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Given: Law of Conservation of Angular Momentum.

  • Reverse spinning with dense atmosphere (92 times > Earth & CO2 dominant sulphur based).
  • Surface same degree of aging all over.
  • Hypothetical large impact is not a sufficient answer.

Assuming any object large enough to alter a planets rotation or even orbit would likely destroy most of its shape, yet Venus has retained a spherical property with a seemingly flat, even terrain indicating no volcanoes,and few if any visible meteor impacts. It would be fragmented and dispersed for billions of years. Even the question of what meteor, comet, asteroid composition could survive traveling that close to the sun's temperature, radiation, electromagnetic energy, solar flares, or gravity to equal a mass reactionary change as to alter it's spin.

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Is Venus the only planet/moon to spin in an opposite direction? –  Arjang Mar 31 '11 at 5:50
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""Assuming any object large enough to alter a planets rotation or even orbit would likely destroy most of its shape, "" This assumption is plainly wrong. Any celestial body which exceeds some hundreds of kilometers diameter will adopt spherical form, even when cold or made from diamond. BTW, in case of such an disastrous impact, both bodys would be liquefied very likely. –  Georg Mar 31 '11 at 13:27
    
@Georg suggests that a large portion of matter involved in a theoretical impact would liquefy. Thats more of plausible theory to me. In that in would be a shearing away of more then half the planets mass which would affect the spin given the change in mass and density. Again assuming that part of the planet survived and maintained its original orbit. Could Venus have had a greater mass before? –  tigerskill Mar 31 '11 at 20:40
    
Who knows? Venus' nearly exactly orthogonal axis (with respect to plane of orbit) and low excenticity orbit do not fit to such violent prcesses, I presume. Just too unlikely. –  Georg Mar 31 '11 at 22:07
    
The leading theory for the Moon's formation is a planet-sized body colliding with Earth, yet the Earth is manifestly spherical and this doesn't pose a problem. Given time a large-enough body will settle back into a sphere. It's certainly possible for Venus to have been struck and yet still be a sphere. Given a large-enough impact the entire surface would liquefy, therefore the "same degree of aging" would be found all over. Finally, venus has more volcanoes than any other planet wiki –  Mark Beadles Dec 30 '11 at 16:35

4 Answers 4

Well, I Binged and found some references.

Seems that a collision is most probable, if it happened at a time when the whole system was malleable. But there is no solid explanation.

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You stated the most obvious vague answer on the web with little effort other than a google reference. I can't vote it down since I don't yet have more then 125 reputataion. In fact I suggested clearly that "Theoretical large impact is not a sufficient answer." –  tigerskill Mar 31 '11 at 7:23
    
Dear Tigerskill, I am sorry, I thought I had provided a link, it is hidden under the word "references". From my search, there is no sufficient answer out there, which you could have determined yourself by searching. If there were, it would not be hidden from searches. Venus is not an esoteric subject. –  anna v Mar 31 '11 at 10:55
    
"Theoretical large impact not a sufficient answer" - the argument in the OP is that it is unreasonable given the solidified mass of present Venus. So this linked speculation is that the angular momentum was formed at a time when all the planets had lesser mass/angular momentum than today. After all how do planets get their rotation (and rotation direction) initially? –  Roy Simpson Mar 31 '11 at 12:27
    
@Roy Simpson Yes. It is similar to the dominant hypothesis for the formation of the moon, hypotheses abound and the dominant at present is from a collision at a time when the earth was still malleable ( hence not broken up into pieces). universetoday.com/19718/formation-of-the-moon . A similar hypothesis for the Venus, where it did not break into two but was slowed in its rotation. It is all hypothetical . –  anna v Mar 31 '11 at 12:36
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Interesting links, but what I suspect lies at the core of this question is the "conservation of angular momentum in early solar system" issue. I have seen questions like this before. Here one is asking about Venus. So there have to be angular momentum assumptions in these models, or explanations via N body gravitational chaos physics, tidal effects on rotating gas clouds, etc. Individual collisions between protoplanets are to be assumed and expected too. Then anything retrograde has to be shown to be physically possible. –  Roy Simpson Mar 31 '11 at 13:29

IMO there is no solid explanation, as anna said. Only clues (WP).

In this simulation (2002) Long term evolution of the spin of Venus- II, Numerical simulations we find a mix of: 'chaotic zone', instability, large impact, close encounter, tidal effects, planetary perturbations,...

There is room for speculation:
I think that the heavy atmosphere is not a significant factor of slowing the rotation.
I discarded any violent event because it can easily change more than one parameter; in this case we have only one (the direction).
The planet's minute axial tilt (less than three degrees, compared with 23 degrees for Earth) make me think to keep only the tidal perturbation, although the present configuration Sun-Venus-Earth is not able to justify it.
As the Venusian surface rotates as low as 6.5 km/h (on Earth is about 1,670 km/h) we can think that Venus may have changed the direction of rotation not long time ago.
The solar system angular momentum problem is not solved (the planets strangely have almost all of it) and I think that the solution of this does one is not related to the present question.
The equation 35 of this paper (a new model, undiscussed) allows the slow evolution of the configuration Sun-Venus-Earth.

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There seems a lot of conjecture in any event. Venus could have been a meteor, with an innate spin, that swung by the Sun and have been captured into our Solar systems anticlockwise orbital arrangement. Retaining her original spin momentum, clockwise relative to the others.

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Did you mean to post this as a comment maybe? Please read the faq and the help center –  Pranav Hosangadi Dec 15 '13 at 8:32
    
Hi Ubuntu South Africa. Welcome to Phys.SE. This post (v1) reads more like a comment or a question rather than an answer. To ask a question go here. Update (v2): Greeting and question removed, cf. this meta post. –  Qmechanic Dec 15 '13 at 10:15
    
Hi Ubuntu . Welcome. Your answer sounded like a question. We tend to be more like a class presentation here than a friendly discussion and it has been edited accordingly by the moderator. The answers are supposed to be graded for posterity :) by the up arrows. Now on the content, I think if one calculates the probability for such a large planet to be on its own and pass the sun and be captured the number would come out very small. There do exist rogue planets en.wikipedia.org/wiki/Rogue_planet but the universe is very large and probabilities of falling into orbit small. –  anna v Dec 15 '13 at 18:37
    
I meant the probability of having the correct velocity to be captured into orbit is small , although I have not calculated it. –  anna v Dec 15 '13 at 18:44

This is a very late response, but there is no accepted answer as of yet, and none of the answer quite hit the mark.


Regarding the magical collision hypothesis, that smacks of being rather non-scientific. Scientists as well as Missourians are wont to say, "Show me!" Other than the fact that Venus's rotation is anomalous, what, exactly, is the evidence for a collision with enough oomph to create this anomalous rotation? Even more problematically, this collision hypothesis hand waves away the problem of Venus's thick atmosphere.

Part of the problem here is thinking that the current rotation rates and rotation axes of the terrestrial planets are somehow related to the initial angular momentum of protoplanetary disk from which the planets formed. That may well be the case for the two gas giants in the solar system, but it's not the case for the terrestrial planets. The primordial angular momenta of the terrestrial planets is not a conserved quantity thanks to external torques from the Sun, Jupiter, moons, and other planets. Mercury is in a 3:2 spin-orbit resonance. Mars has suffered chaotic variations in its rotational state due to perturbations from Jupiter. Whatever angular momenta those two planets had initially is long lost. The Earth's Moon has apparently stabilized the Earth's rotation axis, but has sapped its primordial rotation rate. So what about Venus?

Helder Velez's answer to me comes closest to the mark but misses some key points. Helder explicitly discounted Venus's thick atmosphere as playing a role. That Venus has a very thick atmosphere may well be a key part of the answer. Helder referenced the second of two papers published in Icarus on Venus's rotation by Correia and Laskar but did not the reference the first (or the similar Nature article by Correia and Laskar published couple of years prior to those Icarus articles), and Helder did not pay attention to the key point in the Correia and Laskar: Venus rotation is a natural consequence of Venus's thick atmosphere. No collision is needed.

A parsimonious explanation of Venus's rotational state would not need a magical gigantic impact that even more magically did not blow away Venus's primordial atmosphere. This parsimonious explanation is exactly what Correia and Laskar argue happened in their Nature paper and their two Icarus papers. Venus rotates the way it does because this is one of the four final states in which a collision-free terrestrial planet with a very thick atmosphere would rotate. Two of those final states have Venus rotating prograde, the other two, retrograde. The prograde rotational states are statistically unlikely compared to the retrograde rotational states. Venus's thick atmosphere plays a key role in determining Venus's final, stable rotational state.


References:

Correia, A. C., & Laskar, J. (2001). The four final rotation states of Venus. Nature, 411(6839), 767-770.

Correia, A., Laskar, J., & de Surgy, O. N. (2003). Long-term evolution of the spin of Venus: I. theory. Icarus, 163(1), 1-23.

Correia, A., & Laskar, J. (2003). Long-term evolution of the spin of Venus: II. numerical simulations. Icarus, 163(1), 24-45.

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protected by Qmechanic Dec 15 '13 at 10:14

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