The Images of Venus They Didn't Show You in School | Our Solar System's Planets

Venus is a beautiful, elegant planet; seemingly  very calm and almost tranquil on the surface, wrapped in a soft cloud like a blanket.  From an outsider’s perspective, it’s clear why it’s named Venus, the Roman  god of Love. But go beneath the cloud layer, and you’ll find quite the opposite.

Scorching  temperatures, volcanism and a crushing atmosphere are what you'd actually find on the surface. There are few places in our solar system more deadly, and its acid-laced environment  makes visiting next to impossible. So what do we know about this beautiful yet  hellish planet?

More than you might think. Hi I’m Alex McColgan, and you’re watching  Astrum. Join me today as we delve into what makes this planet so unique in our solar  system.

Get ready to find out everything you could want to know about Venus. Let’s start by stepping back a bit to see where this planet fits into our solar  system. Venus is the 2nd planet from the Sun and it’s our closest neighbour.

Its average  orbital radius around the Sun is 0. 72AU or roughly 108 million kms. It doesn’t vary  much at all from this mean orbital radius, as it’s the planet with the least eccentric orbit,  orbiting nearly in a perfect circle.

At Venus’ closest approach to us, it is the closest of any  other planet, being only 41 million kms away. Interestingly though, this is not when it’s  brightest in our sky, as when its closest to us, we only see the night side as it’s between us  and the Sun. It is still visible though as the sunlight refracts through the atmosphere.

It’s  actually brightest when it’s a thinner crescent shape in the sky, and when this happens, it is  the brightest object we see at night after the moon. As such, Venus is commonly misreported as  an "unidentified flying object". U.

S. President Jimmy Carter reported having seen a UFO in 1969,  which later analysis suggested was probably Venus. Countless other people have mistaken Venus  for something more exotic due to its startling brightness.

I recently had the pleasure of looking  at Venus through a telescope and remarkably the crescent shape of it was very visible. With Venus orbiting between us and the Sun, it may make you wonder if Venus ever eclipses the  Sun from our viewpoint on Earth, and the answer is yes, but surprisingly, very rarely. Transits  happen in pairs, the pairs being 8 years apart, but every pair only happens once every 100 or  so years.

The last transit we had was in 2012, but if you didn’t see that I’m afraid the  next one won’t be until 2117. The reason for this rarity is because the orbiting plane of  Venus is not exactly the same as Earth’s. Also, Venus only catches up with Earth every 584 or  so days.

These two things combined ensure that, although a spectacular and predictable sight,  it also means we’ll probably only ever have the chance to see it once or twice in our lifetimes. All the planets orbit anticlockwise around the Sun and with this, Venus is no different. But unlike  all the other planets, it rotates clockwise, or in other words in a retrograde rotation.

Not  only that, but it has an extremely slow rotation, rotating once every 243 Earth days – slower than  any other planet. This makes a sidereal day longer than a Venusian year, a Venusian year lasting 224  Earth days. A sidereal day, if you remember from my recent Mercury episode (which you can check  out here, if you missed it), is one rotation of the planet.

Because of this retrograde rotation  however, a solar day (which is sunrise to sunrise) is considerably shorter, at 117 Earth days. This  means you’d only experience just less than 2 days on Venus in one year. I just want to give you  some perspective as to how slowly it rotates; at the equator the planet is only rotating at  6.

5km/h! This slow rotation makes it the second most spherical object in the solar system, after  the Sun. It is unclear why Venus rotates backwards compared to the rest of the planets, but it  could be due to a big impact with another object billions of years ago, or tidal locking with the  Sun, or tidal effects on the Venusian atmosphere.

Its mass and size are very similar to our  Earth, hence why it’s often referred to as our sister or twin planet. Venus is one of  the four inner terrestrial planets and it is a rocky planet. Its diameter is slightly smaller  than Earth’s at 12,100km compared to Earth’s 12740km, and its density is 5.

3 g/cm3  compared to our 5. 5 g/cm3. This means the gravity on Venus is only a tenth weaker than  that on Earth; surface gravity being 8.

9 m/s2. But this is where the similarities end. Because  on the surface of Venus, the atmosphere pressure is 92 times greater than that on Earth.

That’s  an equivalent of 1km under Earth’s oceans. The reason for this is because the density of  Venus’ atmosphere is 93 times greater than Earth’s. And fit that amount of gas into a space  slightly smaller than what we have here on Earth, and you can understand why it’s so densely packed.

The atmosphere consists mainly of CO2 gas, and combined with sulphur dioxide clouds, you’re left  with the strongest greenhouse effect in the solar system, with temperatures of 462°C at the surface  on average. This makes the surface temperature greater than Mercury’s, even though Mercury is  closer to the Sun, and Venus only gets 25% of the solar radiation that Mercury does. The difference  is that Mercury doesn’t have an atmosphere to retain the heat, whereas Venus certainly does. 

This means at night time and even at the poles, the temperature remains fairly constant. Venus really is cooking; it absorbs so much heat. But like a thermal flask it retains  it and doesn’t let much escape.

With an axial tilt of only 3 degrees, it also means seasonal  changes in temperature are also very minimal. Wind speeds aren’t very high on Venus’s surface,  only being a couple of kilometres an hour, but because of the thickness of the atmosphere it  applies a strong force on the obstructions, moving small rocks and dust across the surface. On the  other hand, wind speed at the cloud layer is much faster, reaching speeds of 300km/h.

These winds at  the cloud tops circle the planet about every four to five Earth days which makes the planet look  like its rotating a lot faster than it actually is. The cloud layer itself sits above the thick  CO2 and consists mainly of sulphur dioxide and sulphuric acid droplets. Sulphuric acid, just as a  side note, is highly corrosive and this acid rain just adds to the hellish nature of Venus, although  it does evaporate before it hits the surface.

The clouds on Venus are highly reflective, only  allowing about 10% of the sunlight through, and because they cover the entire planet, it  obstructs a visual view of the surface from space. These clouds are also capable of producing  lightning much like on Earth, although it’s not as common. Recently it has been discovered that  Venus has a large vortex at the South Pole much like on Saturn.

Now Venus is the image on the  left, and Saturn on the right. They are shaped quite differently, and Venus only has one storm,  whereas incredibly every single black dot in the Saturn image is a separate storm, with the main  vortex being in the centre. The vortex on Venus is at an altitude of 59km which is just above the  cloud deck.

Which leads on to an interesting point about the atmosphere of Venus. Because at about  50km up, the air pressure and temperature would be are tolerable byfor Earth standards. Even  the gravity would feel very much like Earth.

The only problem with a person actually being  there is the air itself. But if you were to have an airtight plane or something like this, the  conditions would actually be very Earth like. Now I want to head back down to the surface  of Venus a little bit, as we actually have some real photos of the surface thanks to the  pioneering efforts of the Russians back in the 60s to 80s.

The probe Venera 7 in 1970 was the  first probe to ever land on another planet and send data back, the previous attempts resulted in  the probes signal terminating before touchdown. Venera 7 probably fell over on impact, and so  the only reading it gave was the temperature at the surface, which was 475 degrees. Venera 8  confirmed that at the surface the visibility was quite clear, with a visibility range of about  1 km, as the cloud layers end at quite a high altitude meaning it was suitable for cameras in  future missions.

Venera 9 sent back the first ever image of the surface of Venus. Venera 10, 13  and 14 over the course of 6 years sent back more imagery, this time in colour, as well as a lot  of data regarding the conditions of the planet. Since then, there have been a number of probes  that have mapped out the surface of Venus.

Using radar, they’re able to see through the cloud cover  and see imagethe planet’s landscape in very high definition. The surface of Venus is dotted with a  lot of big, but not necessarily active volcanos. It has 167 volcanos which are over 100km in  diameter.

The only complex of this size on Earth is the big island of Hawaii. This doesn’t  mean Venus is more volcanically active than Earth, but this is due to the fact that Venus has  a much older crust than on Earth. Earth has plate tectonics releasing heat and renewing  the surface fairly regularly, (“regularly” at least being 100 million years).

Venus on the other  hand doesn't have any plate tectonics. Instead, its crust is estimated to be about 300-600 million  years old, when a global resurfacing event likely occurred. The theory is that the mantel under the  crust heated up so much that it forced its way up through the crust, covering most of the surface  with lava.

An incredible 80% of Venus' surface is made up of cooled lava plains, and there are  literally hundreds of thousands of volcanos in one form or another. There are also 900 impact  craters to be found on Venus, although none less than 3 km in diameter. This is because anything  smaller than 50m in diameter would fragment and burn up before it even hit the surface.

And finally let’s have a look at the magnetosphere. Venus doesn’t have its own  magnetic field, which surprised everyone when it was first discovered as Venus’ composition is  very similar to Earth’s. But without more data, it’s hard to say why this might be; although a  study in the Journal “Earth and Science Planetary Letters” 2017 suggested that perhaps it was  to do with the absence of a massive impact in Venus’ history.

Earth had at least one massive  impact – it’s what formed the Moon, and it’s possible it played a part in kick-starting  our magnetic dynamo. But Venus never had such an impact – perhaps this explains the lack of a  similar field? Regardless, as a result of this, solar and cosmic radiation interacts a lot with  the upper atmosphere of the planet, producing lightning and an induced magnetosphere.

Solar wind  also strips off the low-density molecules out of the atmosphere meaning that Venus has a tail,  similar to a comet. Under certain conditions, this tail can tickle Earth when they are in  conjunction with each other. Unfortunately, this tail isn’t visible with the naked eye.

Sadly, we've come to the end of the video. But I'd just like to say thank you so much  for watching this far. And if you enjoyed it, I have a lot of other videos about our other  planets which may be of interest to you as well.

So be sure to check those out! Our Solar System  is filled with some truly incredible sights, and there’s always more to discover. But for now,  thanks again for watching and see you next time.