AskDefine | Define Venus

Dictionary Definition



1 the second nearest planet to the sun; visible as an early `morning star' or an `evening star'; rotates slowly clockwise (in the opposite direction from the normal rotation of the planets); "before it was known that they were the same object the evening star was called Venus and the morning star was called Lucifer"
2 goddess of love; counterpart of Greek Aphrodite [syn: Urania]
3 type genus of the family Veneridae: genus of edible clams with thick oval shells [syn: genus Venus]

User Contributed Dictionary

See also venus



From Latin meaning "love, sexual desire, loveliness, beauty, charm", possibly cognate with Sanskrit vanas, (desire).


Proper noun

  1. the goddess of love, beauty, and natural productivity
  2. The second planet in our solar system, named for the goddess; represented in astronomy and astrology by .

Derived terms




Proper noun

  1. Venus (goddess)


Proper noun

  1. Venus (1,2)



Proper noun

  1. Venus (1,2)


Proper noun

Venus f, genitive Veneris
  1. Roman goddess of natural productivity
  2. the second planet in our solar system

Derived terms




Venus m



Venus m

Extensive Definition

Venus (pronounced ) is the second-closest planet to the Sun, orbiting it every 224.7 Earth days. It is the brightest natural object in the night sky, except for the Moon, reaching an apparent magnitude of −4.6. Because Venus is an inferior planet, from Earth it never appears to venture far from the Sun: its elongation reaches a maximum of 47.8°. Venus reaches its maximum brightness shortly before sunrise or shortly after sunset, for which reason it is often called the Morning Star or the Evening Star.
Classified as a terrestrial planet, it is sometimes called Earth's "sister planet", for the two are similar in size, gravity, and bulk composition. Venus is covered with an opaque layer of highly reflective clouds of sulfuric acid, preventing its surface from being seen from space in visible light; this was a subject of great speculation until some of its secrets were revealed by planetary science in the twentieth century. Venus has the densest atmosphere of all the terrestrial planets, consisting mostly of carbon dioxide, as it has no carbon cycle to lock carbon back into rocks and surface features, nor organic life to absorb it in biomass. It has become so hot that the earth-like oceans the young Venus is believed to have possessed have totally evaporated, leaving a dusty dry desertscape with many slab-like rocks. The best hypothesis is that the evaporated water vapor has dissociated and, with the lack of a planetary magnetic field, the hydrogen has been swept into interplanetary space by the solar wind. The atmospheric pressure at the planet's surface is 92 times that of the Earth.
Venus's surface has been mapped in detail only in the last 22 years, by Project Magellan. It shows evidence of extensive volcanism, and the sulfur in the atmosphere is taken by some experts to show that there has been some recent volcanism, but it is an enigma as to why no evidence of lava flow accompanies any of the visible caldera. It is also noteworthy that there are a surprisingly low number of impact craters. This demonstrates that the surface is relatively young, approximately half a billion years old. There is no evidence for plate tectonics, possibly because its crust is too strong to subduct without water to make it less viscous, and some suggest that instead Venus loses its internal heat in periodic massive resurfacing events.
The adjective Venusian is commonly used for items related to Venus, though the Latin adjective is the rarely used Venerean; the now-archaic Cytherean is still occasionally encountered. Venus is the only planet in the Solar System named after a female figure, although two dwarf planets—Ceres and Eris—also have female names.

Physical characteristics

Venus is one of the four solar terrestrial planets, meaning that, like the Earth, it is a rocky body. In size and mass, it is very similar to the Earth, and is often described as its 'sister'. The diameter of Venus is only 650 km less than the Earth's, and its mass is 81.5% of the Earth's. However, conditions on the Venusian surface differ radically from those on Earth, due to its dense carbon dioxide atmosphere. The mass of the atmosphere of Venus is 96.5% carbon dioxide, with most of the remaining 3.5% composed of nitrogen.

Internal structure

Though there is little direct information about its internal structure, the similarity in size and density between Venus and Earth suggests that it has a similar internal structure: a core, mantle, and crust. Like that of Earth, the Venusian core is at least partially liquid. The slightly smaller size of Venus suggests that pressures are significantly lower in its deep interior than Earth. The principal difference between the two planets is the lack of plate tectonics on Venus, likely due to the dry surface and mantle. This results in reduced heat loss from the planet, preventing it from cooling and providing a likely explanation for its lack of an internally generated magnetic field.


About 80% of Venus's surface consists of smooth volcanic plains. Two highland 'continents' make up the rest of its surface area, one lying in the planet's northern hemisphere and the other just south of the equator. The northern continent is called Ishtar Terra, after Ishtar, the Babylonian goddess of love, and is about the size of Australia. Maxwell Montes, the highest mountain on Venus, lies on Ishtar Terra. Its peak is 11 km above Venus's average surface elevation. The southern continent is called Aphrodite Terra, after the Greek goddess of love, and is the larger of the two highland regions at roughly the size of South America. Much of this continent is covered by a network of fractures and faults.
As well as the impact craters, mountains, and valleys commonly found on rocky planets, Venus has a number of unique surface features. Among these are flat-topped volcanic features called farra, which look somewhat like pancakes and range in size from 20–50 km across, and 100–1000 m high; radial, star-like fracture systems called novae; features with both radial and concentric fractures resembling spiders' webs, known as arachnoids; and coronae, circular rings of fractures sometimes surrounded by a depression. All of these features are volcanic in origin.
Almost all Venusian surface features are named after historical and mythological women. The only exceptions are Maxwell Montes, named after James Clerk Maxwell, and two highland regions, Alpha Regio and Beta Regio. These three features were named before the current system was adopted by the International Astronomical Union, the body that oversees planetary nomenclature.
Cartesian coordinates of physical features on Venus are expressed relative to its prime meridian, defined as the line of longitude passing through a radar-bright spot at the center of the oval feature Eve, which lies to the south of Alpha Regio.

Surface geology

Much of Venus's surface appears to have been shaped by volcanic activity. Overall, Venus has several times as many volcanoes as Earth, and it possesses some 167 giant volcanoes that are over 100 km across. The only volcanic complex of this size on Earth is the Big Island of Hawaii. While rainfall drives thunderstorms on Earth, there is no rainfall on the surface of Venus (though it does rain sulfuric acid in the upper atmosphere that evaporates around 25 km above the surface) One possibility is that ash from a volcanic eruption was generating the lightning. Another intriguing piece of evidence comes from measurements of sulfur dioxide concentrations in the atmosphere, which were found to drop by a factor of 10 between 1978 and 1986. This may imply that the levels had earlier been boosted by a large volcanic eruption.
There are almost 1,000 impact craters on Venus, more or less evenly distributed across its surface. On other cratered bodies, such as the Earth and the Moon, craters show a range of states of erosion, indicating a continual process of degradation. On the Moon, degradation is caused by subsequent impacts, while on Earth, it is caused by wind and rain erosion. However, on Venus, about 85% of craters are in pristine condition. The number of craters together with their well-preserved condition indicates that the planet underwent a total resurfacing event about 500 million years ago. Earth's crust is in continuous motion, but it is thought that Venus cannot sustain such a process. Without plate tectonics to dissipate heat from its mantle, Venus instead undergoes a cyclical process in which mantle temperatures rise until they reach a critical level that weakens the crust. Then, over a period of about 100 million years, subduction occurs on an enormous scale, completely recycling the crust.


Venus has an extremely thick atmosphere, which consists mainly of carbon dioxide and a small amount of nitrogen. The atmospheric mass is 93 times that of Earth's atmosphere while the pressure at the planet's surface is about 92 times that at Earth's surface—a pressure equivalent to that at a depth of nearly 1 kilometer under Earth's oceans. The density at the surface is 65 kg/m³ (6.5% that of water). The enormously CO2-rich atmosphere, along with thick clouds of sulfur dioxide, generates the strongest greenhouse effect in the solar system, creating surface temperatures of over 460 °C. This makes Venus's surface much hotter than Mercury's which has a minimum surface temperature of -220 °C and maximum surface temperature of 420 °C, even though Venus is nearly twice Mercury's distance from the Sun and receives only 25% of Mercury's solar irradiance. Because of the lack of any moisture on Venus, there is almost no relative humidity (no more than 1%) on the surface, creating a heat index of 450 °C to 480 °C.
Studies have suggested that several billion years ago Venus's atmosphere was much more like Earth's than it is now, and that there were probably substantial quantities of liquid water on the surface, but a runaway greenhouse effect was caused by the evaporation of that original water, which generated a critical level of greenhouse gases in its atmosphere. Thermal inertia and the transfer of heat by winds in the lower atmosphere mean that the temperature of Venus's surface does not vary significantly between the night and day sides, despite the planet's extremely slow rotation. Winds at the surface are slow, moving at a few kilometers per hour, but because of the high density of the atmosphere at Venus's surface, they exert a significant amount of force against obstructions, and transport dust and small stones across the surface. This alone would make it difficult for a human to walk through, even if the heat were not a problem. Above the dense CO2 layer are thick clouds consisting mainly of sulfur dioxide and sulfuric acid droplets. These clouds reflect about 60% of the sunlight that falls on them back into space, and prevent the direct observation of Venus's surface in visible light. The permanent cloud cover means that although Venus is closer than Earth to the Sun, the Venusian surface is not as well lit. In the absence of the greenhouse effect caused by the carbon dioxide in the atmosphere, the temperature at the surface of Venus would be quite similar to that on Earth. Strong 300 km/h winds at the cloud tops circle the planet about every four to five earth days.
In 2007 the Venus Express probe discovered that a huge double atmospheric vortex exists at the south pole of the planet.


The surface of Venus is effectively isothermal; it retains a constant temperature between day and night and between the equator and the poles. The planet's minute axial tilt (less than three degrees, compared with 23 degrees for Earth), also minimises seasonal temperature variation. The only appreciable variation in temperature occurs with altitude. In 1995, the Magellan probe imaged a highly reflective substance at the tops of Venus's highest mountain peaks which bore a strong resemblance to terrestrial snow. This substance arguably formed from a similar process to snow, albeit at a far higher temperature. Too volatile to condense on the surface, it rose in gas form to cooler higher elevations, where it then fell as precipitation. The identity of this substance is not known with certainty, but speculation has ranged from elemental tellurium to lead sulfide (galena).
The clouds of Venus are capable of producing lightning much like the clouds on Earth.

Magnetic field and core

In 1980, The Pioneer Venus Orbiter found that Venus's magnetic field is both weaker and smaller (i.e. closer to the planet) than Earth's. What small magnetic field is present is induced by an interaction between the ionosphere and the solar wind, rather than by an internal dynamo in the core like the one inside the Earth. Venus's magnetosphere is too weak to protect the atmosphere from cosmic radiation.
This lack of an intrinsic magnetic field at Venus was surprising given that it is similar to Earth in size, and was expected to also contain a dynamo in its core. A dynamo requires three things: a conducting liquid, rotation, and convection. The core is thought to be electrically conductive, however. Also, while its rotation is often thought to be too slow, simulations show that it is quite adequate to produce a dynamo. This implies that the dynamo is missing because of a lack of convection in Venus's core. On Earth, convection occurs in the liquid outer layer of the core because the bottom of the liquid layer is much hotter than the top. Since Venus has no plate tectonics to let off heat, it is possible that it has no solid inner core, or that its core is not currently cooling, so that the entire liquid part of the core is at approximately the same temperature. Another possibility is that its core has already completely solidified.

Orbit and rotation

Venus orbits the Sun at an average distance of about 108 million km, and completes an orbit every 224.65 days. Although all planetary orbits are elliptical, Venus is the closest to circular, with an eccentricity of less than 0.01. When Venus lies between the Earth and the Sun, a position known as 'inferior conjunction', it makes the closest approach to Earth of any planet, lying at a distance of about 41 million km. The Sun would appear to rise in the west and set in the east. At the equator, Venus's surface rotates at 6.5 km/h; on Earth, the rotation speed at the equator is about 1,600 km/h.
If viewed from above the Sun's north pole, all of the planets are orbiting in a counter-clockwise direction; but while most planets also rotate counter-clockwise, Venus rotates clockwise in "retrograde" rotation. The question of how Venus came to have a slow, retrograde rotation was a major puzzle for scientists when the planet's rotation period was first measured. When it formed from the solar nebula, Venus would have had a much faster, prograde rotation, but calculations show that over billions of years, tidal effects on its dense atmosphere could have slowed down its initial rotation to the value seen today.
A curious aspect of Venus's orbit and rotation periods is that the 584-day average interval between successive close approaches to the Earth is almost exactly equal to five Venusian solar days. Whether this relationship arose by chance or is the result of some kind of tidal locking with the Earth, is unknown.
Venus is currently moonless, though the asteroid 2002 VE68 presently maintains a quasi-orbital relationship with it. According to Alex Alemi and David Stevenson of the California Institute of Technology, their recent study of models of the early solar system shows that it is very likely that, billions of years ago, Venus had at least one moon, created by a huge impact event. About 10 million years later, according to Alemi and Stevenson, another impact reversed the planet's spin direction. The reversed spin direction caused the Venusian moon to gradually spiral inward until it collided and merged with Venus. If later impacts created moons, those moons also were absorbed the same way the first one was. The Alemi/Stevenson study is recent, and it remains to be seen what sort of acceptance it will achieve in the scientific community.


Venus is always brighter than the brightest stars, with its apparent magnitude ranging from −3.8 to −4.6. This is bright enough to be seen even in the middle of the day, and the planet can be easy to see when the Sun is low on the horizon. As an inferior planet, it always lies within about 47° of the Sun.
Venus 'overtakes' the Earth every 584 days as it orbits the Sun.
As it moves around its orbit, Venus displays phases like those of the Moon: it is new when it passes between the Earth and the Sun, full when it is on the opposite side of the Sun, and a half-phase when it is at its maximum elongations from the Sun. Venus is brightest when it is a thin crescent; it is much closer to Earth when a thin crescent than when gibbous, or full.
A long-standing mystery of Venus observations is the so-called Ashen light—an apparent weak illumination of the dark side of the planet, seen when the planet is in the crescent phase. The first claimed observation of ashen light was made as long ago as 1643, but the existence of the illumination has never been reliably confirmed. Observers have speculated that it may result from electrical activity in the Venusian atmosphere, but it may be illusory, resulting from the physiological effect of observing a very bright crescent-shaped object.

Studies of Venus

Early studies

Venus was known in the Hindu Jyotisha since early times as the planet Shukra. In the West, before the advent of the telescope, Venus was known only as a 'wandering star'. Several cultures historically held its appearances as a morning and evening star to be those of two separate bodies. Pythagoras is usually credited with recognizing in the sixth century BC that the morning and evening stars were a single body, though he thought that Venus orbited the Earth. When Galileo first observed the planet in the early 17th century, he found that it showed phases like the Moon's, varying from crescent to gibbous to full and vice versa. This could be possible only if Venus orbited the Sun, and this was among the first observations to clearly contradict the Ptolemaic geocentric model that the solar system was concentric and centered on the Earth.
Venus's atmosphere was discovered as early as 1790 by Johann Schröter. Schröter found that when the planet was a thin crescent, the cusps extended through more than 180°. He correctly surmised that this was due to scattering of sunlight in a dense atmosphere. Later, Chester Smith Lyman observed a complete ring around the dark side of the planet when it was at inferior conjunction, providing further evidence for an atmosphere. The atmosphere complicated efforts to determine a rotation period for the planet, and observers such as Giovanni Cassini and Schröter incorrectly estimated periods of about 24 hours from the motions of markings on the planet's apparent surface.

Ground-based research

Little more was discovered about Venus until the 20th century. Its almost featureless disc gave no hint as to what its surface might be like, and it was only with the development of spectroscopic, radar and ultraviolet observations that more of its secrets were revealed. The first UV observations were carried out in the 1920s, when Frank E. Ross found that UV photographs revealed considerable detail that was absent in visible and infrared radiation. He suggested that this was due to a very dense yellow lower atmosphere with high cirrus clouds above it.
90% of the surface Venus appears to be recently solid basalt lava. Spectroscopic observations in the 1900s gave the first clues about Venus's rotation. Vesto Slipher tried to measure the Doppler shift of light from Venus, but found that he could not detect any rotation. He surmised that the planet must have a much longer rotation period than had previously been thought. Later work in the 1950s showed that the rotation was retrograde. Radar observations of Venus were first carried out in the 1960s, and provided the first measurements of the rotation period which were close to the modern value.
Radar observations in the 1970s revealed details of Venus's surface for the first time. Pulses of radio waves were beamed at the planet using the 300 m radio telescope at Arecibo Observatory, and the echoes revealed two highly reflective regions, designated the Alpha and Beta regions. The observations also revealed a bright region attributed to mountains, which was called Maxwell Montes. These three features are now the only ones on Venus which do not have female names.
The best radar images obtainable from Earth revealed features no smaller than about 5 km across. More detailed exploration of the planet could only be carried out from space.

Exploration of Venus

Early efforts

The first robotic space probe mission to Venus, and the first to any planet, began on February 12 1961 with the launch of the Venera 1 probe. The first craft of the otherwise highly successful Soviet Venera program, Venera 1 was launched on a direct impact trajectory, but contact was lost seven days into the mission, when the probe was about 2 million km from Earth. It was estimated to have passed within 100,000 km from Venus in mid-May.
The United States exploration of Venus also started badly with the loss of the Mariner 1 probe on launch. The subsequent Mariner 2 mission enjoyed greater success, and after a 109-day transfer orbit on December 14 1962 it became the world's first successful interplanetary mission, passing 34,833 km above the surface of Venus. Its microwave and infrared radiometers revealed that while Venus's cloud tops were cool, the surface was extremely hot—at least 425 °C, finally ending any hopes that the planet might harbor ground-based life. Mariner 2 also obtained improved estimates of Venus's mass and of the astronomical unit, but was unable to detect either a magnetic field or radiation belts.

Atmospheric entry

The Venera 3 probe crash-landed on Venus on March 1 1966. It was the first man-made object to enter the atmosphere and strike the surface of another planet, though its communication system failed before it was able to return any planetary data. Venus's next encounter with an unmanned probe came on October 18 1967 when Venera 4 successfully entered the atmosphere and deployed a number of science experiments. Venera 4 showed that the surface temperature was even hotter than Mariner 2 had measured at almost 500 °C, and that the atmosphere was about 90 to 95% carbon dioxide. The Venusian atmosphere was considerably denser than Venera 4's designers had anticipated, and its slower than intended parachute descent meant that its batteries ran down before the probe reached the surface. After returning descent data for 93 minutes, Venera 4's last pressure reading was 18 bar at an altitude of 24.96 km. The joint Venera 4–Mariner 5 data were analyzed by a combined Soviet-American science team in a series of colloquia over the following year, in an early example of space cooperation.
Armed with the lessons and data learned from Venera 4, the Soviet Union launched the twin probes Venera 5 and Venera 6 five days apart in January 1969; they encountered Venus a day apart on May 16 and May 17 that year. The probes were strengthened to improve their crush depth to 25 atmospheres and were equipped with smaller parachutes to achieve a faster descent. Since then-current atmospheric models of Venus suggested a surface pressure of between 75 and 100 atmospheres, neither was expected to survive to the surface. After returning atmospheric data for a little over fifty minutes, they both were crushed at altitudes of approximately 20 km before going on to strike the surface on the night side of Venus.
In the meantime, the United States had sent the Mariner 10 probe on a gravitational slingshot trajectory past Venus on its way to Mercury. On February 5, 1974, Mariner 10 passed within 5790 km of Venus, returning over 4,000 photographs as it did so. The images, the best then achieved, showed the planet to be almost featureless in visible light, but ultraviolet light revealed details in the clouds that had never been seen in Earth-bound observations.
The American Pioneer Venus project consisted of two separate missions. The Pioneer Venus Orbiter was inserted into an elliptical orbit around Venus on December 4 1978, and remained there for over thirteen years studying the atmosphere and mapping the surface with radar. The Pioneer Venus Multiprobe released a total of five probes which entered the atmosphere on December 9 1978, returning data on its composition, winds and heat fluxes.
Four more Venera lander missions took place over the next four years, with Venera 11 and Venera 12 detecting Venusian electrical storms; and Venera 13 and Venera 14, landing four days apart on March 1 and March 5 1982, returning the first color photographs of the surface. All four missions deployed parachutes for braking in the upper atmosphere, but released them at altitudes of 50 km, the dense lower atmosphere providing enough friction to allow for an unaided soft landing. Both Venera 13 and 14 analyzed soil samples with an on-board X-ray fluorescence spectrometer, and attempted to measure the compressibility of the soil with an impact probe.

Manned Venus flyby

A manned Venus flyby mission, using Apollo program hardware, was proposed in the late 1960s. The mission was planned to launch in late October or early November of 1973, and would have used a Saturn V to send three men to fly past Venus in a flight lasting approximately one year. The spacecraft would have passed approximately 5,000 kilometres from the surface of Venus about four months later.

Radar mapping

The United States' Magellan probe was launched on May 4, 1989 with a mission to map the surface of Venus with radar. The probe is undertaking a detailed study of the Venusian atmosphere and clouds, and will also map the planet's plasma environment and surface characteristics, particularly temperatures. Its mission is intended to last a nominal 500 Earth days, or around two Venusian years. The European Space Agency (ESA) will also launch a mission to Mercury, called BepiColombo, which will perform two flybys of Venus in August 2013 before it reaches Mercury orbit in 2019.
Future dedicated missions to Venus are planned. Japan's aerospace body JAXA is planning to launch its Venus climate orbiter, the PLANET-C, in 2010. Under its New Frontiers Program, NASA has proposed a lander mission called the Venus In-Situ Explorer to land on Venus to study surface conditions and investigate the elemental and mineralogical features of the regolith, equipped with a core sampler to drill into the surface to study pristine rock samples not weathered by the very harsh surface conditions of the planet. Other proposed Venus exploration concepts include rovers, balloons, and Venus airplane concepts.

Venus in human culture

Historic understanding

As one of the brightest objects in the sky, Venus has been known since prehistoric times and as such has gained an entrenched position in human culture. It is described in Babylonian cuneiformic texts such as the Venus tablet of Ammisaduqa, which relates observations that possibly date from 1600 BC. The Babylonians named the planet Ishtar (Sumerian Inanna), the personification of womanhood, and goddess of love. The Ancient Egyptians believed Venus to be two separate bodies and knew the morning star as Tioumoutiri and the evening star as Ouaiti. Likewise believing Venus to be two bodies, the Ancient Greeks called the morning star , (Latinized Phosphorus), the "Bringer of Light" or , (Latinized Eosphorus), the "Bringer of Dawn". The evening star they called (Latinized Hesperus) (, the "star of the evening"), but by Hellenistic times, they realized the two were the same planet. Hesperos would be translated into Latin as Vesper and Phosphoros as Lucifer ("Light Bearer"), a poetic term later used to refer to the fallen angel cast out of heaven. The Romans would later name the planet in honor of their goddess of love, Venus, whereas the Greeks used the name of her Greek counterpart, Aphrodite (Phoenician Astarte).
To the Hebrews it was known as ("shining"), ("bright"), ("deer of the dawn") and ("star of the evening").
Venus was important to the Maya civilization, who developed a religious calendar based in part upon its motions, and held the motions of Venus to determine the propitious time for events such as war.
The Maasai people named the planet Kileken, and have an oral tradition about it called The Orphan Boy.
Venus is important in many Australian aboriginal cultures, such as that of the Yolngu people in Northern Australia. The Yolngu gather after sunset to await the rising of Venus, which they call Barnumbirr. As she approaches, in the early hours before dawn, she draws behind her a rope of light attached to the Earth, and along this rope, with the aid of a richly decorated "Morning Star Pole", the people are able to communicate with their dead loved ones, showing that they still love and remember them. Barnumbirr is also an important creator-spirit in the Dreaming, and "sang" much of the country into life.


Goddesses such as Gaia and Terra were named after the Earth, and not vice versa. Jerome translated Septuagint heosphoros and Hebrew helel as lucifer, in Isaiah 14:12.
Venus in Afrikaans: Venus (planeet)
Venus in Tosk Albanian: Venus (Planet)
Venus in Old English (ca. 450-1100): Venus
Venus in Arabic: الزهرة
Venus in Aragonese: Benus (planeta)
Venus in Franco-Provençal: Vènus (planèta)
Venus in Asturian: Venus (planeta)
Venus in Azerbaijani: Venera
Venus in Bengali: শুক্র গ্রহ
Venus in Min Nan: Kim-chheⁿ
Venus in Banyumasan: Venus
Venus in Belarusian: Планета Венера
Venus in Belarusian (Tarashkevitsa): Вэнэра (плянэта)
Venus in Central Bicolano: Venus
Venus in Bosnian: Venera
Venus in Breton: Gwener (planedenn)
Venus in Bulgarian: Венера (планета)
Venus in Catalan: Venus (planeta)
Venus in Chuvash: Венера (планета)
Venus in Czech: Venuše (planeta)
Venus in Corsican: Stedda Diana
Venus in Welsh: Gwener (planed)
Venus in Danish: Venus (planet)
Venus in German: Venus (Planet)
Venus in Estonian: Veenus
Venus in Modern Greek (1453-): Αφροδίτη (πλανήτης)
Venus in Spanish: Venus (planeta)
Venus in Esperanto: Venuso
Venus in Basque: Artizar
Venus in Persian: ناهید (سیاره)
Venus in Faroese: Venus
Venus in French: Vénus (planète)
Venus in Western Frisian: Fenus
Venus in Irish: Véineas (pláinéad)
Venus in Gan Chinese: 金星
Venus in Scottish Gaelic: Ribhinn (planaid)
Venus in Galician: Venus (planeta)
Venus in Gujarati: શુક્ર (ગ્રહ)
Venus in Classical Chinese: 金星
Venus in Korean: 금성
Venus in Hawaiian: Hōkūloa
Venus in Armenian: Վեներա
Venus in Hindi: वीनस
Venus in Croatian: Venera (planet)
Venus in Ido: Venero
Venus in Iloko: Venus (planeta)
Venus in Indonesian: Venus
Venus in Interlingua (International Auxiliary Language Association): Venus (planeta)
Venus in Ossetian: Венерæ (планетæ)
Venus in Icelandic: Venus (reikistjarna)
Venus in Italian: Venere (astronomia)
Venus in Hebrew: נוגה
Venus in Javanese: Venus
Venus in Pampanga: Venus
Venus in Kannada: ಶುಕ್ರ
Venus in Georgian: ვენერა (პლანეტა)
Venus in Kashubian: Wenus
Venus in Cornish: Gwener (planet)
Venus in Swahili (macrolanguage): Zuhura
Venus in Haitian: Venis (planèt)
Venus in Kurdish: Gelawêj (gerstêrk)
Venus in Latin: Venus (planeta)
Venus in Latvian: Venēra (planēta)
Venus in Luxembourgish: Venus (Planéit)
Venus in Lithuanian: Venera (planeta)
Venus in Limburgan: Venus (planeet)
Venus in Lingala: Mokwɛtɛ
Venus in Hungarian: Vénusz
Venus in Macedonian: Венера
Venus in Malayalam: ശുക്രന്‍ (ഗ്രഹം)
Venus in Maltese: Venere (pjaneta)
Venus in Marathi: शुक्र ग्रह
Venus in Malay (macrolanguage): Zuhrah
Venus in Moksha: Циле
Venus in Dutch: Venus (planeet)
Venus in Nepali: शुक्रग्रह
Venus in Japanese: 金星
Venus in Norwegian: Venus
Venus in Norwegian Nynorsk: Planeten Venus
Venus in Novial: Venus (planete)
Venus in Uzbek: Venera (sayyora)
Venus in Low German: Venus (Planet)
Venus in Polish: Wenus
Venus in Portuguese: Vénus (planeta)
Venus in Kölsch: Veenuß (Planneet)
Venus in Romanian: Venus (planetă)
Venus in Quechua: Ch'aska
Venus in Russian: Венера (планета)
Venus in Northern Sami: Venus
Venus in Sanskrit: शुक्र
Venus in Albanian: Venusi
Venus in Sicilian: Vèniri
Venus in Simple English: Venus (planet)
Venus in Slovak: Venuša
Venus in Slovenian: Venera
Venus in Serbian: Венера (планета)
Venus in Finnish: Venus
Venus in Swedish: Venus
Venus in Tagalog: Benus (planeta)
Venus in Tamil: வெள்ளி (கோள்)
Venus in Telugu: శుక్రుడు
Venus in Thai: ดาวศุกร์
Venus in Vietnamese: Sao Kim
Venus in Tajik: Зӯҳра
Venus in Turkish: Venüs (gezegen)
Venus in Ukrainian: Венера (планета)
Venus in Urdu: زہرہ
Venus in Contenese: 金星
Venus in Samogitian: Aušruos žvaizdie
Venus in Chinese: 金星

Synonyms, Antonyms and Related Words

Adonis, Agdistis, Aldebaran, Amor, Aphrodite, Apollo, Apollo Belvedere, Apollon, Ares, Artemis, Astarte, Ate, Athena, Bacchus, Balder, Canicula, Ceres, Cleopatra, Cora, Cronus, Cupid, Cybele, Demeter, Despoina, Diana, Dionysus, Dis, Dog Star, Earth, Eros, Freya, Gaea, Gaia, Ge, Great Mother, Hades, Hebe, Helios, Hephaestus, Hera, Here, Hermes, Hesper, Hesperus, Hestia, Hymen, Hyperion, Jove, Juno, Jupiter, Jupiter Fidius, Jupiter Fulgur, Jupiter Optimus Maximus, Jupiter Pluvius, Jupiter Tonans, Kama, Kore, Kronos, Love, Lucifer, Magna Mater, Mars, Mercury, Minerva, Mithras, Momus, Narcissus, Neptune, Nike, North Star, Olympians, Olympic gods, Ops, Orcus, Persephassa, Persephone, Phoebus, Phoebus Apollo, Phosphor, Phosphorus, Pluto, Polaris, Poseidon, Proserpina, Proserpine, Rhea, Saturn, Sirius, Tellus, Uranus, Venus de Milo, Vesper, Vesta, Vulcan, Zeus, asteroid, celestial body, comet, daystar, evening star, fixed stars, heavenly body, houri, inferior planet, living sapphires, lodestar, major planet, minor planet, morning star, orb, peri, planet, planetoid, polar star, polestar, secondary planet, solar system, sphere, starry host, stars, superior planet, terrestrial planet, the Graces, wanderer
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