Satellites Could Help Predict Landslides

Image credit: ESA
As winter rains come, thousands of square kilometres of territory across Europe’s heart face a looming threat: steep slopes and waterlogged soils combine to trigger landslides.

A build-up of groundwater within a slope increases its weight and decreases its cohesiveness, weakening the slope’s ability to resist the remorseless pull of gravity. The heavy earth flows downward. For all in the path of a landslide the results are devastating, and frequently lethal.

“In Italy, landslides have claimed an average of 54 victims per year during the last half century,” says Nicola Casagli of Italy’s National Group for Hydro-geological Disaster Prevention (GNDCI),a research network working with Italy’s Civil Protection Department.

“The extreme rainfall of our climate, our mountainous geography and recent uncontrolled urbanisation of unstable land makes us one of the countries most affected by landslide hazards. The total cost of direct damage done by Italian landslides is estimated at between one and two thousand million Euro per year.”

Very gradual ground shifts are known to precede more major landslides. Often these are on a scale of millimetres ? too slight to even be noticed by local observers, but enough to be detected via satellite using a powerful technique called radar interferometry.

It involves mathematically combining multiple radar images of the same site – acquired using instruments such as the Synthetic Aperture Radar (SAR) aboard ESA’s ERS spacecraft – in such a way that tiny changes in the landscape occurring between images are highlighted.

This technique is the basis of a new project called Service for Landslide Monitoring (SLAM), enabling landslide susceptibility mapping across parts of Italy and Switzerland, two of the European countries most under threat. GNDCI is one of three national-level users working with SLAM, along with Italy’s Ministry of the Environment and Switzerland’s Federal Office for Water and Geology (FOWG).

“Surface movements assessed over wide areas are one of the best indicators of landslide activity, and can be employed for risk forecasting,” added Casagli. “Extremely slow movements usually occur for several weeks or months before a sudden collapse.”

Trial services are being provided across Italy’s Arno river basin as well as a section of the Campania region. In Switzerland the service covers the eastern Valais and Berne cantons.

“Our interest is to have a tool evaluate landslides and mass displacements all across the Swiss Alps,” explains Hugo Raetzo of FOWG. “About 8% of Swiss territory is vulnerable to landslides, making up thousands of square kilometres. The annual landslide frequency varies with the weather ? heavy rainfall can potentially re-accelerate existing landslides.”

Three different service products are available: a large-scale Landslide Motion Survey identifying areas affected by landslides across an entire river basin, a reduced-scale Landslide Displacement Monitoring measuring ground deformation over particular sites of interest, and Landslide Susceptibility Mapping which merges the previous data products with thematic maps of land use, slope, geomorphology and other relevant parameters to provide geological hazard maps.

More than a decade’s worth of ERS data archives are being exploited to derive SLAM products. These products disclose new and essential information to the institutions charged with landslide risk and hazard management. Benefits from the service include the identification and characterisation of displacements both known and previously unknown and the verification of remedial interventions performed in the past to stabilise particular landslides.

The SLAM service is being formally implemented in February and will run until the end of this year. It is entirely funded as part of ESA’s Data User Programme and is carried out by an international consortium led by Planetek Italia with five other partners: Tele-Rilevamento Europa, Gamma Remote Sensing, Spacebel, Geotest and Florence University.

Original Source: ESA News Release

Columbia Astronauts Get Mountains on Mars

Image credit: NASA
NASA Administrator Sean O’Keefe today announced the martian hills, located east of the Spirit Mars Exploration Rover’s landing site, would be dedicated to the Space Shuttle Columbia STS-107 crew.

“These seven hills on Mars are named for those seven brave souls, the final crew of the Space Shuttle Columbia. The Columbia crew faced the challenge of space and made the supreme sacrifice in the name of exploration,” Administrator O’Keefe said.

The Shuttle Columbia was commanded by Rick Husband and piloted by William McCool. The mission specialists were Michael Anderson, Kalpana Chawla, David Brown, Laurel Clark; and the payload specialist was Israeli astronaut Ilan Ramon. On February 1, 2003, the Columbia and its crew were lost over the western United States during re-entry into Earth’s atmosphere.

The 28th and final flight of Columbia was a 16-day mission dedicated to research in physical, life and space sciences. The Columbia crew successfully conducted approximately 80 separate experiments during their mission.

NASA will submit the names of the Mars features to the International Astronomical Union for official designation. The organization serves as the internationally recognized authority for assigning designations to celestial bodies and their surface features.

An image taken by the Mars Global Surveyor Mars Orbiter Camera of the Columbia Memorial Station and Columbia Hills is available on the Internet at: http://www.jpl.nasa.gov/mer2004/rover-images/feb-02-2004/captions/image-10.html.

For information about NASA and the Mars mission on the Internet, visit: http://www.nasa.gov.

The Jet Propulsion Laboratory, a division of the California Institute of Technology, Pasadena, manages the Mars Exploration Rover project for NASA’s Office of Space Science, Washington, D.C. Additional information about the project is available on the Internet at: http://marsrovers.jpl.nasa.gov.

Rosetta Launch Date Approaching

Image credit: ESA
The countdown to Rosetta?s rendezvous in space began on 1 March 1997. At the end of February 2004, seven years and not a few headaches later, the European Space Agency (ESA) probe will at last be setting off on its journey to meet 67P/Comet Churyumov-Gerasimenko.

The long-planned get-together will not however take place until the middle of 2014. A few months after arriving at the comet, Rosetta will release a small lander onto its surface. Then, for almost two years it will investigate Churyumov-Gerasimenko from close up.

Dr Gerhard Schwehm, lead scientist for the Rosetta project, explains that, ?With this mission we will be breaking new ground – this will be the first protracted cometary encounter.? The trip to the meeting place in space will certainly be a long one, located as it is some 4.5 astronomical units from the Sun, which translates into something like 675 million kilometres. Rosetta will be on the road for ten years, during which time it will clock up in excess of five billion kilometres.

Launch in February 2004
Rosetta will be waved off on 26 February when it lifts off from the space centre in Kourou, French Guiana, aboard an Ariane 5 launcher. Shortly after the spacecraft?s release, its solar panels will be deployed and turned towards the Sun to build up the necessary power reserves. Its various systems and experiments will be gradually brought into operation and tested. Just three months into the mission the first active phase will be over, followed by final testing of the experiments in October 2004. Rosetta will then spend the following years flying a lonely path to the comet, passing by the Earth, Mars, the Earth and the Earth again.

There is no alternative to this detour, for even Ariane 5, the most powerful launcher on the market today, lacks the power to hurl the probe on a direct route to the comet. To get the required momentum, it will rely on swing-by man?uvres, using the gravitation pull of Mars (in 2007) and the Earth (three times, in 2005, 2007 and 2008) to pick up speed.

Asteroids for company
A change is as good as a rest, and a meeting with at least one asteroid should help break the monotony for Rosetta. The spacecraft will come close to an asteroid at the end of 2008. Asteroids are, it will be remembered, rocky bodies, some as large as mountains, some even larger, that orbit the Sun in much the same way as planets.

?These ?brief encounters? are a scientific opportunity and also a chance to test Rosetta?s instrument payload,? says Gerhard Schwehm. But asteroid exploration also serves an entirely practical purpose: ?The more we find out about them, the better the prospect of being able one day to avert a possible collision.? Following a period of low-activity cruising, the probe?s course will be adjusted one last time in May 2011. From July 2011, a further two-and-a-half years’ radio silence will be observed, and Rosetta, left entirely to its own resources, will fly close to the Jupiter orbit.

Link-up in 2014
Finally, in January 2014, the probe will be reactivated and will, by October 2014, be only a few kilometres distant from Churyumov-Gerasimenko. This is where the dream of so many scientists becomes reality. Having deposited its precious lander cargo on the comet?s surface, Rosetta will continue to orbit Churyumov-Gerasimenko and together they will spend the next seventeen months flying towards the Sun.

Rosetta was built by an international consortium led by Astrium. The lander probe was developed in Cologne under the aegis of the DLR, Germany?s space agency, with contributions from ESA and research centres in Austria, Finland, France, Hungary, Ireland, Italy and Great Britain.

The comet explorer carries ten scientific instruments. Their job is to draw out the secrets of the comet?s chemical and physical composition and reveal its magnetic and electrical properties. Using a specially designed camera, the lander will take pictures in the macro and micro ranges and send all the data thus acquired back to Earth, via Rosetta.

?This will be our first ever chance to be there, at first hand, so to speak, as a comet comes to life,? Schwehm goes on to explain. When Churyumov-Gerasimenko gets to within about 500 million kilometres of the Sun, the frozen gases that envelop it will evaporate and a trail of dust will be blown back over hundreds of thousands of kilometres. When illuminated by the Sun, this characteristic comet tail then becomes visible from Earth. In the course of the mission, the processes at work within the cometary nucleus will be studied and measured more precisely than has ever before been possible, for earlier probes simply flew past their targets.

?As we will be accompanying Churyumov-Gerasimenko for two years, until the comet reaches its closest point to the Sun and travels away from it, we can at long last hope to acquire new knowledge about comets. We are confident we will come a step nearer to understanding the origins and formation of our solar system and the emergence of life on Earth.?

More information on the Rosetta launch can be found on: http://www.esa.int/rosetta

More on ESA Science Programme at: http://www.esa.int/science

Original Source: ESA News Release

Twin Rovers Examining at the Same Time

Image credit: NASA/JPL
Each of NASA’s two Mars Exploration Rovers is using its versatile robotic arm for positioning tools at selected targets on the red planet.

Also, a newly completed 360-degree color panorama from Opportunity shows a trail of bounce marks coming down the inner slope of the small crater where the spacecraft came to rest when it landed on Mars nine days ago.

Opportunity extended its arm early today for the first time since pre-launch testing. “This was a great confirmation for the team,” said Joe Melko of NASA’s Jet Propulsion Laboratory, Pasadena, Calif. Melko is mechanical systems engineer for the arm, which is also called the instrument deployment device.

Mission controllers at JPL are telling Opportunity to use two of the instruments on the arm overnight tonight to examine a patch of soil in front of the rover. A microscope on the arm will reveal structures as thin as a human hair and a Moessbauer Spectrometer will collect information to identify minerals in the soil, according to plans. Tomorrow, the rover will be told to turn the turret at the end of the arm in order to examine the same patch of soil with another instrument, the alpha particle X-ray spectrometer, which reveals the chemical elements in a target.

Spirit is now in good working order after more than a week of computer-memory problems. It is brushing dust off of a rock today with the rock abrasion tool on its robotic arm. After the brushing, Spirit will use the microscope and two spectrometers on the arm to examine the rock.

“We’re moving forward with our science on the rock Adirondack,” said JPL’s Jennifer Trosper, Spirit mission manager. Reformatting of Spirit’s flash memory was postponed from today to tomorrow. The reformatting is a precautionary measure against recurrence of the problem that prevented Spirit from doing much science last week.

Later in the week, Spirit will grind the surface off of a sample area on Adirondack with the rock abrasion tool to inspect the rock’s interior. After observations of Adirondack are completed, the rover will begin rolling again. “We are already strategizing how to drive far and fast,” Trosper said.

Observations by each rover’s panoramic camera help scientists choose where to drive and what to examine with the instruments on each rover’s arm. Dr. Jeff Johnson, a rover science team member from the U.S. Geological Survey’s Astrogeology Team, Flagstaff, Ariz., said that 14 filters available on each rover’s panoramic camera allow the instrument to provide much more information for identifying different types of rocks than can be gleaned from color images such as the new panoramic view.

“By looking at the brightness values in each of these wavelengths, we can start to get an idea of the things we’re interested in, especially to unravel the geological history of these landing sites,” Johnson said.

The main task for both rovers in coming weeks and months is to find clues in rocks and soil about past environmental conditions, particularly about whether the landing areas were ever watery and possibly suitable for sustaining life.

Each martian day, or “sol” lasts about 40 minutes longer than an Earth day. Spirit begins its 31st sol on Mars at 1:23 a.m. Tuesday, Pacific Standard Time. Opportunity begins its 11th sol on Mars at 1:44 p.m. Tuesday, PST. The two rovers are halfway around Mars from each other.

JPL, a division of the California Institute of Technology in Pasadena, manages the Mars Exploration Rover project for NASA’s Office of Space Science, Washington, D.C. Images and additional information about the project are available from JPL at http://marsrovers.jpl.nasa.gov and from Cornell University, Ithaca, N.Y., at http://athena.cornell.edu.

Original Source: NASA/JPL News Release

Spirit is Fully Recovered

Image credit: NASA/JPL
NASA’s Mars Exploration Rover Spirit is healthy again, the result of recovery work by mission engineers since the robot developed computer-memory and communications problems 10 days ago.

“We have confirmed that Spirit is booting up normally. Tomorrow we’ll be doing some preventive maintenance,” Dr. Mark Adler, mission manager at NASA’s Jet Propulsion Laboratory, Pasadena, Calif., said Sunday morning.

Spirit’s twin, Opportunity, which drove off its lander platform early Saturday, will be commanded tonight to reach out with its robot arm early Monday, said JPL’s Matt Wallace, mission manager. Opportunity will examine the soil in front of it over the next few days with a microscope and with a pair of spectrometer instruments for determining what elements and minerals are present.

For Spirit, part of the cure has been deleting thousands of files from the rover’s flash memory — a type of rewritable electronic memory that retains information even when power is off. Many of the deleted files were left over from the seven- month flight from Florida to Mars. Onboard software was having difficulty managing the flash memory, triggering Spirit’s computer to reset itself about once an hour.

Two days after the problem arose, engineers began using a temporary workaround of sending commands every day to put Spirit into an operations mode that avoided use of flash memory. Now, however, the computer is stable even when operating in the normal mode, which uses the flash memory.

“To be safe, we want to reformat the flash and start again with a clean slate,” Adler said. That reformatting is planned for Monday. It will erase everything stored in the flash file system and install a clean version of the flight software.

Today, Spirit is being told to transmit priority data remaining in the flash memory. The information includes data from atmospheric observations made Jan. 16 in coordination with downward-looking observations by the European Space Agency’s Mars Express orbiter. Also today, Spirit will make new observations coordinated with another Mars Express overflight and will run a check of the rover’s miniature thermal emission spectrometer.

Spirit will resume examination of a rock nicknamed Adirondack later this week and possibly move on to a lighter-colored rock by week’s end.

Each martian day, or “sol” lasts about 40 minutes longer than an Earth day. Spirit begins its 30th sol on Mars at 12:44 a.m. Monday, Pacific Standard Time. Opportunity begins its 10th sol on Mars at 1:05 p.m. Monday, PST. The two rovers are halfway around Mars from each other.

The main task for both Spirit and Opportunity in coming weeks and months is to find geological clues about past environmental conditions at their landing sites, particularly about whether the areas were ever watery and possibly suitable for sustaining life.

JPL, a division of the California Institute of Technology in Pasadena, manages the Mars Exploration Rover project for NASA’s Office of Space Science, Washington, D.C. Images and additional information about the project are available from JPL at http://marsrovers.jpl.nasa.gov and from Cornell University, Ithaca, N.Y., at http://athena.cornell.edu.

Original Source: NASA/JPL News Release

Progress Docks with Station

Image credit: NASA
An unmanned Russian resupply ship smoothly linked up to the International Space Station this morning, delivering 2-1/2 tons of food, fuel, spare parts and supplies to the two residents on board.

With Expedition 8 Commander and NASA Science Officer Mike Foale and Flight Engineer Alexander Kaleri looking on, the ISS Progress 13 docked to the aft port of the Zvezda Service Module at 7:13 a.m. CST (1313 GMT) as the two craft flew 230 statute miles above Central Asia.

Foale and Kaleri were in Zvezda, prepared to take over manual control of the operation if it had been necessary, but the Progress craft automatically docked to the module through pre-programmed computer command with no problem.

The Progress was the first ship to arrive at the ISS since Foale and Kaleri were launched more than 100 days ago. They are well past the midway mark of a planned 6-? month mission on the complex. The next ship to reach the Station will be the Soyuz TMA-4 capsule in April, carrying a new crew to replace Foale and Kaleri.

After leak checks are completed to insure a tight seal between Progress and the ISS, Kaleri will open up the ship?s hatch later today so he and Foale can begin unloading its cargo on Sunday. The cargo includes spare parts for environmental systems and a new flex hose to help vent condensation and air from the Destiny Laboratory?s optically pure viewing window. A small leak in an identical flex hose was found to have caused a slight pressure decay in the ISS earlier this month.

Information on the crew’s activities aboard the Space Station, future launch dates, as well as Station sighting opportunities from anywhere on the Earth, is available on the Internet at:

http://spaceflight.nasa.gov/

Details on Station science operations can be found on an Internet site administered by the Payload Operations Center at NASA’s Marshall Space Flight Center in Huntsville, Ala., at:

http://scipoc.msfc.nasa.gov/

Original Source: NASA News Release

Are Galaxy Clusters Corrupting Our View of the Big Bang?

Image credit: RAS
In recent years, astronomers have obtained detailed measurements of the cosmic microwave background radiation – the ‘echo’ from the birth of the Universe during the Big Bang.

These results appear to indicate with remarkable precision that our Universe is dominated by mysterious ‘cold dark matter’ and ‘dark energy’. But now a group of UK astronomers has found evidence that the primordial microwave echoes may have been modified or ‘corrupted’ on their 13 billion year journey to the Earth.

The results from a team at the University of Durham, led by Professor Tom Shanks, are based on a new analysis of data from NASA’s Wilkinson Microwave Anisotropy Probe (WMAP) satellite.

The team has found that nearby galaxy clusters appear to lie in regions of sky where the microwave temperature is lower than average. This behaviour could be accounted for if the hot gas in the galaxy clusters has interacted with the Big Bang photons as they passed by and corrupted the information contained in this echo of the primordial fireball. Russian physicists R. A. Sunyaev and Ya. B. Zeldovich predicted such an effect in the early 1970’s, shortly after the discovery of the cosmic microwave background radiation.

This Sunyaev-Zeldovich effect has previously been seen in the cases of detailed observations of the microwave background in the vicinity of a few rich galaxy clusters and the WMAP team themselves have reported seeing the effect in their own data, close to cluster centres.

Now the Durham team has found evidence that hot gas in the clusters may influence the microwave background maps out to a radius of nearly 1 degree from the galaxy cluster centres, a much larger area than previously detected. This suggests that the positions of “clusters of clusters” or “superclusters” may also coincide with cooler spots in the pattern of microwave background fluctuations.

“The photons in the microwave background radiation are scattered by electrons in nearby clusters,” said Professor Shanks. “This causes important changes to the radiation by the time it reaches us.”

“If the galaxy clusters located several billion light years from Earth also have the same effect, then we must consider whether it is necessary to modify our interpretation of the satellite maps of the microwave background radiation.”

If the Durham result is confirmed, then the consequences for cosmology could be highly significant. The signature for dark energy and dark matter lies in the detailed structure of the ripples detected in the microwave background, tiny temperature variations that were created at a time when the radius of the Universe was a thousand times smaller than it is today.

If this primordial pattern has been corrupted by processes taking place in the recent past, long after galaxies and galaxy clusters formed, then it will, at best, complicate the interpretation of the microwave echo and, at worst, begin to undermine the previous evidence for both dark energy and cold dark matter.

“The power of this wonderful WMAP data is that it indicates that interpreting the microwave background ‘echo’ may be less straightforward than previously thought,” said team member Sir Arnold Wolfendale (previously Astronomer Royal).

The WMAP team has already reported that their measurements of the Big Bang’s microwave echo may have been compromised by the process of galaxy formation at an intermediate stage in the Universe’s history. They presented evidence that gas heated by first-born stars, galaxies and quasars may have also corrupted the microwave signal when the Universe was 10 or 20 times smaller than at the present day. Thus both the WMAP and Durham results suggest that the microwave echo of the Big Bang may have had to come through many more obstacles on its journey to the Earth than had previously been thought, with consequent possible distortion of the primordial signal.

“Our results may ultimately undermine the belief that the Universe is dominated by an elusive cold dark matter particle and the even more enigmatic dark energy,” said Professor Shanks.

Although the observational evidence for the standard model of cosmology remains strong, the model does contain very uncomfortable aspects. These arise first because it is based on two pieces of “undiscovered physics” – cold dark matter and dark energy – neither of which has been detected in the laboratory. Indeed, the introduction of these two new components greatly increases the complication of the standard Big Bang inflationary model.

The problems of dark energy run particularly deep: for example, its observed density is so small that it may be quantum mechanically unstable. It also creates problems for the theories of quantum gravity, which suggest that we may live in a Universe with 10 or 11 dimensions, all of them shrunk, with the exceptions of three in space and one in time.

Many theorists would therefore like an escape route from today’s standard model of cosmology and it remains to be seen how far these observations discussed by the Durham group will go in this direction. But if correct, they suggest that the rumours that we are living in a “New Era of Precision Cosmology” may prove to be premature!

Original Source: RAS News Release

Interview with Michael Benson

Michael Benson, author of Beyond: Visions of the Interplanetary Probes (read Universe Today’s review) took some time from his busy schedule, and nasty cold, to answer some of our questions about his book and interest in astronomy and space exploration. Benson was interviewed by Mark Mortimer.

Universe Today: You say this book is the cumulation of sifting through tens of thousands of image files on computers. What was your selection criteria for the few that made it into the book?

Michael Benson: Well, to start off with, the jaw-drop factor, of course. Stuff that was incredible, I tried my best to get in. After that, though, of course you have the inevitable limitations of the book medium, with its fixed number of pages, plus then I had to divide the solar system up into chapters and try to give each one at least its due if not more, pretty soon I realized I had to winnow the available images down to not as many as I would have liked. And then there was the color versus B&W question — I wanted to get in as many good color shots as I could, though I have a real weakness for black and white photography. Essentially, though, whatever really made me gaze in amazement got in. I have to say, though, that I have a lot of really first-rate processed pictures on my hard drive that I’d love to use elsewhere sometime. Some of it has never been seen before, except for by a small cadre of planetary scientists, and then usually in black and white.

UT: As an artist did you feel like an outsider when discussing these images or did you feel like a member of the group of technicians?

MB: Neither. I always approached them as an aesthetic challenge — how to get them to “pop” — to reveal that they weren’t shot through a digitized grid but through optically pure glass, as it were. And much of the work behind getting them to the right place was technical — using photoshop or other programs — but this is also the tool of a photographer, or ‘artist’ if you will. And even when working with Dr. Paul Geissler, who is an eminent planetary scientist and remote imaging expert, I didn’t feel like an outsider — we had a good collaboration — nor like I belonged to some group of techies either. (I don’t think he feels like the latter either, come to think of it, though he recently took a job at the US Geological Survey — which makes highly accurate maps of all the planets based on space imaging! Which is about as technical as it gets.)

UT: How would you compare the artistic qualities and values of colour to black and white in this medium?

MB: I like both for different reasons. It also depends on the planetary body being represented, to an extent. Black and white pictures of Jupiter’s implacably volcanic, sulphurously yellow-orange moon Io, for example, practically don’t make any sense in a book of this type. They make perfect sense when it comes to conducting science, but would’ve been a bit hard to justify having them in my book, given that Io is by far the most lurid object in the Solar System. And by the same token Europa, Io’s closest neighboring moon, which is a spherical iceberg of fissured, chaotic ice, doesn’t really need to be in color — though it also looks awesome in color. But you get the essence of its story in black and white, if I can put it that way. (Though part of that essence is in fact its mystery — what’s going on under that global ice-cap?)

UT: Do you have a favourite/most photogenic planet? For example Venus seems to be heavily weighed in the book.

MB: Actually, Venus gets fewer pages than either Mars or Jupiter. Jupiter may be the most complex and compelling, though Saturn is a close second, because of its perfect rings. Saturn could scarcely be _more_ photogenic — we’re very lucky to have it in the solar system, because it shows what cosmic perfection really is. And as for Jupiter, as I said in my book, it’s a solar system in miniature — it’s endlessly fascinating and kinetic. The last quality is hard to show with stills, but not impossible.

UT: How were you able to convince a publisher to go for a book of images freely available on the web?

MB: Many of the images were available in raw form at specialized planetary science sites, not “freely available,” in the sense that they required substantial processing and mosacking, rendering into color or what have you. Plus even the images that are more readily available — for example, at NASA’s outreach site A Planetary Photojournal — still required substantial processing, most of them, to get them to work at the resolution quality we have available on the page, as opposed to the screen, where lower resolutions still work.

But the premise of the question is a bit flawed. Publishers are delighted if they can base a book on public domain images, because then they don’t have to pay for it!

UT: Considering the forward, do you think a living carbon based life form will explore our solar system? Other star systems? Do you think humans will do this?

MB: I do. We suffer a bit of temporal tunnel vision as a species. Even if we don’t do it for a hundred or two hundred years in the case of the solar system — and much later for the stars — I still think we’ll do it. Our current hesitation about it has to do with the sluggish pace of crewed exploration after Apollo and also the sense that the environments are so hostile that it might not be desirable to do it. But technology will march onwards and make these such things easier. And then, as soon as it is possible for tourists to actually go to, for example, Jupiter, there will be a huge rush to go there. Or Mars, of course. Or the Moon…

UT: Considering the afterward, where do you think people fit into the universal schema of things?

MB: Oh, I tend to agree with Ren — Lawrence Weschler — that for now at least we seem to be the only creatures that can experience that sense of awe that is ultimately one of the roots of our sentience. My discussion with him had to do with whether machines could ever experience this. I believe one day they will, he’s not so sure. Wasn’t it Asimov who, when asked if he really believed machines would one day think, said “well, I’m a machine, and I think”?

But in the end I think Ren’s daughter Sara is right in saying that the universe in a sense needs us, because we are capable of appreciating its beauty. Another way of putting it, I suppose, is that we are one of the ways in which the universe can appreciate its own splendor. And of course we are pieces of work ourselves, just to coin a phrase!

UT: No 3D images are in the book though we are presently getting some from Mars. What is your opinion of the artistic value of 3D images for this subject and media?

MB: Well, as someone who has barely pried my 3-D glasses of my nose for the last couple weeks, as I peer in fascination at the images from the Spirit and Opportunity rovers, I don’t know how objective I can be on the question. I really like it — though more for that “you are there” sensation than for aesthetic reasons I suppose. But there is no reason why 3-D images can’t be savored for their aesthetic qualities as well. I’ll be able to answer with more conviction on the question after this whole rover experiment is over, because there will really be many thousands of 3-D pictures to go through by then, and no doubt some of them will work on the multiple levels required to be considered art. So the jury — not that I consider myself a jury — is out on the question, but not for too long. Personally, I’d love to see a purple-orange cactus appear on the lip of a crater one of these days — though the artistic qualities of the shot will be the last thing on anyone’s mind if that happens!

Hubble Sees Atmosphere Blowing Off a Planet

Image credit: ESA
The well-known extrasolar planet HD 209458b, provisionally nicknamed Osiris, has surprised astronomers again. Oxygen and carbon have been found in its atmosphere, evaporating at such an immense rate that the existence of a new class of extrasolar planets ? ?the chthonian planets? or ?dead? cores of completely evaporated gas giants – has been proposed.

Oxygen and carbon have been detected in the atmosphere of a planet beyond our Solar System for the first time. Scientists using the NASA/ESA Hubble Space Telescope have observed the famous extrasolar planet HD 209458b passing in front of its parent star, and found oxygen and carbon surrounding the planet in an extended ellipsoidal envelope – the shape of a rugby-ball. These atoms are swept up from the lower atmosphere with the flow of the escaping atmospheric atomic hydrogen, like dust in a supersonic whirlwind.

The team led by Alfred Vidal-Madjar (Institut d?Astrophysique de Paris, CNRS, France) reports this discovery in a forthcoming issue of Astrophysical Journal Letters.

The planet, called HD 209458b, may sound familiar. It is already an extrasolar planet with an astounding list of firsts: the first extrasolar planet discovered transiting its sun, the first with an atmosphere, the first observed to have an evaporating hydrogen atmosphere (in 2003 by the same team of scientists) and now the first to have an atmosphere containing oxygen and carbon. Furthermore the ?blow-off? effect observed by the team during their October and November 2003 observations with Hubble had never been seen before.

In honour of such a distinguished catalogue this extraordinary extrasolar planet has provisionally been dubbed ?Osiris?. Osiris is the Egyptian god who lost part of his body ? like HD 209458b – after his brother killed and cut him into pieces to prevent his return to life.

Oxygen is one of the possible indicators of life that is often looked for in experiments searching for extraterrestrial life (such as those onboard the Viking probes and the Spirit and Opportunity rovers), but according to Vidal-Madjar: ?Naturally this sounds exciting – the possibility of life on Osiris – but it is not a big surprise as oxygen is also present in the giant planets of our Solar System, like Jupiter and Saturn?.

What, on the other hand was surprising was to find the carbon and oxygen atoms surrounding the planet in an extended envelope. Although carbon and oxygen have been observed on Jupiter and Saturn, it is always in combined form as methane and water deep in the atmosphere. In HD 209458b the chemicals are broken down into the basic elements. But on Jupiter or Saturn, even as elements, they would still remain invisible low in the atmosphere. The fact that they are visible in the upper atmosphere of HD 209458b confirms that atmospheric ?blow off? is occurring.

The scorched Osiris orbits ?only? 7 million kilometres from its yellow Sun-like star and its surface is heated to about 1,000 degrees Celsius.

Whereas hydrogen is a very light element – the lightest in fact – oxygen and carbon are much heavier in comparison. This has enabled scientists to conclude that this phenomenon is more efficient than simple evaporation. The gas is essentially ripped away at a speed of more than 35,000 km/hour. ?We speculate that even heavier elements such as iron are blown off at this stage as well? says team member Alain Lecavelier des Etangs (Institut d’Astrophysique de Paris, CNRS, France).

The whole evaporation mechanism is so distinctive that there is reason to propose the existence of a new class of extrasolar planets – the chthonian planets, a reference to the Greek God Kht?n, used for Greek deities from the hot infernal underworld (also used in the French word autochton). The chthonian planets are thought to be the solid remnant cores of ?evaporated gas giants?, orbiting even closer to their parent star than Osiris. The detection of these planets should soon be within reach of current telescopes both on the ground and in space.

The discovery of the fierce evaporation process is, according to the scientists, ?highly unusual?, but may indirectly confirm theories of our own Earth?s childhood. ?This is a unique case in which such a hydrodynamic escape is directly observed. It has been speculated that Venus, Earth and Mars may have lost their entire original atmospheres during the early part of their lives. Their present atmospheres have their origins in asteroid and cometary impacts and outgassing from the planet interiors?, says Vidal-Madjar.

Original Source: ESA News Release

James Cameron’s Plans for Mars

Image credit: James Cameron
As an artist and filmmaker, James Cameron is credited on major Hollywood productions in virtually all roles: writer, director, producer, editor, visual effects, actor, art director, and even crew. Cameron wrote and directed such science fiction classics as “Terminator 2: Judgement Day” (1991), “The Abyss” (1989), and “Aliens” (1986). He received an Academy Award for Best Director for 1997’s “Titanic,” which was also the largest grossing film in history.

Astrobiology Magazine’s Executive Producer, Helen Matsos, sat down with James Cameron and discussed his project slate. During their discussions, Cameron shared how he became interested in Mars and his unique renderings commissioned to represent the key stages in a future human mission to the red planet. As Cameron said about his directorial view: “I think that any kind of exploration should always try to acquire the highest level of imaging. That’s how you engage people — you can put them there, give them the sense that they’re standing there on the surface of Mars.”

The Design Reference Mission (DRM) covers Earth launch to Mars landing, Mars cruise to Mars launch, and Earth return. The mission entails sending cargo ahead, docking the crew at the space station, then meeting up with the cargo supplies once on Mars.

Cameron underscored the need to illustrate the details for each stage of the DRM. And whether deploying a crew or robotic explorers, the mission needed to connect more to a shared human story of discovery. A future Astrobiology Magazine feature will highlight Cameron’s reflections on making such a mission come to life, but this director’s preview offers tantalizing visual cues to what is going on robotically today on Mars.

“The [1997] Sojourner Rover became a character to millions of people, a protagonist in a story. How long is it going to survive, could it perform its mission? It wasn’t anthropomorphic in any way, there was absolutely no emotion in a little solar powered machine that was being commanded from eighty million miles away, and yet people thought of it as a character. The reason we thought of it as a character is that it represented us in a way. It was our consciousness moving that vehicle around on the surface of Mars. It’s our collective consciousness — focused down to that little machine – that put it there. So it was a celebration of who and what we are.”

“It takes our entire collective consciousness and projects it there – to that point in time and space. That’s what the Sojourner Rover did.”

“I was involved in a private company that was going to try to land two rovers on the Moon. That collapsed in the dot com crash – they ran out of money. I’m loosely involved with people who are going to be doing future robotic missions to Mars. I’m involved in terms of imaging, and of how imaging might be improved in terms of story telling. I’ve been very interested in the Humans to Mars movement –the ‘Mars Underground’ — and I’ve done a tremendous amount of personal research for a novel, a miniseries, and a 3-D film.”

“In doing this fictional story about the first humans to Mars — a subject that has been done in the movies, but never done very well, I think — people in the Hollywood community have no idea of what that means. The average person walking around has no idea of what’s involved. I called up NASA and said ‘who’s in charge of Mars?’ It turns out that NASA has (scientists studying Mars) everywhere, but there’s no one person in charge. It’s taken me years to ferret around and talk to everybody.”

In the course of designing this project, we never got past the design stage, although we will eventually. Right now it’s just, ‘what’s everything going to look like?’ What it looked like was determined by how it worked, and how it worked was determined by the mission architecture. ”

“The thing I found about human mission architectures for going to Mars is that if you change one piece or one assumption, it has a ripple effect through the whole thing, and it looks different coming out the other end. You do things differently, your spacecraft are configured differently, your surface mission looks different, the time you spend on the planet looks different. So a certain set of fundamental assumptions had to be made and then we had to design everything for what it was going to look like.”

“I wanted it to be highly realistic. Obviously I don’t think we can predict now, twenty-some years before the fact, exactly how it is going to be done, but we can make a set of very plausible assumptions. We got involved in the design of it, and predicated it on a series of assumptions, and then I went to JSC (Johnson Space Center) to talk to some of the people in the human exploration and development group. I asked, ‘Does this look like what you guys thought?’ They had created overall architectural guidelines in the DRM – the Design Reference Mission – but there were no pictures. Nobody knew what it was really going to look like.”

I said, ‘Look, this is our proposal for what a Hab would look like, and what a pressurized rover would look like, and we made certain assumptions based on how we operate deep submersibles, for example, in terms of how the manipulators would work taking samples and so on.’ And they said, ‘Hey, this is neat! Thanks! If you ever want to get out of filmmaking, come here and hang with us.’

The stages of the Cameron’s Mars Reference Design take a crew and cargo ship from a heavy-lift launch to the flat, red plains of Mars. See the slideshow version.

A Biconic Aeroshell and Fairing is used to transport payloads into space atop a heavy launch vehicle. A single cargo mission will preceed the crew to Mars. The cargo mission provides all the necessary equipment a Mars crew will require to explore the Martian surface for 500 to 600 days.

Included in this cargo are the Cargo Landing Vehicle (CLV), an In Situ Propellant Production Plant Reactor and two inflatable surface Habitats (Hab). This cargo will be placed in the Biconin Aeroshell and will Aerobraking to slow its descent into the martian atmosphere. A heavy-lift launch vehicle will deliver the Crew Transfer Vehicle (CTV) into low Earth orbit (LEO). The CTV will deploy in orbit and rendezvous with the crew at the International Space Station (ISS).

The CTV comprises several systems:an inflatable habitat called the TransHab; the Crew Lander and Rover; and the Aeroshell. The petals of the Aeroshell deploy and lock in place. After cruise, the CTV will tumble end-over-end during Trans-Mars Injection (TMI), creating a 0.38 times earth gravity environment, identical to conditions on Mars. The Crew Lander and Rover, along with their aeroshell will separate from the CTV and enter into the martian atmosphere.

Upon successful aerobraking in the Mars’ atmosphere, the Biconic aeroshell will fall away as large parachutes further assist to slow the CLV in its powered landing. The crew will use steering flaps and reaction control thrusters to guide their entry. During descent, the packed Habs are jettisoned.

The jettisoned Habs will inflate during its independent descent, providing airbag protection to the Cargo Modules housed inside. The aeroshell itself is jettisoned and large parachutes are used to slow the Crew Lander and Rover during descent.

The Crew Lander and Rover will use powerful engines to hover before landing. The Rover’s variable suspension will be capable of absorbing the shock of landing as well as increasing the Rover’s ground clearance. In addition to the Rover’s descent engines, the vehicle will serve as transport and mobile laboratory. A robotic manipulator and crane will allow the crew to interact remotely with the surface. Forward and dorsal docking tunnels simplify crew transfers to the Hab. Power will come from crygenic fuel tanks and a photovoltaic array. The vehicle’s port side includes a centrifugal blower to keep dust to a minimum.

On the surface, the crew must locate both Habs and transport them to the CLV site. The Crew Lander/Rover docks with one of the Habs via the forward hatch. The Mars Mission Base will have a modular design of components that allow for several geometric configurations and expansion.

After landing, the In Situ Propellant Production (ISPP) plant deploys nuclear reactors to power the production of water, oxygen and methane using hydrogen and carbon dioxide as raw materials.

The CLV and ISPP will provide liquid oxygen and methane (LOX/CH4) propellant to the Ascent Crew vehicle. The Ascent Crew vehicle will rendezvous with the Earth Return Vehicle in orbit around Mars.

Original Source: Astrobiology Magazine