Posted on by Fraser Cain

Mars Society Responds to Bush Announcement

Image credit: NASA
On January 14, President George Bush gave a speech at NASA headquarters outlining a new strategic orientation for the American space agency. While some of the initial ideas for implementing the new space policy can and should be substantially improved upon, the policy overall clearly represents a significant and long-overdue step in the right direction for the American space program. The Steering Committee of the Mars Society therefore welcomes the new policy as presented in Presidential Directive entitled ?A Renewed Spirit of Discovery,? and strongly urges Congress to provide the funds requested for the initial steps requested for the program over the next fiscal year.

Our analysis of the important strengths and required areas for improvement of the new policy is presented below.

Analysis
As stated, the new Bush space policy offers both opportunities and pitfalls to those interested in furthering human exploration and expansion into space in general, and Mars in particular. While not representing the start of an actual Moon/Mars program, since nearly all serious spending for hardware systems other than the crew capsule is deferred to administrations coming into office in 2009 or beyond, it does in fact clear the ground for the initiation of such a program should the 2009 administration be so inclined. It also provides a certain amount of free energy that, if handled properly in the 2004-2008 period, could be used to help insure the emergence of a powerful human exploration initiative within the time frame of the 2009 administration.

In his speech, Bush redefined the purpose of the American space program as the ?establishment of a human presence throughout the solar system.? This statement may seem to some like a mere rhetorical flourish, but it actually has important concrete programmatic significance, as it legitimizes NASA spending supporting technology development for human exploration of the Moon and Mars. Such spending was forbidden under the previous order of things, and for the past ten years technologists seeking funding for important human Moon/Mars exploration technologies had to justify them by arguing their value for other established programs, such as the JPL-led robotic exploration program or the ISS. This has made it impossible to obtain adequate funding for many technologies, such as planetary in-situ resource utilization (ISRU), and has led to disasters such as the promising JSC-led Transhab inflatable habitation program, which was derailed when the discovery that planetary exploration technology work was being done under ISS cover led to cancellation by congressional staff. It is for this reason that the Mars Society has had since its Founding Convention in 1998 campaigned for the establishment of a NASA line item for the support of human exploration technology development, so that such activity could take place openly. Bush?s initiative fully accomplishes this objective, with healthy initial program funding. For this reason, if no other, Bush?s move must be seen as an extremely positive development.

The new policy will also create a program organization at NASA headquarters, called Code T, which will significantly raise the level of NASA efforts to develop efficient plans for human planetary exploration. This is also a welcome development.

In addition, the Bush policy also provides a basis for including human exploration research requirements within the design of robotic planetary missions. In the late nineties, representatives of the human exploration missions office at JSC attempted to utilize flight opportunities aboard the JPL-led robotic Mars exploration landers, but as the JSC researchers had neither a mandate nor money, they had neither force nor funds to back up their requests, and were dealt with accordingly. Under the new space policy, both a mandate and funds should be available to support human exploration related research and technology flight experiments aboard robotic lunar and planetary spacecraft. This could allow such payloads to either fly as paying customers aboard the JPL/Code S sponsored science spacecraft, or alternatively, support the funding of human exploration program-controlled robotic landers whose primary mission would be to provide engineering data for the human exploration program, with other science payloads carried on a space-available basis.

The Bush policy also identifies where the funds required to support a true human exploration initiative will come from, to wit the redirection of the existing Space Shuttle and ISS budgets. Currently, the Shuttle budget runs about $4 billion per year, while the ISS budget is between one and two billion. This total of $5-$6 billion per year is more than sufficient to get humans to both the Moon and Mars within ten years of actual program start. Thus the initiative can be done within the existing NASA budget of about $16 billion per year in 2004 dollars, a level found supportable by presidents and congressional majorities of both political parties for the past four presidential terms. Thus the financial basis for the program is clear, and is not a budget buster or in any way fantastical.

In his speech, the President invited all nations to join with the United States in pursuing the proposed program. We welcome this statement, as we fully agree that the exploration and settlement of the solar system is a great goal that can help bring humanity together, one that is worthy of, and requires, the mobilization of the best talents of all the peoples of the Earth.

For various political and diplomatic reasons, the Bush policy delays the phase out of the Shuttle and ISS until 2010, thereby delaying substantial human exploration program start until about that time. Thus the choice on whether or not to really start a Moon or Mars human exploration program, and what its pace or objectives should be, is effectively being placed in the hands of the 2009 administration.

The merit of this decision is debatable. A key point however, is that the 2009 administration will have a choice. By making clear that the fundamental purpose of the human spaceflight program is to allow humans to FLY ACROSS SPACE (the Apollo era vision) to explore other worlds, rather than to allow humans to EXPERIENCE SPACE (the Shuttle era vision), the Bush policy (should it be sustained by either his reelection or the concurrence on this issue of an alternative 2005 administration) effectively precludes the commitment of NASA to a second generation Shuttle (?Shuttle 2?) as its next major program. As recently as a few months ago, substantial factions within space policy circles in both congress and NASA projected such a Shuttle 2 program as the agency?s next major project after ISS. Had that occurred the future would have looked like this: the present decade would be consumed with returning the Shuttle to flight and building ISS. The next decade would be devoted to extending the life of Shuttle and developing Shuttle 2. The 2020?s would then be a repeat of the 1980?s, attempting to make Shuttle 2 operational, leading to a decision in 2030 on the next major project, which probably would have been ISS-2. Thankfully, this ?Groundhog Day? scenario for perpetual stagnation in space has now been foreclosed on.

The decision to punt the responsibility for implementation, and thus the control, of the program to the 2009 administration promises to make the next five years an extremely interesting time for space advocates. In his speech, Mr. Bush defined human expansion into the solar system as NASA?s goal, and posed the idea of a lunar base initiated by 2020 as the strategy by which this objective might be approached. That is one plan, but the next five years will see other plans put forward for consideration by the political class as efficient means by which the desired overall goal can be achieved with maximum speed, reliability, and at minimum cost. The great debate on what our strategy for reaching the Moon and the planets should be has thus not been closed by Bush?s speech, but opened.

The victory in this healthy battle of ideas will go to those people who convince the players, not merely of today, but of 2009 and beyond, of the merit of their concepts. The Mars Society welcomes this challenge, and will seek to actively participate in this discussion to contribute its technical expertise and to convey an understanding to the political class, the technical community, the press, and the public that within the context of the new space policy, that the near-term human exploration of Mars is feasible, affordable, and truly worthy of the efforts and risks required.

In transitioning from one kind of space program to another, every effort should be made to prevent unnecessary collateral damage to valuable parts of the old program. The decision announced by NASA headquarters late last week to abandon the planned Shuttle mission to upgrade and reboost the Hubble Space Telescope (HST) is an example of the kind of mistake that needs to be avoided. The Cosmic Origins Spectrograph and Widefield Camera 3 designed to bring the HST to its full potential have already been built and tested, and promise an enormous scientific return upon delivery to orbit. If the Bush plan were to stand down the Shuttle immediately, and save the $24 billion required to operate it through 2010 so as to initiate the Moon/Mars program with substantial funding immediately, that would be one thing. But given the decision to return the Shuttle to flight, canceling the Hubble upgrade would only save about $200 million, or 1% of the Shuttle program?s budget, while destroying about 90% of its scientific value. This is extremely foolish.

Safety arguments won?t wash either; if the Shuttle is safe enough to fly to the ISS, its safe enough to perform its mission to Hubble. Indeed, while Shuttle missions to the Hubble may lack the on-orbit safe-haven of the ISS, the low-inclination of Hubble flights enables launch aborts to warm tropical waters, where crew survival chances are much better than in the frigid north Atlantic abort sites required by ISS launches. Moreover, it is difficult to understand how an agency which is too risk adverse to undertake a Shuttle mission to Hubble could possibly be serious in considering a mission to the Moon or Mars.

The cancellation of the Hubble mission can thus only be described as a serious mistake, apparently committed in the name of the desire to appear ?decisive? in breaking from the old paradigm in favor of the new. In addition to the harm done to astronomy, it would be a very bad thing for the infant new space policy to begin its life with a such a distasteful record. Under no circumstances should the alleged impending availability of the James Webb Space Telescope be accepted as a rationale for abandoning Hubble, either. That would be to repeat the mistake NASA made in abandoning the Saturn V for the supposedly superior Shuttle, or Skylab for the ISS ? errors which set back the space program by decades of time of tens of billions of dollars. If NASA?s leadership will not see reason on this issue, Congress should take forceful action to reverse this very bad decision.

Technological Issues
The right way to do a program whose objectives encompass both a permanent lunar base and the human exploration of Mars is to design a set of transportation hardware that can accomplish human Mars missions, a modified modular subset of which can be used to support lunar activities. Approaching the problem in this way can save a great deal of time and money, as only one hardware set needs to be developed instead of two. It also maximizes the value of the Moon as a testing ground for Mars, since under this approach to Moon missions will be done using the Mars hardware, and serve directly to shake it out. Provided this is the approach adopted, a program initiated in 2009 could easily achieve piloted lunar landing by 2015 and launch the first human Mars expedition by 2018. The build up of a permanent lunar base and continued Mars missions could then occur simultaneously. Since it is only possible to launch to Mars every other year in any case, the implications of a running concurrent programs are simply that the lunar program launch rate would be reduced somewhat during Mars launch years. Concurrent launch programs would also serve to minimize launch costs by maximizing the rate of production of the booster production lines, as the cost of running a launch vehicle manufacturing facility increases only marginally with a higher production rate. To use a mundane analogy, it takes very little extra labor to cook two steaks instead of one, provided you cook them both at the same time. In the production of launch vehicles this kitchen parable holds even more force, as labor costs overwhelmingly dominate those of materials.

Within the context of such a well-planned Moon/Mars program, there are certain technologies that are essential. We address only two of the most critical, heavy lift boosters and ISRU.

Heavy Lift Boosters
The key technical instrumentality required to make lunar bases and Mars missions feasible is a heavy lift vehicle with a hydrogen/oxygen upper stage capable of throwing payloads in the 50-tonne class on Trans-lunar or Trans-Mars injection. This is the capability demonstrated during the 1960?s by the Saturn V. Once such a vehicle is available, roundtrip Lunar missions or one-way delivery of habitations and other heavy payloads to the lunar surface can be readily accomplished with a single launch. Piloted Mars missions can also be accomplished using multiple discrete Trans-Mars launches of such a system, with no on-orbit assembly, as shown by the Mars Direct plan (Zubrin and Baker, 1990), the Stanford Mission plan (Lusignan, et al 1992), or the JSC Design Reference Mission 3 (Weaver et al, 1994).

Such Saturn V class launch systems can be readily created at this point either by converting the Shuttle launch stack through elimination of the orbiter and its replacement with a LOx/H2 upper stage, or the creation of new, all-liquid propulsion booster systems. The Mars Society was recently shown plans by one major aerospace company for evolving its existing line of medium lift boosters to create a family of modular heavy lift boosters with payloads ranging through quarter, half, and full Saturn V capabilities. Based on this company?s experience with previous successful launch vehicle developments, the entire development program to create the whole family of boosters could be accomplished in five years with a development cost of about $4 billion. The recurring launch cost for the Saturn V class system design was $300 million per launch, or less than $1000/lb for payload delivery to LEO. The methods of creating such booster families are obvious to experienced launch vehicle engineers, and we have no doubt that this company?s competitors have plans for creating similar hardware sets with comparable development costs and schedules.

The claims by certain pundits opposed to any exploration initiative that a new heavy lift booster would cost tens of billions to develop can thus readily be shown to have no basis in fact. Such heavy lift vehicles would also have many applications outside of the human exploration program.

ISRU
Both lunar bases and Mars expeditions are strongly benefited through the use of in-situ resource utilization (ISRU) techniques for the production of return propellant, human consumables, and vehicle fuels and oxygen for use in extended missions on a planetary surface. The mission mass savings for either lunar bases or Mars missions resulting from ISRU has been demonstrated in numerous studies, and significantly exceeds that offered by advanced propulsion concepts with much higher development and recurring system costs.

Effective ISRU require both chemical processing systems and reliable sources of power, for which space nuclear systems offer the greatest promise. We therefore strongly commend the administration for its Prometheus project to create such space nuclear systems. However we note that up until now, the sole applications considered by NASA for its space nuclear power systems have been spacecraft power and nuclear electric propulsion (NEP). Without dismissing the important value of NEP for outer solar system robotic missions and other missions involving large velocity changes undertaken across extended time frames, we note that the size of NEP units required to supply propulsion for human exploration missions are on the order of 10,000 kilowatts. In contrast, when used to produce chemical propellants on planetary surfaces, the required reactor size to support human exploration is reduced to about 100 kilowatts. This is because a much smaller reactor stationed on a planetary surface making propellant can emit energy over a long period of time prior to flight, store it as chemical propellant, which then can release the energy as fast as it is needed under flight conditions. The mission mass leverages achieved by such ISRU supported chemical propulsion options are greater than those offered by NEP, while for inner solar system missions, the flight times are less (two orders of magnitude less for Lunar applications). In addition, the ISRU-supported chemical systems can be used not only for orbital transfer, but for planetary ascent.

Thus while space nuclear power is enabling for ISRU, it is ISRU that greatly reduces the cost, and increases the value of space nuclear power in supporting human exploration. The two technologies should thus be pursued in parallel, and an appropriate fraction of the Prometheus budget applied towards bringing ISRU applications of space nuclear power to flight status, and to support robotic missions demonstrating such technology on the Moon and Mars.

Furthermore, requirements should be written into the Prometheus program to insure that the power systems developed are compatible for operation on the surface of the Moon and Mars, since their use on the planetary surface to produce propellants and consumables represents by far the most advantageous method of employing them to support near-term human space exploration, and their power is needed on the surface to support base operations in any case.

Both ISRU technology and heavy lift booster development should thus be central priorities of the Code T effort over the immediate period.

Other systems should be developed with similar concern for maximum commonality of hardware and technology across lunar and Mars mission applications.

Political Implications
The train of events set in motion by the new space policy will create a decision point circa 2009 that will offer three alternatives for future action. These are;

1. The 2009 administration could choose to abort the Moon/Mars program altogether, and simply use the Crew Exploration Vehicle (CEV) as a capsule launched atop expendables as a way of continuing to visit the ISS. This would lead to a Mir-type extended ISS program, conducted at lower cost than possible using Shuttle launches, but with no discernable purpose. This would result in stagnation in space for however long such a programmatic decision prevailed, and probable retrogression on heavy lift, ISRU, and other programs necessary for human exploration.

2. The 2009 administration could decide to proceed in accordance with idea of building a lunar base, starting 2020, without concern for the Mars mission except to make claims that lunar experience will no doubt be useful later when others contemplate going to Mars. This would result in the development of mostly incompatible lunar program hardware (except the booster), making it necessary to start developing an entire new hardware set circa 2030, or possibly 2040, given the budgetary entanglements such a stand-alone lunar program would create, making it likely that the first Mars landing would not occur before the middle of the 21st Century. Alternatively, given the limited interest provided by repeated dead-end Lunar expeditions, the program could simply expire.

3. The 2009 administration could decide to launch a humans to Mars program, with the objective of reaching Mars within ten years, with expeditions to the Moon using a modified subset of the Mars flight hardware beginning around program year 7. Because only one hardware set would need to be developed instead of two, and because in aerospace cost equals people times time, this represents a much lower cost approach to achieving the goals set forth in the new space policy than alternative (b). Moreover, it is the only approach that will result in human explorers walking on Mars within the working lifetime of any adult today.

It is therefore imperative that everyone who wishes to see the human exploration of Mars become a reality do everything he or she can to fight for the bold course represented by option C. In the labs and engineering organizations, in the press, in the classroom and the committee room, in the Arctic and in the desert, in the halls of congress, and in every venue of public opinion ranging from books and technical papers to internet newsgroups and late night talk radio, each will need to play their part.

A door has been opened, and a battle of ideas that will determine the shape of the human future for many years to come has now been truly joined. Where it will lead is up to us. Contending visions that two weeks ago were mere hypothetical debates among space activists have now entered the center of political discourse. We welcome the challenge. For as reason is our witness and courage is our guide, we shall prevail.

Original Source: Mars Society News Release

Posted on by Fraser Cain

Opportunity’s Hardware is Working Properly

Image credit: NASA/JPL
During the second day on Mars for NASA’s Opportunity rover, key science instruments passed health tests and the rover made important steps in communicating directly with Earth.

Halfway around the planet, during its 22nd day on Mars, NASA’s Spirit obeyed commands for transmitting information that is helping engineers set a strategy for fixing problems with the rover’s computer memory.

On Earth this morning, scientists marveled at a high-resolution color “postcard” of Opportunity’s surroundings. The mosaic of 24 frames from the panoramic camera shows details from the edge of the lander to the distant horizon beyond the rim of the rover’s small home crater.

“We’re looking out across a pretty spectacular landscape,” said Dr. Jim Bell of Cornell University, Ithaca, N.Y., lead scientist for the panoramic cameras on Spirit and Opportunity. “It’s going to be a wonderful area for geologists to explore with the rover.”

The color view shows dark soil that brightened where it was compacted by the rolling spacecraft, and an outcropping of bedrock on the inside slope of the 20-meter (66-foot) crater in which the rover sits. Opportunity will be commanded to finish taking a 360- degree color panorama of the site during its third Mars day, which began at 12:01 p.m. PST today.

Another major step planned for Opportunity’s third day is to begin using its high-gain antenna for communicating directly with Earth at a high data rate, said Jackie Lyra of NASA’s Jet Propulsion Laboratory, Pasadena, Calif., activity lead for this rover event. In preparation for this transition, Opportunity found the Sun with its panoramic camera yesterday. Once oriented by knowing the position of the Sun, it can calculate how to point its high-gain antenna toward Earth.

“We’re making steady progress in our effort to get the wheels of the rover dirty,” said Mission Manager Jim Erickson of JPL. Still the earliest scenario for the rover to drive off its lander platform is more than a week away.

Opportunity has tested the three scientific sensing instruments on its robotic arm that will be used for up-close examination of rocks and soil: the microscopic imager, the alpha particle X-ray spectrometer for determining what elements are present, and a Moessbauer spectrometer for identifying iron-containing minerals. “I’m pleased to report that all are in perfect health,” said Dr. Steve Squyres of Cornell University, Ithaca, N.Y., principal investigator for the science instruments on the rovers.

Squyres had been especially concerned about the Moessbauer spectrometer because tests conducted while the spacecraft was on its way to Mars showed that an internal calibration system was not working as intended. However, after the rover landed on Mars, the instrument is functioning normally again. The Moessbauer spectrometer’s function for identifying iron-bearing minerals will be important in the scientific goal of determining the origin of iron-bearing hematite deposits in the Meridiani Planum region selected as Opportunity’s landing site.

“We have a perfectly functioning Moessbauer spectrometer, and given that we are now perched atop the hematite capital of the Solar System, that’s a good thing,” Squyres said.

Restoration efforts continue making progress on Spirit. “We have a patient in rehab, and we’re nursing her back to health,” said JPL’s Jennifer Trosper, mission manager.

Engineers found a way to stop Spirit’s computer from resetting itself about once an hour by putting the spacecraft into a mode that avoids use of flash memory. Flash memory is a type common in many electronic products, such as digital cameras, for storing information even when the power is off. The rover also has random- access memory, which cannot hold information during the rover’s overnight sleep. One of the next steps planned is to erase from flash memory the files stored there from the spacecraft’s cruise to Mars from Earth. That is intended to lessen the task of managing the flash memory files.

The rovers’ main task is to explore their landing sites during coming months for evidence in the rocks and soil about whether the sites’ past environments 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

Posted on by Fraser Cain

Rosetta Will Launch in a Month

Image credit: ESA
Rosetta is scheduled to be launched on board an Ariane-5 rocket on 26 February from Kourou, French Guiana.

Originally timed to begin about a year ago, Rosetta’s journey had to be postponed, as a precaution, following the failure of a different version of Ariane-5 in December 2002. This will be the first mission to orbit and land on a comet, one of the icy bodies that travel throughout the Solar System and develop a characteristic tail when they approach the Sun.

This delay meant that the original mission’s target, Comet Wirtanen, could no longer be reached. Instead, a new target has been selected, Comet 67P/Churyumov-Gerasimenko, which Rosetta will encounter in 2014 after a ?billiard ball? journey through the Solar System lasting more than ten years. Rosetta?s name comes from the famous ?Rosetta Stone?, from which Egyptian hieroglyphics were deciphered almost 200 years ago. In a similar way, scientists hope that the Rosetta spacecraft will unlock the mysteries of the Solar System.

Comets are very interesting objects for scientists, since their composition reflects how the Solar System was when it was very young and still ‘unfinished’, more than 4600 million years ago. Comets have not changed much since then. In orbiting Comet Churyumov-Gerasimenko and landing on it, Rosetta will collect information essential to an understanding of the origin and evolution of our Solar System. It will also help discover whether comets contributed to the beginnings of life on Earth. In fact comets are carriers of complex organic molecules that, delivered to Earth through impacts, perhaps played a role in the origin of living forms. Furthermore, ?volatile? light elements carried by comets might also have played an important role in forming the Earth?s oceans and atmosphere.

?Rosetta is one of the most challenging missions undertaken so far,? says Professor David Southwood, ESA Director of Science. ?No one has ever attempted such a mission, unique for its scientific implications as well as for its complex and spectacular interplanetary space manoeuvres.? Before reaching its target in 2014, Rosetta will circle the Sun four times on wide loops in the inner Solar System. During its long trek, the spacecraft will have to endure some extreme thermal conditions. Once it is close to Comet Churyumov-Gerasimenko, scientists will take it through a delicate braking manoeuvre; the spacecraft will then closely orbit the comet, and gently drop a lander on it. It will be landing on a small, fast-moving ?cosmic bullet? about whose ‘geography’ very little is known yet.

An amazing 10-year interplanetary trek
Rosetta is a three-tonne box-type spacecraft about three metres high, with two 14-metre solar panels. It consists of an orbiter and a lander. The lander is approximately one metre across and 80 centimetres high. It will be attached to the side of the orbiter during the journey to Comet Churyumov-Gerasimenko. Rosetta carries 21 experiments in total, 10 of them on the lander. They will be kept in hibernation during most of its 10-year trek towards the comet.

Why does Rosetta’s cruise need to take so long? To reach Comet Churyumov-Gerasimenko, the spacecraft needs to go out into deep space as far out from the Sun as Jupiter. No launcher could possibly get Rosetta there directly. ESA’s spacecraft will gather speed from gravitational ?kicks? provided by four planetary fly-bys: one of Mars in 2007 and three of Earth in 2005, 2007 and 2009. During the trip, Rosetta will also twice pass through the asteroid belt, where a fly-by with one or more of these primitive objects is possible. A number of candidate targets have already been identified, but the final selection will be made after launch, once the amount of surplus fuel has been verified by mission engineers. During these encounters, scientists plan to switch on Rosetta’s instruments for scientific studies of these largely unexplored Solar System bodies.

Long trips in deep space include many hazards, such as extreme changes in temperature. Rosetta will leave the benign environment of near-Earth space to the dark, frigid regions beyond the asteroid belt. To manage these thermal loads, experts have done very tough pre-launch tests to study Rosetta’s endurance. For example, they have heated its external surfaces to more than 150?C, then cooled it to -150?C in the next test.

The spacecraft will be fully reactivated prior to the comet rendezvous manoeuvre in 2014. Then, Rosetta will orbit the comet ? an object only about 4 kilometres in diameter – while it cruises through the inner Solar System at 135 000 kilometres per hour. At the time of the rendezvous ? around 675 million kilometres from the Sun ? Comet Churyumov-Gerasimenko will hardly show any surface activity. This means that the characteristic ?coma? (the comet?s ?atmosphere?) and the tail will not be formed yet, because of the distance from the Sun. The comet’s tail is in fact made of dust grains and frozen gases from the comet’s surface that vaporise because of the Sun’s heat.

Over a period of six months, Rosetta will extensively map the comet’s surface, prior to selecting a landing site. In November 2014, the lander will be ejected from the spacecraft from a height which could be as low as one kilometre. Touchdown will be at walking speed, about one metre per second. Immediately after touchdown, the lander will fire a harpoon into the ground to avoid bouncing off the surface back into space, since the comet?s extremely weak gravity alone would not hold onto the lander. Operations and scientific observations on the surface will last at least a week, but may continue for many months. Besides taking close-up pictures, the lander will drill into the dark organic crust and sample the primordial ices and gases.

During and after the lander operations, Rosetta will continue orbiting and studying the comet: it will be the first spacecraft to witness at close quarters the changes taking place in a comet when the comet approaches the Sun and grows its coma and tail and then travels away from it. The trip will end in December 2015, after 12 years of adventure, when the comet has made its closest approach to the Sun and is on its way towards the outer Solar System.

Studying a comet on the spot
Rosetta’s goal is to examine the comet in great detail. The instruments on the orbiter include several cameras and spectrometers that work at different wavelengths: infrared, ultraviolet, visible and microwave. In addition, there are various other instruments to make in situ analysis. Together, they will provide, amongst other things, very high-resolution images and information about the shape, density, temperature and chemical composition of the comet. Rosetta?s instruments will analyse the gases and dust grains in the coma that forms when the comet becomes active, as well as the interaction with the solar wind.

The ten experiments on the lander will make an on-the-spot analysis of the composition and structure of the comet?s surface and subsurface material. A drilling system will take samples down to 30 centimetres below the surface and feed these to the ?composition analysers?. Other instruments will measure properties such as near-surface strength, density, texture, porosity, ice phases and thermal properties. Microscopic studies of individual grains will tell us about the texture.

Ground operations
All scientific data including those relayed from the lander will be stored on the orbiter for downlink to Earth at the next ground station contact. ESA has installed a new deep-space antenna at New Norcia, near Perth in Western Australia, as the main communications link between the spacecraft and ESOC Mission Control in Darmstadt, Germany. This 35-metre diameter parabolic antenna allows the radio signal to reach distances of more than a million kilometres from Earth. The radio signals, travelling at the speed of light, will take up to 50 minutes to cover the distance between the spacecraft and Earth.

Building Rosetta
Rosetta was selected as a mission in 1993. The spacecraft has been built by Astrium Germany as prime contractor. Major subcontractors are Astrium UK (spacecraft platform), Astrium France (spacecraft avionics), and Alenia Spazio (assembly, integration, and verification). Rosetta?s industrial team involves more than 50 contractors from 14 European countries, Canada and the United States.

Scientific consortia from institutes across Europe and the United States have provided the instruments on the orbiter. A European consortium under the leadership of the German Aerospace Research Institute (DLR) has provided the lander. Rosetta has cost ESA EUR 770 million at 2000 economic conditions. This includes the launch and the entire period of development and mission operations from 1996 to 2015. The lander and the experiments, the so-called ‘payload’, are not included since they are funded by the member states through scientific institutes.

Original Source: ESA News Release

Posted on by Fraser Cain

Astronomers See a Star Before it Exploded

Image credit: Gemini
Like a doctor trying to understand an elderly patient’s sudden demise, astronomers have obtained the most detailed observations ever of an old but otherwise normal massive star just before and after its life ended in a spectacular supernova explosion.

Imaged by the Gemini Observatory and Hubble Space Telescope (HST) less than a year prior to the gigantic explosion, the star is located in the nearby galaxy M-74 in the constellation of Pisces. These observations allowed a team of European astronomers led by Dr. Stephen Smartt of the University of Cambridge, England to verify theoretical models showing how a star like this can meet such a violent fate.

The results were published in the January 23, 2004 issue of the journal Science. This work provides the first confirmation of the long-held theory that some of the most massive (yet normal) old stars in the Universe end their lives in violent supernova explosions.

“It might be argued that a certain amount of luck or serendipity was involved in this finding,” said Dr. Smartt. “However, we’ve been searching for this sort of normal progenitor star on its deathbed for some time. I like to think that finding the superb Gemini and HST data for this star is a vindication of our prediction that one day we had to find one of these stars in the immense data archives that now exist.” Click here for more details on Dr. Smartt’s ongoing supernova program.

During the last few years, Smartt’s research team has been using the most powerful telescopes, both in space and on the ground, to image hundreds of galaxies in the hope that one of the millions of stars in these galaxies will some day explode as a supernova. In this case, the renowned Australian amateur supernova hunter, Reverend Robert Evans, made the initial discovery of the explosion (identified as SN203gd) while scanning galaxies with a 12-inch (31cm) backyard telescope from his home in New South Wales, Australia in June, 2003.

Following Evans’ discovery, Dr. Smartt’s team quickly followed up with detailed observations using the Hubble Space Telescope. These observations verified the exact position of the original or “progenitor” star. Using this positional data, Smartt and his team dug through data archives and discovered that observations by the Gemini Observatory and HST contained the combination of data necessary to reveal the nature of the progenitor.

The Gemini data was obtained during the commissioning of the Gemini Multi-Object Spectrograph (GMOS) on Mauna Kea, Hawaii in 2001. These data were also used to produce a stunning high-resolution image of the galaxy that clearly shows the red progenitor star. Click here for the full resolution Gemini image.

Armed with the earlier Gemini and HST observations Smartt’s team was able to demonstrate that the progenitor star was what astronomers classify as a normal red supergiant. Prior to exploding, this star appeared to have a mass about 10 times greater, and a diameter about 500 times greater than that of our Sun. If our sun were the size of the progenitor it would engulf the entire inner solar system out to about the planet Mars.

Red supergiant stars are quite common in the universe and an excellent example can be easily spotted during January from almost anywhere on the Earth by looking at Betelgeuse, the bright red shoulder star in the constellation of Orion (see finder chart here.) Like SN2003gd, it is believed that Betelgeuse could meet the same explosive fate at any time from next week to thousands of years from now.

After SN2003gd exploded, the team observed its gradually fading light for several months using the Isaac Newton Group of telescopes on La Palma. These observations demonstrated that this was a normal type II supernova, which means that the ejected material from the explosion is rich in hydrogen. Computer models developed by astronomers have long predicted that red supergiants with extended, thick atmospheres of hydrogen would produce these type II supernovae but until now have not had the observational evidence to back up their theories. However, the fantastic resolution and depth of the Gemini and Hubble images allowed the Smartt team to estimate the temperature, luminosity, radius and mass of this progenitor star and reveal that it was a normal large, old star. “The bottom-line is that these observations provide a strong confirmation that the theories for both stellar evolution and the origins of these cosmic explosions are correct,” said co-author Seppo Mattila of Stockholm Observatory.

This is only the third time astronomers have actually seen the progenitor of a confirmed supernova explosion. The others were peculiar type II supernovae: SN 1987A, which had a blue supergiant progenitor, and SN 1993J, which emerged from a massive interacting binary star system. Click here for more details.

Dr. Smartt concludes, “Supernova explosions produce and distribute the chemical elements that make up everything in the visible Universe ? especially life. It is critical that we know what type of stars produce these building blocks if we are to understand our origins.”

Archived Gemini and HST data was critical to the success of this project. “This discovery is a perfect example of archival data’s immense value to new scientific projects,” said Dr. Colin Aspin who is the Gemini Scientist responsible for the development of the Gemini Science Archive (GSA). He continued, “this discovery demonstrates the spectacular results that can be realized by using archival data and stresses the importance of developing the GSA for future generations of astronomers.”

The Gemini Multi-Object Spectrograph used to make the Gemini observations are twin instruments built as a joint partnership between Gemini, the Dominion Astrophysical Observatory, Canada, the UK Astronomy Technology Centre and Durham University, UK. Separately, the U.S. National Optical Astronomy Observatory provided the detector subsystem and related software. GMOS is primarily designed for spectroscopic studies where several hundred simultaneous spectra are required, such as when observing star and galaxy clusters. GMOS also has the ability to focus astronomical images on its array of over 28 million pixels.

The Isaac Newton Group of Telescopes (ING) is an establishment of the Particle Physics and Astronomy Research Council (PPARC) of the United Kingdom, the Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO) of the Netherlands and the Instituto de Astrof?sica de Canarias (IAC) in Spain. The ING operates the 4.2 metre William Herschel Telescope, the 2.5 metre Isaac Newton Telescope, and the 1.0 metre Jacobus Kapteyn Telescope. The telescopes are located in the Spanish Roque de Los Muchachos Observatory on La Palma which is operated by the Instituto de Astrof?sica de Canarias (IAC).

Background Information:

Supernovae are among the most energetic phenomena observed in the entire Universe. When a star of more than about eight times the mass of our Sun reaches the end of its nuclear fuel reserve, its core is no longer stable from collapsing under its own immense weight. As the core of the star collapses, the outer layers are ejected in a fast-moving shock wave. This huge energy release results in a supernova that is about one billion times brighter than our Sun, and is comparable to the brightness of an entire galaxy. After destroying itself, the core of the star becomes either a neutron star or a black hole.

The team is composed of Stephen J. Smartt, Justyn R. Maund, Margaret A. Hendry, Christopher A. Tout, and Gerald F. Gilmore (University of Cambridge, UK), Seppo Mattila (Stockholm Observatory, Sweden), and Chris R. Benn (Isaac Newton Group of Telescopes, Spain).

Original Source: Gemini News Release

Posted on by Fraser Cain

Halo Around a Gamma Ray Burst

Image credit: PPARC
The discovery of a unique phenomenon: a beautiful set of expanding X-ray halos surrounding a gamma-ray burst which have never been seen before, (see Movie link at end), has been announced by an international team of astronomers led by Dr Simon Vaughan of the University of Leicester. The research has been accepted for publication in the Astrophysical Journal.

Gamma-ray bursts (GRB) are the most energetic form of radiation in the Universe and can be used to probe any material between Earth and the burst. In this case, the GRB lies behind the plane of our Galaxy, so its light has to travel through the gas and dust in the Galactic disc to reach us.

ESA’s gamma ray observatory satellite ‘Integral’ detected the 30 second long GRB 031203 on December 3rd 2003 and the halos were discovered in a follow-up observation that started 6 hours after the burst with ESA’s ‘XMM-Newton’ X-ray space telescope.

Commenting on the discovery, Professor Ian Halliday, Chief Executive of the UKs Particle Physics and Astronomy Research Council (PPARC) said Gamma-ray bursts are the most violent events in the Universe. Unlike the serene beauty of the stars that we can see with our eyes, the Gamma Ray Universe is a place of dramatic explosions, cosmic collisions and matter being sucked into black holes.

Halliday added This is a wonderful example of two of ESAs most advanced observatories in which UK scientists have made a significant contribution, working in harmony to reveal a new level of scientific understanding.

The fading X-ray emission from the GRB – the afterglow – is clearly seen in the image from the X-ray cameras on XMM-Newton. Uniquely, two rings centred on the afterglow were also seen. Dr Vaughan said “These rings are due to dust in our own Galaxy which is illuminated by the X-rays from the gamma-ray burst. The dust scatters some of the X-rays causing the rings, in the same way as fog scatters the light from a car’s headlights.” He added “Its like a shout in a cathedral; the shout of the gamma-ray burst is louder, but the Galactic reverberation, seen as the rings, is more beautiful.”

Due to the finite speed of light, X-rays from more distant dust reach us later, giving rise to the appearance of expanding rings. Dr Vaughan said “We expect to see an expanding ring on the sky if the dust is in a sheet roughly in the plane of the sky, but as we see two rings there must be two dust sheets between us and the GRB. Understanding how dust is distributed in our Galaxy is important. Dust helps cool gas clouds which can then collapse to form stars and planets. Knowing where dust is located helps astronomers determine where star and planet formation is likely to occur.”

Expanding X-ray dust scattering rings have never been seen before. Slower moving rings seen in visible light around a very few supernovae are caused by a similar effect.

The two halos are due to thin sheets of dust at 2,900 and 4,500 light-years away; the astronomers accurately measured the distances from the expansion rate of the halos. The distances have an uncertainty of just 2%, a remarkable level of accuracy for an object in our Galaxy. The nearest dust sheet is probably part of the Gum nebula, a bubble of hot gas resulting from many supernova explosions. The GRB itself is thought to have occurred in a small galaxy about a billion light-years away (one of the closest GRB galaxies).

Astronomers are still trying to understand the mysterious gamma-ray bursts. Some occur with the supernova explosion of a massive star when it has used up all of its fuel, although only stars which have lost their outer layers and which collapse to make a black hole seem able to make a GRB.

Today Integral and XMM-Newton provide astronomers with their most powerful facilities for studying gamma-ray bursts, but 2004 will see the launch of “Swift”, a new NASA mission with major UK involvement, which will be dedicated to GRBs. This will work in concert with the two ESA satellite observatories, providing more opportunities for discoveries in this cutting edge field. UK participation in Integral, XMM-Newton and Swift is funded by the Particle Physics and Astronomy Research Council.

Original Source: PPARC

Posted on by Fraser Cain

Search for Beagle 2 is Winding Down

Image credit: Beagle 2
No contact has been made with the Beagle 2 lander, despite repeated efforts over the last few days to communicate via the Mars Express and Mars Odyssey spacecraft and the Jodrell Bank radio telescope in Cheshire, UK.

At a press briefing in London this afternoon, members of the Beagle 2 team described the latest efforts to contact their missing lander.

“We haven?t found Beagle 2, despite three days of intensive searching,” said Professor Colin Pillinger, lead scientist for Beagle 2. “Under those circumstances, we have to begin to accept that, if Beagle 2 is on the Martian surface, it is not active.

“That isn?t to say that we are going to give up on Beagle. There is one more thing that we can do – however, it is very much a last resort. We will be asking the American Odyssey spacecraft (team) tomorrow whether they will send an embedded command – a hail to Beagle with a command inside it. If it gets through, it will tell Beagle to switch off and reload the software. We are now working on the basis that there is a corrupt system and the only way we might resurrect is to send that command.”

“We can also ask Mars Express to send that command. However, they cannot send it probably until the 2 or 3 February,” he added.

“We?ll move with the next phase in the search for Beagle 2,” said Professor Pillinger. “We have discussed on our side of the house what we intend to do in the future. We are dedicated to trying to refly Beagle 2 in some shape or form, therefore we need to know how far it got because we need know which parts of this mission we don?t have to study in further detail.”

Detailing the efforts to contact Beagle 2 in recent days, Mark Sims, Beagle 2 Mission Manager from the University of Leicester, explained that the lander should have entered an emergency communication mode known as CSM2 no later than 22 January. In this mode, the spacecraft?s receiver is switched on throughout daylight hours on Mars. The only possible explanation that no communication has been established during the last few days is that the lander?s battery is in a low state of charge.

Meanwhile, the academia-industry “Tiger Team” at the National Space Centre in Leicester is beginning to concentrate on detailed analysis of the possible causes for failure of the mission and the lessons that can be learned for future missions.

The analysis of the mission now under way includes an assessment of the landing site ellipse from orbital images, reanalysis of atmospheric conditions during the entry into the Martian atmosphere on 25 December, examination of the separation from Mars Express and of the cruise phase preceding arrival at Mars.

One extremely useful piece of evidence could be provided by an image of the lander. The team is hoping that the High Resolution Stereo Camera on Mars Express or the camera on board Mars Global Surveyor may eventually be able to capture an image that reveals its location on the Martian surface.

Original Source: PPARC News Release

Posted on by Fraser Cain

Opportunity is in a Small Crater

Image credit: NASA/JPL
A small impact crater on Mars is the new home for NASA’s Opportunity rover, and a larger crater lies nearby. Scientists value such crater locations as a way to see what’s beneath the surface without needing to dig.

Encouraging developments continued for Opportunity’s twin, Spirit, too. Engineers have determined that Spirit’s flash memory hardware is functional, strengthening a theory that Spirit’s main problem is in software that controls file management of the memory. “I think we’ve got a patient that’s well on the way to recovery,” said Mars Exploration Rover Project Manager Pete Theisinger at NASA’s Jet Propulsion Laboratory, Pasadena, Calif.

Opportunity returned the first pictures of its landing site early today, about four hours after reaching Mars. The pictures indicate that the spacecraft sits in a shallow crater about 20 meters (66 feet) across.

“We have scored a 300-million mile interplanetary hole in one,” said Dr. Steve Squyres of Cornell University, Ithaca, N.Y., principal investigator for the science instruments on both rovers.

NASA selected Opportunity’s general landing area within a region called Meridiani Planum because of extensive deposits of a mineral called crystalline hematite, which usually forms in the presence of liquid water. Scientists had hoped for a specific landing site where they could examine both the surface layer that’s rich in hematite and an underlying geological feature of light-colored layered rock. The small crater appears to have exposures of both, with soil that could be the hematite unit and an exposed outcropping of the lighter rock layer.

“If it got any better, I couldn’t stand it,” said Dr. Doug Ming, rover science team member from NASA Johnson Space Center, Houston. With the instruments on the rover and just the rocks and soil within the small crater, Opportunity should be allow scientists to determine which of several theories about the region’s past environment is right, he said. Those theories include that the hematite may have formed in a long-lasting lake or in a volcanic environment.

An even bigger crater, which could provide access to deeper layers for more clues to the past, lies nearby. Images taken by a camera on the bottom of the lander during Opportunity’s final descent show a crater about 150 meters (about 500 feet) across likely to be within about one kilometer or half mile of the landing site, said Dr. Andrew Johnson of JPL. He is an engineer for the descent imaging system that calculated the spacecraft’s horizontal motion during its final seconds of flight. The system determined that sideways motion was small, so Opportunity’s computer decided not to fire the lateral rockets carried specifically for slowing that motion.

Squyres presented an outline for Opportunity’s potential activities in coming weeks and months. After driving off the lander, the rover will first examine the soil right next to the lander, then drive to the outcrop of layered-looking rocks and spend considerable time examining it. Then the rover may climb out of the small crater, take a look around, and head for the bigger crater.

But first, Opportunity will spend more than a week — perhaps two — getting ready to drive off the lander, if all goes well. Engineering data from Opportunity returned in relays via NASA’s Mars Odyssey orbiter early this morning and at midday indicate the spacecraft is in excellent health, said JPL’s Arthur Amador, mission manager. The rover will try its first direct-to-Earth communications this evening.

The main task for both rovers in coming months is to explore the areas around their landing sites for evidence in rocks and soils about whether those areas ever had environments that were watery and possibly suitable for sustaining life.

JPL, 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 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

Posted on by Fraser Cain

Engineers Restore Communications With Spirit

Image credit: NASA/JPL
Hours before NASA’s Opportunity rover will reach Mars, engineers have found a way to communicate reliably with its twin, Spirit, and to get Spirit’s computer out of a cycle of rebooting many times a day.

Spirit’s responses to commands sent this morning confirm a theory developed overnight that the problem is related to the rover’s two “flash” memories or software controlling those memories.

“The rover has been upgraded from critical to serious,” said Mars Exploration Rover Project Manager Peter Theisinger at NASA’s Jet Propulsion Laboratory, Pasadena, Calif. Significant work is still ahead for restoring Spirit, he predicted.

Opportunity is on course for landing in the Meridiani Planum region of Mars. The center of an ellipse covering the area where the spacecraft has a 99 percent chance of landing is just 11 kilometers (7 miles) from the target point. That point was selected months ago. Mission managers chose not to use an option for making a final adjustment to the flight path. Previously, the third and fifth out of five scheduled maneuvers were skipped as unnecessary. ” We managed to target Opportunity to the desired atmospheric entry point, which will bring us to the target landing site, in only three maneuvers,” said JPL’s Dr. Louis D’Amario, navigation team chief for the rovers.

Opportunity will reach Mars at 05:05 Sunday, Universal Time (12:05 a.m. Sunday EST or 9:05 p.m. Saturday PST).

From the time Opportunity hits the top of Mars? atmosphere at about 5.4 kilometers per second (12,000 miles per hour) to the time it hits the surface 6 minutes later, then bounces, the rover will be going through the riskiest part of its mission. Based on analysis of Spirit’s descent and on weather reports about the atmosphere above Meridiani Planum, mission controllers have decided to program Opportunity to open its parachute slightly earlier than Spirit did.

Mars is more than 10 percent farther from Earth than it was when Spirit landed. That means radio signals from Opportunity during its descent and after rolling to a stop have a lower chance of being detected on Earth. About four hours after the landing, news from the spacecraft may arrive by relay from NASA’s Mars Odyssey orbiter. However, that will depend on Opportunity finishing critical activities, such as opening the lander petals and unfolding the rover’s solar panels, before Odyssey flies overhead.

Spirit has 256 megabytes of flash memory, a type commonly used on gear such as digital cameras for holding data even when the power is off. Engineers confirmed this morning that Spirit’s recent symptoms are related to the flash memory when they commanded the rover to boot up and utilize its random-access memory instead of flash memory. The rover then obeyed commands about communicating and going into sleep mode. Spirit communicated successfully at 120 bits per second for nearly an hour.

“We have a vehicle that is stable in power and thermal, and we have a working hypothesis we have confirmed,” Theisinger said. By commanding Spirit each morning into a mode that avoids using flash memory, engineers plan to get it to communicate at a higher data rate, to diagnose the root cause of the problem and develop ways to restore as much functioning as possible.

The work on restoring Spirit is not expected to slow the steps in getting Opportunity ready to roll off its lander platform if Opportunity lands safely. For Spirit, those steps took 12 days.

The rovers’ main task is to explore their landing sites for evidence in the rocks and soil about whether the sites’ past environments 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. 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

Posted on by Fraser Cain

Opportunity Joins Spirit on Mars

Image credit: NASA/JPL

NASA’s Opportunity rover successfully landed on the surface of Mars early Sunday morning, giving the agency two successful landings this month. The spacecraft landed in a region of Mars called Meridiani Planum which is on the opposite side of the planet from Gusev Crater. Initial estimates placed the rover about 24 km down range from the centre of the target area, but well within the regions of hematite which could be an indication of past water. Unlike Spirit, Opportunity landed on its side and righted itself when it opened the petals of its lander. Opportunity’s airbags aren’t blocking the exit ramp, so there won’t be a problem when the rover rolls out onto the Martian surface.

NASA’s second Mars Exploration Rover successfully sent signals to Earth during its bouncy landing and after it came to rest on one of the three side petals of its four-sided lander.

Mission engineers at NASA’s Jet Propulsion Laboratory, Pasadena, Calif., received the first signal from Opportunity on the ground at 9:05 p.m. Pacific Standard Time Saturday via the NASA Deep Space Network, which was listening with antennas in California and Australia.

“We’re on Mars, everybody!” JPL’s Rob Manning, manager for development of the landing system, announced to the cheering flight team.

NASA Administrator Sean O’Keefe said at a subsequent press briefing, “This was a tremendous testament to how NASA, when really focused on an objective, can put every ounce of effort, energy, emotion and talent to an important task. This team is the best in the world, no doubt about it.”

Opportunity landed in a region called Meridiani Planum, halfway around the planet from the Gusev Crater site where its twin rover, Spirit, landed three weeks ago. Earlier today, mission managers reported progress in understanding and dealing with communications and computer problems on Spirit.

“In the last 48 hours, we’ve been on a roller coaster,” said Dr. Ed Weiler, NASA associate administrator for space science. “We resurrected one rover and saw the birth of another.”

JPL’s Pete Theisinger, project manager for the rovers, said, “We are two for two. Here we are tonight with Spirit on a path to recovery and with Opportunity on Mars.”

By initial estimates, Opportunity landed about 24 kilometers (15 miles) down range from the center of the target landing area. That is well within an outcropping of a mineral called gray hematite, which usually forms in the presence of water. “We’re going to have a good place to do science,” said JPL’s Richard Cook, deputy project manager for the rovers.

Once it pushed itself upright by opening the petals of the lander, Opportunity was expected to be facing east.

The main task for both rovers in coming months is to explore the areas around their landing sites for evidence in rocks and soils about whether those areas ever had environments that were 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. 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

Posted on by Fraser Cain

Engineers Struggle to Reestablish Link to Spirit

Image credit: NASA/JPL

NASA engineers have been working overtime to reestablish communications with the Spirit rover after it mysteriously stopped talking to mission control on Wednesday just before it executed an experiment to grind a few millimeters into a rock. They did receive a reassuring confirmation on Thursday that Spirit was receiving transmissions from Earth; although, it hasn’t sent any data back yet. The engineers aren’t sure what caused the problem, but since they did get that confirmation, it’s probably not in the power system, radio, transmitter or some software. A very slow communications link was established on Friday morning, but it’s still unclear exactly what’s wrong or if it’s repairable.

NASA’s Spirit rover communicated with Earth in a signal detected by NASA’s Deep Space Network antenna complex near Madrid, Spain, at 12:34 Universal Time (4:34 a.m. PST) this morning.

The transmissions came during a communication window about 90 minutes after Spirit woke up for the morning on Mars. The signal lasted for 10 minutes at a data rate of 10 bits per second.

Mission controllers at NASA’s Jet Propulsion Laboratory, Pasadena, Calif., plan to send commands to Spirit seeking additional data from the spacecraft during the subsequent few hours.

JPL, 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 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