Question: Does venus have any natural satellites?
About the article "Solar System", section "Venus".

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The existence of retrograde satellites or quasi-satellites was first considered by J. Jackson in 1913 but none was discovered until almost 100 years later.
was the first quasi-satellite to be discovered, in 2002, although it was not immediately recognized as such.
was identified as a quasi-satellite of Venus by Seppo Mikkola, Ramon Brasser, Paul A. Wiegert and Kimmo Innanen in 2004, two years after the actual discovery of the object.
From the perspective of a hypothetical observer in a frame of reference rotating with Venus, it appears to travel around the planet during one Venusian year although it does not orbit Venus but the Sun like any other asteroid.
As quasi-satellite, this minor body is trapped in a 1:1 mean motion resonance with Venus.
Besides being a Venus co-orbital, this Aten asteroid is also a Mercury grazer and an Earth crosser.
exhibits resonant (or near-resonant) behavior with Mercury, Venus and the Earth.
It seems to have been co-orbital with Venus for only the last 7,000 years, and is destined to be ejected from this orbital arrangement about 500 years from now.
During this time, its distance to Venus has been and will remain larger than about 0.2 AU (3·107 km). 
A natural satellite, or moon, is a celestial body that orbits another body, e.g.
a planet, which is called its "primary".
There are 173 known natural satellites orbiting planets in the Solar System, as well as at least eight orbiting IAU-listed dwarf planets.
, over 200 minor-planet moons have been discovered.
There are 76 known objects in the asteroid belt with satellites (five with two satellites each), four Jupiter trojans, 39 near-Earth objects (two with two satellites each), and 14 Mars-crossers.
There are also 84 known natural satellites of trans-Neptunian objects.
Some 150 additional small bodies have been observed within rings of Saturn, but only a few were tracked long enough to establish orbits.
Planets around other stars are likely to have satellites as well, though numerous candidates have been detected to date, none have yet been confirmed.
Of the inner planets, Mercury and Venus have no natural satellites; Earth has one large natural satellite, known as the Moon; and Mars has two tiny natural satellites, Phobos and Deimos.
The large gas giants have extensive systems of natural satellites, including half a dozen comparable in size to Earth's Moon: the four Galilean moons, Saturn's Titan, and Neptune's Triton.
Saturn has an additional six mid-sized natural satellites massive enough to have achieved hydrostatic equilibrium, and Uranus has five.
It has been suggested that some satellites may potentially harbour life, though there is currently no direct evidence of life.
The Earth–Moon system is unique in that the ratio of the mass of the Moon to the mass of the Earth is much greater than that of any other natural-satellite–planet ratio in the Solar System (although there are minor-planet systems with even greater ratios, notably the Pluto–Charon system).
Among the dwarf planets, Ceres and Makemake have no known natural satellites.
Pluto has the relatively large natural satellite Charon and four smaller natural satellites.
Haumea has two natural satellites, and Eris has one.
The Pluto–Charon system is unusual in that the center of mass lies in open space between the two, a characteristic sometimes associated with a double-planet system. 
Venus became a popular subject of painting and sculpture during the Renaissance period in Europe.
As a "classical" figure for whom nudity was her natural state, it was socially acceptable to depict her unclothed.
As the goddess of sexuality, a degree of erotic beauty in her presentation was justified, which appealed to many artists and their patrons.
Over time, "venus" came to refer to any artistic depiction in post-classical art of a nude woman, even when there was no indication that the subject was the goddess.
The Birth of Venus (Botticelli) (c. 1485)  Sleeping Venus (c. 1501)  Venus of Urbino (1538)  Venus with a Mirror (c. 1555)  Rokeby Venus  Olympia (1863)  The Birth of Venus (Cabanel) (1863)  The Birth of Venus (Bouguereau) (1879)  Venus of Cherchell, Gsell museum in Algeria  "Venus Victrix", and "Venus Italica" by Antonio Canova In the field of prehistoric art, since the discovery in 1908 of the so-called "Venus of Willendorf" small Neolithic sculptures of rounded female forms have been conventionally referred to as Venus figurines.
Although the name of the actual deity is not known, the knowing contrast between the obese and fertile cult figures and the classical conception of Venus has raised resistance to the terminology. 
Venus orbits the Sun at an average distance of about , and completes an orbit every 224.65 days.
Although all planetary orbits are elliptical, Venus's orbit is the closest to circular, with an eccentricity of less than 0.01.
When Venus lies between Earth and the Sun, a position known as inferior conjunction, it makes the closest approach to Earth of any planet at an average distance of 41 million km.
The planet reaches inferior conjunction every 584 days, on average.
Owing to the decreasing eccentricity of Earth's orbit, the minimum distances will become greater over tens of thousands of years.
From the year 1 to 5383, there are 526 approaches less than 40 million km; then there are none for about .
During periods of greater eccentricity, Venus can come as close as 38.2 million km.
All the planets of the Solar System orbit the Sun in an anti-clockwise direction as viewed from above the Sun's north pole.
Most planets also rotate on their axes in an anti-clockwise direction, but Venus rotates clockwise (called "retrograde" rotation) once every 243 Earth days—the slowest rotation period of any planet.
A Venusian sidereal day thus lasts longer than a Venusian year (243 versus 224.7 Earth days).
Venus's equator rotates at , whereas Earth's is approximately .
Venus's rotation has slowed down by per Venusian sidereal day since the Magellan spacecraft visited it ago.
Because of the retrograde rotation, the length of a solar day on Venus is significantly shorter than the sidereal day, at 116.75 Earth days (making the Venusian solar day shorter than Mercury's 176 Earth days); one Venusian year is about 1.92 Venusian (solar) days long.
To an observer on the surface of Venus, the Sun would rise in the west and set in the east.
Venus may have formed from the solar nebula with a different rotation period and obliquity, reaching its current state because of chaotic spin changes caused by planetary perturbations and tidal effects on its dense atmosphere, a change that would have occurred over the course of billions of years.
The rotation period of Venus may represent an equilibrium state between tidal locking to the Sun's gravitation, which tends to slow rotation, and an atmospheric tide created by solar heating of the thick Venusian atmosphere.
The 584-day average interval between successive close approaches to Earth is almost exactly equal to 5 Venusian solar days, but the hypothesis of a spin–orbit resonance with Earth has been discounted.
Venus has no natural satellites, though the asteroid 2002 VE68 presently maintains a quasi-orbital relationship with it.
Besides this quasi-satellite, it has two other temporary co-orbitals, and .
In the 17th century, Giovanni Cassini reported a moon orbiting Venus, which was named Neith and numerous sightings were reported over the following , but most were determined to be stars in the vicinity.
Alex Alemi's and David Stevenson's 2006 study of models of the early Solar System at the California Institute of Technology shows Venus likely had at least one moon created by a huge impact event billions of years ago.
About 10 million years later, according to the study, another impact reversed the planet's spin direction and caused the Venusian moon gradually to spiral inward until it collided and merged with Venus.
If later impacts created moons, these were absorbed in the same way.
An alternative explanation for the lack of satellites is the effect of strong solar tides, which can destabilize large satellites orbiting the inner terrestrial planets. 
In the context of spaceflight, a satellite is an artificial object which has been intentionally placed into orbit.
Such objects are sometimes called artificial satellites to distinguish them from natural satellites such as the Moon.
The world's first artificial satellite, the Sputnik 1, was launched by the Soviet Union in 1957.
Since then, thousands of satellites have been launched into orbit around the Earth.
Some satellites, notably space stations, have been launched in parts and assembled in orbit.
Artificial satellites originate from more than 50 countries and have used the satellite launching capabilities of ten nations.
A few hundred satellites are currently operational, whereas thousands of unused satellites and satellite fragments orbit the Earth as space debris.
A few space probes have been placed into orbit around other bodies and become artificial satellites to the Moon, Mercury, Venus, Mars, Jupiter, Saturn, Vesta, Eros, and the Sun.
Satellites are used for a large number of purposes.
Common types include military and civilian Earth observation satellites, communications satellites, navigation satellites, weather satellites, and research satellites.
Space stations and human spacecraft in orbit are also satellites.
Satellite orbits vary greatly, depending on the purpose of the satellite, and are classified in a number of ways.
Well-known (overlapping) classes include low Earth orbit, polar orbit, and geostationary orbit.
About 6,600 satellites have been launched.
The latest estimates are that 3,600 remain in orbit.
Of those, about 1,000 are operational; the rest have lived out their useful lives and are part of the space debris.
Approximately 500 operational satellites are in low-Earth orbit, 50 are in medium-Earth orbit (at 20,000 km), the rest are in geostationary orbit (at 36,000 km).
Satellites are propelled by rockets to their orbits.
Usually the launch vehicle itself is a rocket lifting off from a launch pad on land.
In a minority of cases satellites are launched at sea (from a submarine or a mobile maritime platform) or aboard a plane (see air launch to orbit).
Satellites are usually semi-independent computer-controlled systems.
Satellite subsystems attend many tasks, such as power generation, thermal control, telemetry, attitude control and orbit control.