Question: Does Venus feature 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 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. 
 Venus (0.7 AU from the Sun) is close in size to Earth (0.815 Earth masses) and, like Earth, has a thick silicate mantle around an iron core, a substantial atmosphere, and evidence of internal geological activity.
It is much drier than Earth, and its atmosphere is ninety times as dense.
Venus has no natural satellites.
It is the hottest planet, with surface temperatures over 400 °C (752°F), most likely due to the amount of greenhouse gases in the atmosphere.
No definitive evidence of current geological activity has been detected on Venus, but it has no magnetic field that would prevent depletion of its substantial atmosphere, which suggests that its atmosphere is frequently replenished by volcanic eruptions.
It is the innermost of the outer irregular retrograde satellites of Jupiter, and does not seem to belong to any group.