coincides with the [[barycenter]] of the two larger celestial bodies. Other reference frames for n-body simulations include those that place the origin to follow the center of mass of a body, such as the heliocentric and the geocentric reference frames.<ref>{{Cite journal |last1=Guerra |first1=André G C |last2=Carvalho |first2=Paulo Simeão |date=1 August 2016 |title=Orbital motions of astronomical bodies and their centre of mass from different reference frames: a conceptual step between the geocentric and heliocentric models |journal=Physics Education |volume=51 |issue=5|doi=10.1088/0031-9120/51/5/055012 |arxiv=1605.01339 |bibcode=2016PhyEd..51e5012G }}</ref> The choice of reference frame gives rise to many phenomena, including the [[Retrograde and prograde motion|retrograde motion]] of [[Inferior and superior planets|superior planets]] while on a geocentric reference frame.