The International Astronomical Union at its XVIth General Assembly in Grenoble in 1976, accepted (Resolution No. 1) a whole new consistent set of astronomical constants[1] recommended for reduction of astronomical observations, and for computation of ephemerides. It superseded the IAU's previous recommendations of 1964 (see IAU (1964) System of Astronomical Constants), became in effect in the Astronomical Almanac from 1984 onward, and remained in use until the introduction of the IAU (2009) System of Astronomical Constants. In 1994 the IAU recognized that the parameters became outdated, but retained the 1976 set for sake of continuity, but also recommended to start maintaining a set of "current best estimates".[2]
this "sub group for numerical standards" had published a list, which included new constants (like those for relativistic time scales).
The system of constants was prepared[3] by Commission 4 on ephemerides led by P. Kenneth Seidelmann (after whom asteroid 3217 Seidelmann is named).
At the time, a new standard epoch (J2000.0) was accepted; followed later by a new reference system with fundamental catalogue (FK5), and expressions for precession of the equinoxes,and in 1979 by new expressions for the relation between Universal Time and sidereal time,[4] [5] [6] and in 1979 and 1980 by a theory of nutation.[7] [8] There were no reliable rotation elements for most planets, but a joint working group on Cartographic Coordinates and Rotational Elements was installed to compile recommended values.[9] [10]
The IAU(1976) system is based on the astronomical system of units:
| Number | Quantity | Symbol | Value | Unit | Relative uncertainty | Ref. | |
|---|---|---|---|---|---|---|---|
| Defining Constants | |||||||
| 1 | align=center | k | 0.017 202 098 95 | A3/2S−1/2D−1 | defined | ||
| Primary Constants | |||||||
| 2 | align=center | c | 299 792 458 ±1.2 | m s−1 | 4 | [11] | |
| 3 | light time for unit distance | align=center | τA | 499.004 782 ±0.000 002 | s | 4 | |
| 4 | equatorial radius for Earth | align=center | ae | 6 378 140 ±5 | m | 8 | |
| 5 | dynamical form-factor for Earth | align=center | J2 | (108 263 ±1) | 1 | ||
| 6 | geocentric gravitational constant | align=center | GE | (3 986 005 ±3) | m3s−2 | 8 | |
| 7 | constant of gravitation | align=center | G | (6 672 ±4.1) | m3kg−1s−2 | 6.1 | [12] |
| 8 | Earth/Moon mass ratio | align=center | 1/μ | 81.300 7 ±0.000 3 | 4 | ||
| Moon/Earth mass ratio | align=center | μ | 0.012 300 02 | 4 | |||
| 9 | general precession in longitude | align=center | p | 5 029.0966 ±0.15 | " cy−1 | 3 | |
| 10 | obliquity of the ecliptic | align=center | ε | 23°26'21.448" ±0.10 | " | 1 | |
| 11 | constant of nutation at standard epoch J2000 | align=center | N | 9.2055 [13] | " | 3 | |
| Derived Constants | |||||||
| 12 | unit distance (astronomical unit) | align=center | A = cτA | (149 597 870 ±2) | m | 1 | |
| 13 | solar parallax | align=center | π◌ = arcsin(ae/A) | 8.794 148 ±0.000 007 | " | 8 | |
| 14 | constant of aberration for standard epoch J2000 | align=center | κ | 20.495 52 | " | ||
| 15 | flattening factor for the Earth | align=center | f | 0.003 352 81 ±0.000 000 02 | 6 | ||
| reciprocal flattening | align=center | 1/f | (298 257 ± 1.5) | 5 | |||
| 16 | heliocentric gravitational constant | align=center | GS = A3k2/D2 | (132 712 438 ±5) | m3s−2 | 4 | |
| 17 | Sun/Earth mass ratio | align=center | S/E = GS/GE | 332 946.0 ± 0.3 | 9 | ||
| 18 | mass ratio Sun to Earth+Moon | align=center | (S/E)/(1+μ) | 328 900.5 ±0.5 | 1.5 | ||
| 19 | mass of the Sun | align=center | S = GS/G | (19 891 ±12) | kg | 6 | |
| 20 | ratios of mass of Sun to planets+satellites | 1/S | |||||
| Mercury | 6 023 600 | ||||||
| Venus | 408 523.5 | ||||||
| Earth+Moon | 328 900.5 | ||||||
| Mars | 3 098 710 | ||||||
| Jupiter | 1 047.355 | ||||||
| Saturn | 3 498.5 | ||||||
| Uranus | 22 869 | ||||||
| Neptune | 19 314 | ||||||
| Pluto | 3 000 000 | ||||||
| 1. | Masses of minor planets | |
| Number | Name | Mass in solar mass |
|---|---|---|
| (1) | Ceres | (5.9 ±0.3) |
| (2) | Pallas | (1.1 ±0.2) |
| (4) | Vesta | (1.2 ±0.1) |
| 2. | Masses of satellites | ||
| Planet | Number | Satellite | Satellite/Planet mass |
|---|---|---|---|
| Jupiter | I | Io | (4.70 ±0.06) |
| II | Europa | (2.56 ±0.06) | |
| III | Ganymedes | (7.84 ±0.08) | |
| IV | Callisto | (5.6 ±0.17) | |
| Saturnus | I | Titan | (2.41 ±0.018) |
| Neptune | I | Triton | 2 |
| 3. | Equatorial radii |
| Object | Equatorial radius (km) |
|---|---|
| Mercury | 2 439 ±1 |
| Venus | 6 052 ±6 |
| Earth | 6 378.140 ±0.005 |
| Mars | 3 397.2 ±1 |
| Jupiter | 71 398 |
| Saturn | 60 000 |
| Uranus | 25 400 |
| Neptune | 24 300 |
| Pluto | 2 500 |
| Moon | 1 738 |
| Moon's disk, ratio to Earth's equatorial radius | k = 0.272 5076 ae [14] |
| Sun | 696 000 |
| 4. | Gravity fields of the planets | |||||
| Planet | J2 | J3 | J4 | C22 | S22 | S31 |
|---|---|---|---|---|---|---|
| Earth | (+108 263 ±1) | (−254 ±1) | (−161 ±1) | |||
| Mars | (+1 964 ±6) | (+36 ±20) | (-55 ±1) | (+31 ±2) | (+26 ±5) | |
| Jupiter | +0.014 75 | -0.000 58 | ||||
| Saturn | +0.016 45 | -0.0010 | ||||
| Uranus | +0.012 | |||||
| Neptune | +0.004 | |||||
| 5. | Gravity field of the Moon | |
| Quantity | Symbol | Value |
|---|---|---|
| average inclination of equator on ecliptic | I | 5 552.7" |
| moment of inertia | C/MR2 | 0.392 |
| (C-A)/B | β | 0.000 6313 |
| (B-A)/C | γ | 0.000 2278 |
| C20 | -0.000 2027 | |
| C22 | +0.000 0223 | |
| C30 | -0.000 006 | |
| C31 | +0.000 029 | |
| S31 | +0.000 004 | |
| C32 | +0.000 0048 | |
| S32 | +0.000 0017 | |
| C33 | +0.000 0018 | |
| S33 | -0.000 001 | |
IAU commission 4: https://web.archive.org/web/20100412114924/http://www.iau.org/science/scientific_bodies/commissions/4/, http://iaucom4.org/