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參考資料

↑  . 香港中文大學.   [2017-09-12]. （原始内容存档于2021-01-16）.
↑  Jawad, Ala'a H. Roger W. Sinnott , 编. . Sky&Telescope. Nov 1993: pp.76..77.  引文格式1维护：冗余文本 (link)
↑  Meeus, Jean. . Willmann-Bell, Richmond VA USA. 2002: 19..31. ISBN 0-943396-74-3.
↑  formula 47.1 in Jean Meeus (1991): Astronomical Algorithms (1st ed.) ISBN 978-0-943396-35-4
↑  M.Chapront-Touzé, J. Chapront (1988): "ELP2000-85: a semianalytical lunar ephemeris adequate for historical times". Astronomy & Astrophysics 190, 342..352
↑  J.Chapront, M.Chapront-Touzé, G. Francou (2002): "A new determination of lunar orbital parameters, precession constant, and tidal acceleration from LLR measurements （页面存档备份，存于）".  Astronomy & Astrophysics 387, 700–709
↑  Annual aberration is the ratio of Earth's orbital velocity (around 30 km/s) to the speed of light (about 300,000 km/s), which shifts the Sun's apparent position relative to the celestial sphere toward the west by about 1/10,000 radian. Light-time correction for the Moon is the distance it moves during the time it takes its light to reach Earth divided by the Earth-Moon distance, yielding an angle in radians by which its apparent position lags behind its computed geometric position. Light-time correction for the Sun is negligible because it is almost motionless during 8.3 minutes relative to the barycenter (center-of-mass) of the solar system. The aberration of light for the Moon is also negligible (the center of the Earth moves too slowly around the Earth-Moon barycenter (0.002 km/s); and the so-called diurnal aberration, caused by the motion of an observer on the surface of the rotating Earth (0.5 km/s at the equator) can be neglected. Although aberration and light-time are often combined as planetary aberration, Meeus separated them (op.cit. p.210).
↑  Derived Constant #14 from the IAU (1976) System of Astronomical Constants (proceedings of IAU Sixteenth General Assembly (1976): Transactions of the IAU XVIB p.58 (1977)); or any astronomical almanac; or e.g.  （页面存档备份，存于）
↑  formula in: G.M.Clemence, J.G.Porter, D.H.Sadler (1952): "Aberration in the lunar ephemeris", Astronomical Journal 57(5) (#1198) pp.46..47  （页面存档备份，存于）; but computed with the conventional value of 384400 km for the mean distance which gives a different rounding in the last digit.
↑  Apparent mean solar longitude is −20.496" from mean geometric longitude; apparent mean lunar longitude −0.704" from mean geometric longitude; correction to D = Moon − Sun is −0.704" + 20.496" = +19.792" that the apparent Moon is ahead of the apparent Sun; divided by 360×3600"/circle is 1.527×10−5 part of a circle; multiplied by 29.53... days for the Moon to travel a full circle with respect to the Sun is 0.000451 days that the apparent Moon reaches the apparent Sun ahead of time.
↑  see e.g. .   [2006-12-17]. （原始内容存档于2007-02-02）. ; the IERS is the official source for these numbers; they provide TAI−UTC here （页面存档备份，存于） and UT1−UTC here （页面存档备份，存于）; ΔT = 32.184s + (TAI−UTC) − (UT1−UTC)
↑  delay is − (−5.8681") / (60×60×360 "/circle) / (36525/29.530... lunations per Julian century)² × (29.530... days/lunation) days
↑  −5.8681" + 0.5×(−25.858 − −23.8946)
↑  F.R. Stephenson, Historical Eclipses and Earth's Rotation. Cambridge University Press 1997. ISBN 978-0-521-46194-8 . p.507, eq.14.3
↑  31 s / (86400 s/d) / [(36525 d/cy) / (29.530... d/lunation)]²
↑  Stephenson 1997 op.cit. p.38 eq.2.8
↑  Stephenson 1997 op.cit. par.14.8
↑  from differences of various earlier determinations of the tidal acceleration, see e.g. Stephenson 1997 op.cit. par.2.2.3