|How to say it||how to say: /ˈviːnəs/|
|Adjective||Venusian or (rarely) Cytherean, Venerean|
|Reference date J2000|
|Longest distance from the Sun||108,942,109 km
0.728 231 28 AU
|Shortest distance from the Sun||107,476,259 km
0.718 432 70 AU
|Longest distance from the center of its orbital path
0.723 332 AU
|How egg-shaped its orbit is
|How long it takes to complete an orbit||224.700 69 day
0.615 197 0 yr
1.92 Venus solar day
|How long an orbit seems to take
(from the central body)
|Average speed||35.02 km/s|
|Angle above the reference plane
|3.394 71° to Ecliptic
3.86° to Sun’s equator
2.19° to Invariable plane
|Longitude of where it comes up through the reference plane||76.670 69°|
|Angle between its shortest distance from what it orbits around and where it comes up through the reference plane
("argument of periapsis")
|Natural things which orbit around it||None|
|Size and Other Qualities|
|Average distance from its center to its surface||6,051.8 ± 1.0 km
0.949 9 Earths
|Flatness at the poles||0|
|Area of its surface||4.60×108 km²
|Volume inside it||9.38×1011 km³
|Mass||4.868 5×1024 kg
|Average density||5.204 g/cm³|
|Gravity at its surface||8.87 m/s2
|Slowest speed able to escape into space
|How long it takes to turn around one time
(in relation to the stars)
|-243.018 5 day|
|Turning speed||6.52 km/h (1.81 m/s)|
|Angle at which it turns
(in relation to its orbit)
|Long. around the celestial equator
|18 h 11 min 2 s
|Angle above the celestial equator
|How much light it reflects||0.65 (geometric) or 0.75 (bond)|
|up to -4.6 (crescent)
|9.7" – 66.0"|
|Pressure||93 bar (9.3 MPa)|
|Make up||~96.5% Carbon dioxide
0.015% Sulfur dioxide
0.002% Water vapor
0.001 7% Carbon monoxide
0.001 2% Helium
0.000 7% Neon
trace Carbonyl sulfide
trace Hydrogen chloride
trace Hydrogen fluoride
Venus is the second planet from the Sun. It is a terrestrial planet because it has a solid, rocky surface like other planets in the inner solar system. Astronomers have known Venus for thousands of years. The ancient Romans named it after their goddess Venus. Venus is the brightest thing in the night sky except for the Moon. It is sometimes called the morning star or the evening star as it is brightest just before the sun comes up in the morning, and just after the sun goes down in the evening. Venus comes closer to the Earth than any other planet does.
Venus is sometimes called the sister planet of Earth as they are quite similar in size and gravity. In other ways the planets are very different. Venus' atmosphere (air) is mostly carbon dioxide with clouds of sulfuric acid. Sulphuric acid is a chemical that is very poisonous to humans.
The thick atmosphere has made it hard to see the surface, and until the twenty-first century many people thought things might live there. The pressure on Venus' surface is 92 times that of Earth. Venus has no moons. Venus spins very slowly on its axis and it spins in the opposite direction to the other planets.
Physical Properties[change | change source]
Venus is a terrestrial planet so, like the Earth, its surface is made of rock. Venus is much hotter than Earth. All the carbon dioxide in the atmosphere acts like a blanket, trapping heat from the Sun. This effect is called the greenhouse effect and it is very strong on Venus. This makes the surface of Venus the hottest of any planet's surface in the Solar System with an estimated average temperature of 480 °C (896.0 °F). This is hot enough to melt lead or zinc.
Geography[change | change source]
Venus has no oceans because it is much too hot for water. Venus' surface is a dry desert. It is about 80% smooth, rocky plains. Two higher areas called continents make up the north and south of the planet. The north is called Ishtar Terra and the south is called Aphrodite Terra. They are named after the Babylonian and Greek goddesses of love.
Atmosphere[change | change source]
Venus' atmosphere is mostly carbon dioxide and nitrogen gas with clouds of sulphuric acid. Because the atmosphere is so thick or dense the pressure is very high. The pressure is 92 times the pressure on Earth, enough to crush many things.
It is impossible to see the planet's surface from space as the thick cloud layer reflects 60% of the light that hits it. The only way scientists are able to see it is by using infrared and ultraviolet cameras and radar.
Transit of Venus[change | change source]
Venus can sometimes be seen passing between the sun and earth. Venus looks like a black dot when seen through a special telescope. These "transits" happen in pairs eight years apart. Then it's more than a hundred years to the next pair.
Related pages[change | change source]
References and Notes[change | change source]
- Williams, David R. (April 15, 2005). "Venus Fact Sheet". NASA. http://nssdc.gsfc.nasa.gov/planetary/factsheet/venusfact.html. Retrieved 2007-10-12.
- "The MeanPlane (Invariable plane) of the Solar System passing through the barycenter". 2009-04-03. http://home.comcast.net/~kpheider/MeanPlane.gif. Retrieved 2009-04-10. (produced with Solex 10 written by Aldo Vitagliano; see also Invariable plane)
- Harvey, Samantha (2011-02-16). "NASA: Solar System Exploration: Planets: Venus: Moons". NASA. http://solarsystem.nasa.gov/planets/profile.cfm?Object=Venus&Display=Moons. Retrieved 2011-03-31.
- Seidelmann, P. Kenneth; Archinal, B. A.; A’hearn, M. F.; et al. (2007). "Report of the IAU/IAGWorking Group on cartographic coordinates and rotational elements: 2006". Celestial Mechanics and Dynamical Astronomy 90: 155–180. doi:10.1007/s10569-007-9072-y. http://adsabs.harvard.edu/doi/10.1007/s10569-007-9072-y. Retrieved 2007-08-28.
- "Report on the IAU/IAG Working Group on cartographic coordinates and rotational elements of the planets and satellites". International Astronomical Union. 2000. http://www.hnsky.org/iau-iag.htm. Retrieved 2007-04-12.
- Espenak, Fred (1996). "Venus: Twelve year planetary ephemeris, 1995–2006". NASA Reference Publication 1349. NASA/Goddard Space Flight Center. http://sunearth.gsfc.nasa.gov/eclipse/TYPE/venus2.html. Retrieved 2006-06-20.
- "Venus: Facts & Figures". NASA. http://sse.jpl.nasa.gov/planets/profile.cfm?Object=Venus&Display=Facts&System=Metric. Retrieved 2007-04-12.
- "Space Topics: Compare the Planets: Mercury, Venus, Earth, The Moon, and Mars". Planetary Society. http://www.planetary.org/explore/topics/compare_the_planets/terrestrial.html. Retrieved 2007-04-12.
- in our Solar System
- "The Atmosphere of Venus". http://www.windows.ucar.edu/tour/link=/venus/atmosphere.html.
- "Venus - an overview". http://filer.case.edu/sjr16/advanced/venus.html.
- "Temperature on the Surface of Venus". http://hypertextbook.com/facts/2000/GeorgeRyabov.shtml.
- Batson R.M., Russell J.F. (1991), Naming the Newly Found Landforms on Venus, Abstracts of the Lunar and Planetary Science Conference, v. 22, p. 65
Other websites[change | change source]
☾ = moon(s) ∅ = rings
|Mercury||Venus||Earth ☾||Mars ☾|
|Jupiter ☾ ∅||Saturn ☾ ∅||Uranus ☾ ∅||Neptune ☾ ∅|
|Dwarf planets||Ceres||Pluto ☾||Haumea ☾||Makemake|
|Groups and families: Vulcanoids · Near-Earth asteroids · Asteroid belt
Jupiter Trojans · Centaurs · Neptune Trojans · Asteroid moons · Meteoroids · Pallas · Juno · Vesta · Hygiea · Interamnia · Europa
|See also the list of asteroids.|
|Kuiper belt – Plutinos: Orcus · Ixion – Cubewanos: Varuna ·
Quaoar · Huya
|Scattered disc: Sedna|
|Comets||Periodic comets and non-periodic comets
Damocloids · Oort cloud
|See also the list of solar system objects|