alanis: Clouds and shadows on Mars, photographed by Mars Express, 24th May 2012.

Between 28 and 36°S, 284°E, on the arc of highlands that surround the southeast Solis Planum. The crater split between the 2nd and 3rd images is Voeykov, about 75 km across, named for climatologist and geographer Alexander Ivanovich Voeykov (1842-1916). The small, deep crater toward bottom left of the 4th image is Los, named for a village of about 400 people in Gävleborg County, Sweden.

Composite of 3 visible light images for colour, and 5 monochrome images for animation. Colour is not balanced naturalistically, and the slightly psychedelic colours of the clouds are a result of mismatches between the images where the clouds have moved between exposures.

Image credit: ESA. Composite: AgeOfDestruction.

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posting again because the other video is on private

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substitute: Surface of Mars, photographed by Mars Express, 31st May 2007.

84°S 280°E to 75°S 266°E; the top (southernmost) of the image shows the terminus of the Australe Scopuli, fading into Parva Planum.

The vivid violet areas at the bottom of the 3rd and 4th images are where the red channel was blown out; I used the infrared image for this, rather than the (visible) red light image because the latter was even more glitched.

Image credit: ESA. Composite: AgeOfDestruction.

Daedalia Planum

Mars Express imaged Daedalia Planum, a sparsely cratered, untextured plain on the Red Planet featuring solidified lava flows of varying ages. Daedalia Planum lies to the south-east of Arsia Mons, one of the largest volcanoes on Mars. It is 350 km in diameter and rises 14 km. The plain is dominated by numerous lava flows of varying ages. 

Credits:ESA/ DLR/ FU Berlin (G. Neukum)


checkpoint: Surface of Mars, photographed by Mars Express, 11th August 2007.

From about 71°S 285°E to 81°S 277°E; approximately 600 km long and 57 km wide.

At top left, the edge of Schmidt Crater is visible on the northeast edge of Aonia Terra; below, the terrain is cut into by the Cavus Angusti; the brown area is the Planum Angustum; ridged by the Australe Scopuli that surround the south pole.

Composite of visible light images; colours are not naturalistic.

Image credit: ESA. Composite: AgeOfDestruction.

Lava floods the ancient plains of Mars

Two distinct volcanic eruptions have flooded this area of Daedalia Planum with lava, flowing around an elevated fragment of ancient terrain.

The images were acquired by ESA’s Mars Express on 28 November 2013 towards the eastern boundary of the gigantic Tharsis Montes volcanic region, where the largest volcanoes on Mars are found.

The lava flows seen in this image come from Arsia Mons, the southernmost volcano in the Tharsis complex, which lies around 1000 km to the northwest of the region featured here.

This volcanic region is thought to have been active until tens of millions of years ago, relatively recent on the planet’s geological timescale that spans 4.6 billion years.

The rough elevated terrain at the bottom of the main image is imprinted with three distinct but eroded impact craters, the largest of which is about 16.5 km wide and named Mistretta. The ancient foundation it sits on once belonged to the vast southern highlands, but is now surrounded by a sea of lava, like many other isolated fragments.

Lava flows from two distinct eruptions have reached the foot of this particular feature.

The first eruption produced the lava flow to the south of the island (to the left in the image). This flow subsequently experienced extensive faulting due to tectonic forces, resulting in the numerous trough systems.

The younger lava flow (right in the image) must have taken place after the tectonic event that caused the faulting because it overlies both the older lava surface and the tectonic features. Indeed, at the front of the flow, several tongues of lava have flowed preferentially along the lower ground of the troughs.

Another clear indication of the relative ages of the two flows is given by the impact craters: the older, fractured lava flow has more and larger ones than the younger flow.

The younger lava flow also has a rough texture, with many small ridges on the surface. These features form as result of speed gradients within the lava flow due to the difference in temperature between the hot, faster-flowing interior lava and the cooler, slower ‘roof’ of the flow that is exposed to the atmosphere.

But neither lava flow travelled unimpeded. The highland ‘island’ in this scene created an obstacle, forcing them to circle its flanks and override its base, most noticeable to the north.

The wider Daedalia Planum region bears witness to numerous lava flows similar to these, each one overlaying the last. By carefully studying the boundaries between overlapping flows, planetary scientists can build up a picture of the eruption history of the Red Planet’s giant volcanoes.

Image credit: ESA/DLR/FU Berlin

Hello everybody!

So as you can see, the pictures of Les Twins @ the CPH are all marked with ‘www.planum.dk' - which is the studio that hosted the workshop!

Now planum has a tumblr, with the purpose to expand the planum dance community wider, and hopefully inspire more around the world. There are gonna be more to it than just dance, but that is for the future. 

Right now, since it’s very new (its gonna look a lot better in the future) there are gonna be mainly pictures from the twins’ CPH workshop, hopefully a video of it  soon and more. So if you would like to support, give PLANUM’s blog a follow and/or share this so we can build a nice network of amazing people to share the love of dance with! (Click here to follow) 

Thanks in advance! 

Love you guys, xoxo

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Nicky Andersen!


crow: Clouds on Mars, photographed by Mars Express, 4th October 2010.

36 to 43°S, 274 to 276°E on the highlands south of Solis Planum. The Coracis Fossae are somewhat visible at right running vertically down the image.

Coracis is derived from corax, the Latin name of the raven; thus the scientific name of the common or northern raven, Corvus corax.

Animation of 5 monochrome frames, colourized with a composite of 3 visible light images. The colour balance is not naturalistic, but probably close enough here.

Image credit: ESA. Animation: AgeOfDestruction.

Explosive crater twins on Mars

Dramatic underground explosions, perhaps involving ice, are responsible for the pits inside these two large martian impact craters, imaged by ESA’s Mars Express on 4 January.

The ‘twin’ craters are in the Thaumasia Planum region, a large plateau that lies immediately to the south of Valles Marineris, the largest canyon in the Solar System.

The northernmost (right) large crater in this scene was officially given the name Arima in early 2012, but the southernmost (left) crater remains unnamed. Both are just over 50 km wide and display intricate interior features.

Multiple terraces slump from the crater walls onto a flat floor, but perhaps the most striking feature is the central pit, a feature it shares with Arima crater to its north.

Though the large craters in this scene have similar diameters, their central pits are rather different in size and depth, as is clearly evident in the topographical map. Compared to the Arima crater, perhaps more subsurface ice was present and more readily vapourised in the southern crater, punching through slightly thinner crust to leave a larger pit.

Many neighbouring small impact craters also show evidence for subsurface water or ice at the time of impact as evidenced by their ‘rampart’ ejecta blankets.

Image credit: ESA/DLR/FU Berlin (G. Neukum)