Venus, one of the four terrestrial planets, and the planet second from the Sun, is similar to Earth in mass, but differs significantly in its atmosphere because of the heating by the Sun. The heating of Venus's atmosphere has evaporated all of the hydrogen from the atmosphere, completely removing one of the two components of water from the planet.
In this table, the observed values are taken from Yoder (1995).[1] Go to table of characteristics.
3.248586(3±4)×1020 cm3 s−2 | |
4.867×1027 g | |
6.0518(4±1)×108 cm | |
886.992 cm s−2 | |
1.03614×106 cm s−1 | |
5.243 g cm−3 | |
243.0185 d | |
177° 18′ | |
224.695434 d | |
0.72333199 AU | |
0.00677323 | |
2.6139×106 ergs cm−2 s−1 |
[1] Yoder, Charles F. “Astrometric and Geodetic Properties of Earth and the Solar System.” In Global Earth Physics: A Handbook of Physical Constants edited by T.J. Ahrens, 1–31. AGU Reference Shelf, No. 1. Washington: American Geophysical Union, 1995.