Astrophoto Lab
--- your online source for astronomical & satellite images ---

Mars Opposition -- Dec. 13, 1990
General Information
Special Galleries
Deep Space
Stars, Supernovae
Solar System
Earth from Space
NASA Space Programs
Other Astro Images
Space Image Gallery
Useful Links
Credits & Useage
Name: Mars
Description: 4th planet in the Solar System
Satellites: Deimos, Phobos
Diameter: 6794 km
Mass: 6.42e23 kg
Distance (from sun): 227,940,000 km
Year: 686.98 days
Day: 24.6 hrs
Image Credit: Phil James/university of Toledo/NASA

Click the image to buy a print


The images in this color composite were acquired on December 13, 1990, when Mars was 85 million kilometers (53 million miles) from Earth. This was two and one half weeks after opposition, when the angular size of Mars was about two thirds of its maximum at the best oppositions. The north pole is located near the center of the bright bluish clouds at the top of the image.

When the images were taken it was mid-summer in Mars' southern hemisphere. The thin atmosphere of Mars appears relatively clear of dust over most of the planet. However a thick canopy of clouds obscures the icy north polar regions, as is expected during fall and winter in that hemisphere. As on Earth, the periphery of this polar hood region is the locale of intense storm systems which migrate through northern midlatitudes. Details of the cloud structures in such fronts can be seen in the HST images. Extensive thin clouds in the southern hemisphere are perhaps harbingers of a south polar hood which may form as the martian season slowly changes to fall in the southern hemisphere.

The large, dark, "shark's fin"-like feature which dominates this face of Mars is called Syrtis Major Planitia. This was the first feature identified on the surface of the planet by early terrestrial observers in the Seventeenth Century. It was used by Christian Huygens to measure the rotation rate of Mars - a Martian day is about 24 hours and 37 minutes.

Arabia Planitia, the bright region to the west of Syrtis is thought to be bright because of a thin layer of dust (perhaps amounting to a few meters in thickness) deposited on its surface. This region is heavily cratered, and several of these craters can be discerned in the image.

The bright region to the east, Isidis Planitia, is a 1000 kilometer wide (620 miles) impact basin formed as a result of a large meteoroid collision more than two billion years ago. The basin is bright because it is also thought to be covered with fine dust.

Syrtis Major, which slopes about six kilometers from Arabia down into Isidis, is thought to be dark due to deposits of coarse, dark sand on its surface. Relatively strong winds apparently blow upslope (from east to west), scouring the fine dust from the surface and carrying the dust into Arabia. Viking spacecraft images (obtained from 1976 to 1980) have shown the crest of Syrtis Major to be the location of one or more volcanic vents. Volcanic activity in this area of Mars is thought to have ceased about 2.5 billion years ago, and weathering of the dark volcanic basaltic rock is the source of the dark sand currently covering Syrtis Major.

To the south of Syrtis Major is the bright Hellas Planitia basin. About 1800 kilometers across and nearly eight kilometers deep, it was formed about 3.5 billion years ago by the impact of a large asteroid. Normally the basin is either filled with fog and clouds or the site of prevalent dust storms. This is one of the rare seasons when the weather in Hellas is calm and its surface is visible.

Technical Notes

This color image of Mars is a composite of individual images obtained through red, green, and blue filters using the Planetary Camera. About twelve minutes elapsed between exposing the blue and the red image, leading to a slight amount of rotation of the planet between frames. This is evident as a slightly green rim on the eastern limb of Mars, and a slightly red rim on the western limb.

The image was produced in collaboration with Ed Smith and Dana Berry of the Space Telescope Science Institute using STScI's image processing facilities. Raw images obtained with HST suffer from the blurring caused by spherical aberration in the primary mirror. Because the blurring occurs in a mathematically precise manner, image reconstruction or “deconvolution" techniques can be used to analytically reconstruct the actual, undegraded image. The images used to prepare this color composite were "deconvolved" using the Richardson-Lucy algorithm. Because of background noise, the full HST resolution can't be fully recovered but details within about a factor of two of original specifications can be discerned, exceeding ground-based telescope capabilities.