A massive cover-up

Venus is our closest neighbour both in terms of distance and size. It is also a very alien world with surface temperatures of 46O °C and clouds of sulphuric acid.

To get an idea of what the surface of Venus looks like we have to use radar to see through the thick clouds and build up a topographic model, and what we see is a world with features which are in many ways similar to our own.

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Left the mountain range Akna Montes on Venus (NASA/JPL) right Parra Mountains Mexico (JSC)

Mountain ranges, showing folded and faulted rocks structures surrounded by large flat plateaus, are very similar to the mountain chains on Earth. Rifts, which are cracks in the surface of the planet along which volcanoes generate new crust are found on both planets. Large volcanoes are found all over the surface.

However whilst the features seem similar on the surface, there distribution there are stark differences: on Earth, these are linked to plate tectonics, rifts form where plates move apart or break up. Mountains form as the crust crumples as these plates collide. There are also deep trenches such as the Mariana trench, linked to subduction as plate sinks down back into the mantle as a recycling of the surface. The only major features not caused by plate tectonics are hotspot volcanoes such as Hawaii. Even  these hotspots, show the fingerprints of the movements of plates, which causes them to form chains of volcanoes as the plates move over the source creating lines of islands on the surface of the Earth.

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Hawaii islands, formed by the movement of the plates over a hot-spot (JSC)

On Venus, the volcanoes do not form hotspot chains like those on Earth but instead appear at random all over the surface. Whilst both trenches and rifts are seen they are isolated and discontinuous. In short, just like with Mercury, it is a one plate world without plate tectonics.

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Maat Mons, a 3d topographic model of a volcano on Venus (NASA/JPL)

However, unlike Mercury,  Venus’ surface has very few scars from the harsh environment of the solar system. Earth gets rid of it craters through tectonic processes and water eroding them away. Venus, without water or tectonics, has a very young surface with hardly any craters, which suggest that the majority of the surface is less than 500 million years old (very young in solar system terms).

To understand why this is and why Venus seems to have a universally young surface (even parts of Earth’s surface can be several billion years old) we can look at a side effect of plate tectonics: heat removal. the generation of crust at ridges allows heat to move to the surface and be emitted. Without this plate tectonics, heat builds up under the surface over time. If heat builds up over time, it is possible that a layer of hot rock builds up and the hard crust gets thinner as it warms and softens from the underneath and melt.

It is possible that heat may build up and cause occasional sudden and larger scale volcanism over the majority of the planet, covering much of old surface with a new one, erasing the craters, mountain and rifts and allowing new features to form. Whilst this destruction of features hides the history of Venus, it also provides fascinating insights to our nearest but very different planetary neighbour.

 

The world is getting smaller every day

For the smallest of the planets, Mercury is a surprisingly active place with a complex internal structure and magnetic field, however, it’s tectonics is dominated by its size.

Smaller bodies lose heat a lot faster than bigger bodies, due to a higher ratio of surface area to volume, this means that Mercury has cooled relatively rapidly. As the planet cooled it has shrunk. Estimates for this contraction of its radius range from  ~2 – 7 km over its lifetime, whilst this is only 0.2% of its total radius, this equates to its diameter shrinking   44 km at its equator.

Mercury’s surface is a single tectonic plate, it doesn’t have the subduction and rifting zones which can accommodate strain. As the planet has cooled and contracted the crust at the surface has become compressed as the larger diameter crust is pulled in to fit into a smaller area. Rocks when under compression buckle and eventually break and form faults. In the case of Mercury, shallow angle faults known as thrust faults are created. As one part of the crust rides over another it forms cliffs (called “Rupes”) which can be 100’s of km long and several hundred meters high.

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Carnegie Rupes, 2 km high wall running diagonally across the image created by a thrust fault (NASA/Johns Hopkins University Applied Physis Laboratory/Carnegie Institution of Washington)

Where multiple faults interact they can produce complex structures. The Great Valley is 1000 km long valley formed from thrust faults which make up either side and has been bent downwards in the middle.

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The Great Valley (in Blue) close to Rembrandt basin on Mercury, (Nasa/JHUAPL/CIW/DLR/SI)

Smaller scale scarps have also been identified, whilst smaller (10’s of km long and 10’s of meters high) they are often found cutting across small impact craters and smooth younger planes which means that these features are less than 50 million years old and suggests that Mercury is still tectonically active now.

 

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Smaller scarpes from recent tectonic activity, (NASA/JHUAPL/ Carnegie Institution of Washington/Smithsonian Institution

 

Whilst there are other features such as some structures on its surface which are linked to thicker patches of crust probably linked to mantle structures Mercury is dominated by the side effects of being a small cooling planet which is still slowly shrinking.

Earth’s plates

No body is perfect; forces on both the inside and outside of them push and pull them around. This leads to cracks and wrinkles on surfaces which represent the passage of time. On planetary bodies, this is referred to as tectonics.

Most bodies have tectonic features spread out over their surface. Earth is different. The surface is divided up into interlocking blocks which move around over time, called tectonic plates. These plates are constantly moving: colliding, separating or moving past each other, this movement causes the majority (but not all) of earthquakes and volcanoes on the Earth. The vast majority of tectonic features are related to either current or historical plate boundaries.

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The Earth’s tectonic plates, courtesy of the U.S. Geological Survey

The driving force behind plate tectonics is dominated by the gradual overturning of the mantle as it moves heat from the core to the crust in a process called convection. The plates are also pulled by old cold crust sinking down and pulling the plate with it.

These forces linked to the moving of plates transfer stresses through the crust and lead to the rocks deforming. On a large scale, this leads to several features on the Earth’s surface which can be seen from space. In future posts, we’ll look at some of the features on other planets but first, let’s have a look at a few features formed by plate tectonics on the  Earth:

Faults

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A fault offsets banded rock south of the Tien Shan mountains as seen by Landsat 8 (USGS/NASA)

Faults are breaks in rocks along which movement occurs and are associated with earthquakes. They release strain built up in the crust and are found on all plate margins, including those that slide past each other like the San Andras fault. These are often seen as breaks and offsets in geological patterns.

Rifts

In areas where the crust is under tension it can be pulled apart, the rocks break into a series of faults, which form a staircase-like feature dropping down to form a valley. As the crust gets thinner as it is pulled apart it enables volcanism to start and volcanoes form along the valley (such as in the East African Rift valley).

This rifting can continue and the crust can break into two separate plates. with a volcanic ridge in the middle which generates new crust as the two sides move apart. These features form the seas and the oceans.

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East African rift valley, formed by multiple faults (seen as lines going diagonally across the image) which lead to low lying areas as the plate thins  (NASA/JPL)

Mountains

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Mt Everest and other mountains as seen from STS-066 (NASA, JSC)

In areas where plates collide with each other, the outcomes vary depending on the type of crust colliding.  If it involves a thinner denser crust called oceanic crust (which is the type generated by mid-ocean ridges) subduction occurs – an oceanic plate will be forced down and sink into the mantle. This activity leads to a trough and then a line of volcanoes behind them. Where two pieces of thicker, less dense continental crust collide the parts crash into each other they crumple rather thank sink and form mountain ranges such as the Himalayas.

Earth is unique with its highly active plate tectonic system defining its surface, other planets have been and are tectonically active but in different ways with features spread out and controlled by different tectonic systems.

Scarred faces

The Colorado River slowly cutting its way through rock over millions of years has formed a 450 km long, and 1.8 km deep canyon called the Grand Canyon. Whilst up close and even from space it looks impressive, in reality, it’s fairly small compared to other features which scar the planets across the solar system. Today, we’ll look at the three largest rifts and canyons in the solar system.

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The Grand Canyon in the south if the image at seen from the ISS (NASA)

Valles Marineris on Mars at 4000 km long is 9 times as long as the Grand canyon and stretches 1/4 of the way around the entire planet. There are a few theories about how it formed, the most prominent is that the nearby Tharsis bulge (an area which hosts the tallest volcano in the solar system) caused tension in the crust, which lead to it tearing and pulling apart, in a process known as rifting. Erosion then would have deepened the valley further and has produced outflow channels at the end of it.

 

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Valles Mariners, Mars (NASA)

 

One Venus, Baltis Vallis is even longer at nearly 7000 km long, its ends are covered so its original length is unknown. This feature, like the Grand Canyon, was also likely formed by erosion. Instead of water, high-temperature lava flows would have torn up, melted, and dissolved the surfaces as they flowed over them, slowly wearing them away in the same way rivers do on Earth. Similar features were probably once present on the early Earth, Komatiite lavas, found in Australia also show signs of eroding the rocks beneath them and forming channels as they flow through an area.

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a 600km segment of the 7000 km Balits Valley from Radar data collected by Magellan, the channel can be seen as a meandering line going diagonally across the image arrow to arrow (NASA/JPL_

However, the largest in the solar system is right here on Earth the 10’000 km long and up to 8.5 km deep Atlantic Ocean is a large cut into the Earths Surface. Like Valles Marineris, this was formed by rifting rather than a valley. Tectonic forces pulling and pushing Europe and Africa away from the Americas. Plate tectonics allowed the rift to develop much further and volcanism generated new oceanic crust was generated in between the two.

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Bathymetric image of the Atlantic ocean (NOAA)

This quick overview of the largest valleys and rifts in the solar system highlights two main processes which can form them; erosion and tectonics. Volcanism on Venus and Mars, extensional forces tearing the crusts show these planets have been tectonically active. In the next few posts I’ll examine tectonics work across the solar system.

The Anti-Crust

Most people know that the Earth can be divided up into layers, starting with the crust – a skin of hard rock on the surface. Beneath this crust is the mantle; silicate rock which, although solid, moves very slowly over time; convecting and moving heat up to the surface. Beneath this mantle is the core. The Earth’s core is comprised of two parts. The outer core is liquid metal which is spinning away generating the magnetic field for the Earth. The innermost layer is the inner core. A solid lump of iron and nickel.

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Mercury, the smallest of the rocky planets (It’s smaller than the moons Titan and Ganymede) but is very dense (denser than both Venus and Mars even though they are bigger). Whilst Mercury is not as dense as the Earth it is much smaller so it doesn’t compress the material inside as much, its high density is best explained by a much bigger iron core and a smaller silicate mantle/crust compared to the Earth.  Mercury is also the only other rocky planet other than Earth to have a strong magnetic field, which tells us about the internal composition of the core.

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Comparison of Earth Mercury sizes (Earth image: Nasa, Mercury: NASA – APL)

The magnetic and gravity data from Nasa’s MESSANGER probe suggests that it has a crust of about 50 km thick, beneath which there is a mantle, and beneath that we know there is a  core at the centre, as shown by the strong magnetic field and the high density.

This core, like Earth, will likely have a solid inner part and then a liquid outer part, made of iron & nickel.  As the core cools it solidifies in the middle and iron and nickel is removed from the liquid part, causing a relative increase in the other elements such as sulphur, silica, and oxygen left in the liquid. Depending on the composition this mix of different elements may become like oil and water. A sulphur – iron mix separates out from the rest. This sulphur mix is less dense than the rest and floats up to the core-mantle boundary.

The iron-sulphur mix solidifies and forms a hard layer on the underside of the mantle – this is the anti-crust, a thick layer of iron sulphide separating the liquid outer core from the silica-rich mantle.

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Gravity studies of the planet made by looking at small changes in the MESSENGER spacecraft as it orbited suggest that this layer may be present, however, there are a lot of variables to the models used to estimate this. Whilst on Earth seismic studies could be used to verify these, there are no plans to land a probe on Mercury anytime soon to undertake such tests, slight changes in the amounts of Sulpher and other elements could have prevented the formation of the anti-crust.

Whilst the smallest planet in our solar system Mercury has many similarities to that of Earth, the anti-crust is an extra layer and an interesting artefact from cooling worlds.

 

 

Into the Exosphere!

Last time I talked about the different ways rocks breakdown in the space environment. This time we will look at what happens to some of these products of the erosion and weathering of the materials go.

Whilst many of the smaller bodies in the solar system don’t have an atmosphere (which would stop most space weathering), there is still atoms/ions/dust particles floating around above the surface. Whilst this material is too spread out to interact with each other in the way that a gas does in an atmosphere, these materials are still trapped, bound by the gravity of the body – this is called the exosphere.

Unlike other bodies, these exospheres are predominantly comprised of material generated from space-weathering; sputtering releasing atoms, and melting which releases volatile molecules. Some are released from surfaces by heating at sunrise. As the solar wind of charged particles moves over a body, its surface can become charged, dust particles gain a similar charge and so are repelled floating above the surface. The amount of dust is linked to the number of micrometeorite impacts, the intensity of the solar wind, and any magnetic fields. This dust can refract light; giving the appearance of a diffuse sunrise which would otherwise not be possible on an airless world.

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Lunar Horizon Glow on the Moon, generated by dust in its exosphere, taken by Nasa’s Clementine mission (NASA)

For rocker bodies, such as Mercury and the Moon atoms of  Ca, Mg, & K have been detected. For some of the other bodies in the solar system, beyond the frost line – water ice covers many of the bodies like Europa and Enceladus, when the surfaces are broken down by radiation, the hydrogen escapes, leaving oxygen and hydroxide around them.

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The Calcium and Magnesium tails of Mercury as taken by MESSANGER (NASA/Johns Hopkins/ Carnegie institution

These materials don’t stay in the exosphere forever, s0me can be reabsorbed by the surface of the planet, often on the night side of a planet, and the dust and atoms can settle down. Atoms can become charged by sunlight (photo-ionisation), or interaction with charged particles in the solar wind. These ions are caught by solar winds or by magnetic fields and expelled out into interplanetary space or fired at high speed into the ground close to the poles. The force of sunlight hitting atoms or the rare collisions between atoms can slowly add momentum until some material eventually gain enough velocity and can escape the exosphere.

Weathering without any weather

I’ve been reading up on weathering on airless bodies (those without atmospheres) at the moment and so thought I would write a brief overview of the processes which break down rocks in space.

On Earth when we think about weathering as the breakdown or rocks/minerals/soils in situ by physical actions (such as wind, temperature changes, wave action, and biological action) or by chemical action (dissolution, or oxidation like rust).

For many of those physical and chemical actions an atmosphere is needed (life and liquids can’t survive long without an atmosphere) without one weathering occurs by different processes – collectively known as space weathering.

Space weathering is caused by the flow of energetic particles, rays, and fragments of rocks and comets bombarding the surfaces or objects as well as extreme temperature changes. Normal atmospheres do a lot to reduce the impact these influences, but without air to slow them down they impact the surfaces of these bodies and break them down.

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Airless world Mercury is a large body subject to space weathering (NASA/JHUAPL/CIW)

One of the key weathering mechanisms is micrometeorite impacts, these are small (<1 cm) fragments of asteroids and comets, which collide with surfaces and smash them up, forming a layer of broken rock fragments, called regolith, which varies in thickness and size based on the underlying rock types, the length of time a surface is exposed, and the size of a body. The bigger a body is the stronger the gravitational force and the greater the acceleration of particles hitting them and so the higher energy the impact. Impacts also mix-up the regolith bringing material at depth to the surface where it is more exposed to radiation, this mixing progress is called gardening.

These high speed impacts generate a lot of heat which can melt some of the rocks and cause loss of volatile components as well as cause the formation of glasses. The impactors make up a significant amount of material in the regolith, with between 5-20% of the regolith on Mercury estimated to be made from macrometeorites which have impacted the planet.

The other main source of space weathering is radiation, cosmic rays, solar particles, and sunlight, bombarding the unprotected surfaces. Ions caught in solar winds can be implanted into crystal latices or the impact can be of such high energy that it knocks out lighter elements from rocks (a process known as sputtering). Differential heating caused by the day and night cycles can cause fracturing and lighter elements can be lost through heating, in a process called thermal desorption, a key process and one of the main mechanisms behind comments getting their tail.

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Space weathering and erosion in action on a comet (K. Jobse / P. Jenniskens /NASA Ames

These process add up together to cause the reduction of size, and the loss of volatile elements, chemically this leads to reduction which causes the formation of microscopic iron fragments in the regolith and on the edges of glass fragments.

All these minor alterations mean that the surfaces of bodies can be of a different composition to the underlying rocks and this must be taken into account when analysing satellite data to work out what a body is comprised off. Next time we’ll have a look at where some of the eroded products end-up: The Exosphere, but for now if you are interested in this, more detailed overview can be found here.