Why does Venus rotate differently to the other planets?

Question

What's makes this planet special?

Answer 1

We do not have a real explanation...
During the stage of formation of the solar system, the gases and dust accumulated to form one big blog, the sun, and several other blogs that became planets. This cloud of dust was animated with a small rotation, and each blog rotated with slight differences. The Sun formed, and the rest of the dust became planets, still with some remaining rotation. At that time, many small blogs were floating around and hitting each other. It is likely that, at that stage, Venus (or what would become Venus) was hit by another rock, changed rotation, and still running that way.
So, no, Venus is not "special". It is just another rock that was formed at the time...

Answer 2

It rotates differently than the other planets because it is located on the inside (ring) part of the solar system than the earth is to the sun than us... It is always found near the sun. Mercury does this as well. All of the other planets are on the outside rings and retrograde and such.

Answer 3

The orbit of Mercury is the most eccentric of the major planets, with the planet's distance from the Sun ranging from 46,000,000 to 70,000,000 kilometers. It takes 88 days to complete the orbit. The diagram on the left illustrates the effects of the eccentricity, showing Mercury’s orbit with a circular orbit with the same semi-major axis. The higher velocity of the planet when it is near perihelion is clear from the greater distance it covers in each 5-day interval. The size of the spheres, inversely proportional to their distance from the Sun, illustrates the varying heliocentric distance. This varying distance to the Sun, combined with a unique 2:3 resonance of the planet's rotation around its axis, result in complex variations of the surface temperature.

Mercury's orbit is inclined by 7° to the plane of Earth's orbit (the ecliptic), as shown in the diagram on the left. As a result, transits of Mercury across the face of the Sun can only occur when the planet is crossing the plane of the ecliptic at the time it lies between the Earth and the Sun. This occurs about every seven years on average.

Mercury's axial tilt is only 0.01 degrees. This is over 300 times smaller than that of Jupiter, which is the second smallest axial tilt of all planets at 3.1 degrees. This means an observer at Mercury's equator during local noon would never see the sun more than 1/100 of one degree north or south of the zenith.

At certain points on Mercury's surface, an observer would be able to see the Sun rise about halfway, then reverse and set before rising again, all within the same Mercurian day. This is because approximately four days prior to perihelion, Mercury's angular orbital velocity exactly equals its angular rotational velocity so that the Sun's apparent motion ceases; at perihelion, Mercury's angular orbital velocity then exceeds the angular rotational velocity. Thus, the Sun appears to be retrograde. Four days after perihelion, the Sun's normal apparent motion resumes.


[edit] Advance of perihelion
When it was discovered, the slow precession of Mercury's orbit around the Sun could not be completely explained by Newtonian mechanics, and for many years it was hypothesized that another planet might exist in an orbit even closer to the Sun to account for this perturbation (other explanations considered included a slight oblateness of the Sun). The success of the search for Neptune based on its perturbations of Uranus' orbit led astronomers to place great faith in this explanation, and the hypothetical planet was even named Vulcan. However, in the early 20th century, Albert Einstein's General Theory of Relativity provided a full explanation for the observed precession. Mercury's precession showed the effects of mass dilation, providing a crucial observational confirmation of one of Einstein's theories—Mercury is slightly heavier at perihelion than it is at aphelion because it is moving faster, and so it slightly "overshoots" the perihelion position predicted by Newtonian gravity. The effect is very small: the Mercurian relativistic perihelion advance excess is just 43 arcseconds per century. The effect is even smaller for other planets, being 8.6 arcseconds per century for Venus, 3.8 for Earth, and 1.3 for Mars.

Research indicates that the eccentricity of Mercury's orbit varies chaotically from 0 (circular) to a very high 0.47 over millions of years. This is thought to explain Mercury's 3:2 spin-orbit resonance (rather than the more usual 1:1), since this state is more likely to arise during a period of high eccentricity.[13]

Answer 4

Because a giant rock hit it long ago. It's like playing pool and the sun is the pocket.

Answer 5

It's where womankind came from. It's Venuses prerogative.

Answer 6

Because it's female. We like to be different.

Answer 7

becuase her poles are inverted north is south and south is north