Posted on by Fraser Cain

Saturn and Jupiter Formed Differently

Nearly five billion years ago, the giant gaseous planets Jupiter and Saturn formed, apparently in radically different ways.

So says a scientist at the University of California’s Los Alamos National Laboratory who created exhaustive computer models based on experiments in which the element hydrogen was shocked to pressures nearly as great as those found inside the two planets.

Working with a French colleague, Didier Saumon of Los Alamos’ Applied Physics Division created models establishing that heavy elements are concentrated in Saturn’s massive core, while those same elements are mixed throughout Jupiter, with very little or no central core at all. The study, published in this week’s Astrophysical Journal, showed that refractory elements such as iron, silicon, carbon, nitrogen and oxygen are concentrated in Saturn’s core, but are diffused in Jupiter, leading to a hypothesis that they were formed through different processes.

Saumon collected data from several recent shock compression experiments that have showed how hydrogen behaves at pressures a million times greater than atmospheric pressure, approaching those present in the gas giants. These experiments – performed over the past several years at U.S. national labs and in Russia – have for the first time permitted accurate measurements of the so-called equation of state of simple fluids, such as hydrogen, within the high-pressure and high-density realm where ionization occurs for deuterium, the isotope made of a hydrogen atom with an additional neutron.

Working with T. Guillot of the Observatoire de la Cote d’Azur, France, Saumon developed about 50,000 different models of the internal structures of the two giant gaseous planets that included every possible variation permitted by astrophysical observations and laboratory experiments.

“Some data from earlier planetary probes gave us indirect information about what takes place inside Saturn and Jupiter, and now we’re hoping to learn more from the Cassini mission that just arrived in Saturn’s orbit,” Saumon said. “We selected only the computer models that fit the planetary observations.”

Jupiter, Saturn and the other giant planets are made up of gases, like the sun: They are about 70 percent hydrogen by mass, with the rest mostly helium and small amounts of heavier elements. Therefore, their interior structures were hard to calculate because hydrogen’s equation of state at high pressures wasn’t well understood.

Saumon and Guillot constrained their computer models with data from the deuterium experiments, thereby reducing previous uncertainties for the equation of state of hydrogen, which is the central ingredient needed to improve models of the structures of the planets and how they formed.

“We tried to include every possible variation that might be allowed by the experimental data on shock compression of deuterium,” Saumon explained.

By estimating the total amount of the heavy elements and their distribution inside Jupiter and Saturn, the models provide a better picture of how the planets formed through the accretion of hydrogen, helium and solid elements from the nebula that swirled around the sun billions of years ago.

“There’s been general agreement that the cores of Saturn and Jupiter are different,” Saumon said. “What’s new here is how exhaustive these models are. We’ve managed to eliminate or quantify many of the uncertainties, so we have much better confidence in the range within which the actual data will fall for hydrogen, and therefore for the refractory metals and other elements.

“Although we can’t say our models are precise, we know quite well how imprecise they are,” he added.

These results from the models will help guide measurements to be taken by Cassini and future proposed interplanetary space probes to Jupiter.

Los Alamos National Laboratory is operated by the University of California for the National Nuclear Security Administration (NNSA) of the U.S. Department of Energy and works in partnership with NNSA’s Sandia and Lawrence Livermore national laboratories to support NNSA in its mission.

Los Alamos develops and applies science and technology to ensure the safety and reliability of the U.S. nuclear deterrent; reduce the threat of weapons of mass destruction, proliferation and terrorism; and solve national problems in defense, energy, environment and infrastructure.

Original Source: Los Alamos News Release

Posted on by Fraser Cain

New Plan to Move an Asteroid

On 9 July 2004, the Near-Earth Object Mission Advisory Panel recommended that ESA place a high priority on developing a mission to actually move an asteroid. The conclusion was based on the panel?s consideration of six near-Earth object mission studies submitted to the Agency in February 2003.

Of the six studies, three were space-based observatories for detecting NEOs and three were rendezvous missions. All addressed the growing realisation of the threat posed by Near-Earth Objects (NEOs) and proposed ways of detecting NEOs or discovering more about them from a close distance.

A panel of six experts, known as the Near-Earth Object Mission Advisory Panel (NEOMAP) assessed the proposals. Alan Harris, German Aerospace Centre (DLR), Berlin, and Chairman of NEOMAP, says, ?The task has been very difficult because the goalposts have changed. When the studies were commissioned, the discovery business was in no way as advanced as it is now. Today, a number of organisations are building large telescopes on Earth that promise to find a very large percentage of the NEO population at even smaller sizes than visible today.?

As a result, the panel decided that ESA should leave detection to ground-based telescopes for the time being, until the share of the remaining population not visible from the ground becomes better known. The need for a space-based observatory will then be re-assessed. The panel placed its highest priority on rendezvous missions, and in particular, the Don Quijote mission concept. ?If you think about the chain of events between detecting a hazardous object and doing something about it, there is one area in which we have no experience at all and that is in directly interacting with an asteroid, trying to alter its orbit,? explains Harris.

The Don Quijote mission concept will do this by using two spacecraft, Sancho and Hidalgo. Both are launched at the same time but Sancho takes a faster route. When it arrives at the target asteroid it will begin a seven-month campaign of observation and physical characterisation during which it will land penetrators and seismometers on the asteroid?s surface to understand its internal structure.

Sancho will then watch as Hidalgo arrives and smashes into the asteroid at very high speed. This will provide information about the behaviour of the internal structure of the asteroid during an impact event as well as excavating some of the interior for Sancho to observe. After the impact, Sancho and telescopes from Earth will monitor the asteroid to see how its orbit and rotation have been affected.

Harris says, ?When we do actually find a hazardous asteroid, you could imagine a Don Quijote-type mission as a precursor to a mitigation mission. It will tell us how the target responds to an impact and will help us to develop a much more effective mitigation mission.?

On 9 July, the findings were presented to the scientific and industrial community. Representatives of other national space agencies were also invited in the hope that they will be interested in developing a joint mission, based around this concept.

Andr?s Galvez, ESA?s Advanced Concepts Team and technical officer for the NEOMAP report says, ?This report gives us a solid foundation to define programmatic priorities and an implementation strategy, in which I also hope we are joined by international partners?.

With international cooperation, a mission could be launched as early as 2010-2015.

The six mission concepts studied were:

* Earthguard-1 ? a small space telescope for NEO discovery, especially the Atens and ?inner-Earth objects? (IEOs) that are difficult to detect from the ground.
* European Near-Earth Object Survey (EUNEOS) ? a space telescope for NEO discovery
* NEO Remote Observations (NERO) ? an optical/infrared space telescope for NEO discovery and physical characterisation.
* Smallsat Intercept Missions to Objects Near Earth (SIMONE) ? a flotilla of low-cost microsatellites for near-Earth asteroid rendezvous and in-situ remote sensing
* Internal Structure High-resolution Tomography by Asteroid Rendezvous (ISHTAR) ? uses radar tomography for an in-situ study of internal structure
* Don Quijote ? uses explosive charges, an impactor, seismic detectors and accelerometers for an in-situ study of internal structure and momentum transfer

Original Source: ESA News Release

Posted on by Fraser Cain

Two Ecosystems in Antarctica’s Vostok?

Scientists from the Lamont-Doherty Earth Observatory (LDEO) at Columbia University and Rensselaer Polytechnic Institute in New York State have developed the first-ever map of water depth in Lake Vostok, which lies between 3,700 and 4,300 meters (more than 2 miles) below the continental Antarctic ice sheet. The new comprehensive measurements of the lake?roughly the size of North America’s Lake Ontario?indicate it is divided into two distinct basins that may have different water chemistry and other characteristics. The findings have important implications for the diversity of microbial life in Lake Vostok and provide a strategy for how scientists study the lake?s different ecosystems should international scientific consensus approve exploration of the pristine and ancient environment.

Michael Studinger, of the Lamont-Doherty Earth Observatory (LDEO) at Columbia University, said that the existence of two distinct regions with the lake would have significant implications for what sorts of ecosystems scientists should expect to find in the lake and how they should go about exploring them.

“The ridge between the two basins will limit water exchange between the two systems,” he said. “Consequently, the chemical and biological composition of these two ecosystems is likely to be different.”

The National Science Foundation (NSF), an independent federal agency that supports fundamental research and education across all fields of science and engineering, supported the work. NSF manages the U.S. Antarctic Program, which coordinates almost all U.S. science on the southernmost continent.

The new measurements are significant because they provide a comprehensive picture of the entire lakebed and indicate that the bottom of the lake contains a previously unknown, northern sub-basin separated from the southern lakebed by a prominent ridge.

Using laser altimeter, ice-penetrating radar and gravity measurements collected by aircraft, Studinger and Robin Bell, of LDEO, and Anahita Tikku, formerly of the University of Tokyo and now at Rensselaer Polytechnic Institute, estimate that Lake Vostok contains roughly 5400 cubic kilometers (1300 cubic miles) of water. Their measurements also indicate that the top of the ridge dividing the two basins is only 200 meters (650 feet) below the bottom of the icesheet. Elsewhere, the water ranges from roughly 400 meters (1,300 feet) deep in the northern basin to 800 meters (2,600 feet) deep in its southern counterpart.

Water that passes through the lake starts on one end as melted ice from the very bottom of the ice sheet, which refreezes at the other end. According to the new measurements, the base of the ice sheet melts predominantly over the smaller northern basin, while the water in the lake refreezes over the larger southern basin. The researchers assert that water takes between 55,000 and 110,000 years to cycle through the lake.

The arrangement of the two basins, their separation and the characteristics of the meltwater may, the scientists conclude, all have implications for the circulation of water within the lake. It is possible, for example, that if the water in the lake were fresh, meltwater in the northern basin would sink to the bottom of that basin, limiting the exchange of waters between the two basins. The meltwater in the adjacent basin likely would be different.

The two lake basins, they argue, could therefore have very different bottoms.

The scientists also point out that the waters of the two basins may, as a result of the separation, have a very different chemical and even biological composition. Indeed, Lake Vostok, is also of interest to those who search for microbial life elsewhere in the solar system. The lake is thought to be a very good terrestrial analog of the conditions on Europa, a frozen moon of Jupiter. If life can exist in Vostok, scientists have argued, then microbes also might thrive on Europa.

The new measurements also indicate that different strategies may be needed to target sampling of specific types of lake sediments. Those released from the ice sheet represent the rocks over which the ice traveled, for example, and would be more prominent in the northern basin. Material in the southern basin would be more likely to represent the environmental conditions before the ice sheet sealed off the lake.

Scientists deciding whether and how to proceed with an exploration of Lake Vostok say a great deal of technological development would likely be needed before a device could be deployed to conduct contamination-free sampling. Currently, no scientific sampling of the lake is being carried out.

The ultimate goal of any sampling would be to obtain water and sediment samples from the lake bottom.

The team published the new maps in the June 19 edition of Geophysical Research Letters, a publication of the American Geophysical Union.

Original Source: NSF News Release

Posted on by Fraser Cain

Saturn’s Southern Atmosphere

Cassini captured intriguing cloud structures on Saturn as it neared its rendezvous with the gas giant. Notable is the irregularity in the eastern edge of the dark southern polar collar. The image was taken with the narrow angle camera on May 21, 2004, from a distance of 22 million kilometers (13.7 million miles) from Saturn through a filter sensitive to absorption and scattering of sunlight in the near infrared by methane gas (centered at 727 nanometers). The image scale is 131 kilometers (81 miles) per pixel. No contrast enhancement has been performed on this image.

The Cassini-Huygens mission is a cooperative project of NASA, the European Space Agency and the Italian Space Agency. The Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Cassini-Huygens mission for NASA’s Office of Space Science, Washington, D.C. The imaging team is based at the Space Science Institute, Boulder, Colorado.

For more information about the Cassini-Huygens mission, visit http://saturn.jpl.nasa.gov and the Cassini imaging team home page, http://ciclops.org.

Posted on by Fraser Cain

The Search for More Earths

Until a decade ago, astronomers weren’t even sure there were any planets outside the Solar System. You’d be hard-pressed to find anyone who believed we had the only planets in the entire Universe, but we still didn’t have any direct evidence they existed. That all changed in October 5, 1995 when Michel Mayor and Didier Queloz announced they had discovered a planet half the mass of Jupiter orbiting furiously around a star called 51 Pegasi. The discoveries came fast; at last count, there are 122 confirmed extrasolar planets.

But these extrasolar systems generally look nothing like our own Solar System. Many contain massive planets which orbit extremely close to their parent star; no chance for life there. Planets roughly the size and orbit of Jupiter have been uncovered, but it’s impossible for the current technology to see anything the size of our own Earth.

Fortunately, there’s a series of ground and space-based observatories in the works that should be capable of detecting Earth-sized planets around other stars. NASA and the ESA are working towards the goal of being able to directly photograph these planets and measure the composition of their atmospheres. Find large amounts of oxygen, and you’ve found life.

Corot – 2006
The European Space Agency will be the first off the mark in the hunt for rocky planets with the launch of Corot in 2006. It’ll carefully monitor the brightness of stars, watching for a slight dimming that happens in regular intervals. These dimmings are called “transits”, and happen when a planet passes in between the Earth and a distant star. The concept of a “transit” should be fresh in your mind – Venus performed one recently on June 8, 2004. Corot will be sensitive enough to detect rocky planets as small as 10 times the size of the Earth.

A follow on mission, Eddington, was originally scheduled for launch in 2007, would have been able to spot planets half the size of the Earth. But it was recently canceled, unfortunately.

Kepler – 2007
The first space observatory designed to find Earth-sized planets in orbit around other stars will be Kepler, named after the German astronomer who devised the laws of planetary motion. It’s scheduled to launch in 2007, and will also use the transit method to detect planets.

Kepler has an extremely sensitive photometer hooked up to its one-metre telescope. It’ll monitor the brightness of hundreds of thousands of stars in a chunk of sky about the same size as your outstretched hand, and watch for that telltale periodic “dimming”.

Over the course of its four year mission, Kepler should discover plenty of objects orbiting other stars, and its photometer is just sensitive enough that it should notice an Earth-sized planet as it crosses in front of a star for a few hours.

Space Interferometry Mission – 2009
Next up will be the Space Interferometry Mission, due for launch in 2009. Once in space, the SIM will take up a position in orbit that trails the Earth as it goes around the Sun, slowly drifting further and further away – this’ll give it a good, stable view of the heavens, without having the Earth around to block the view.

The observatory is designed to measure the distance to stars with incredible precision. It’s so precise, that it should be able to spot a star being moved through the gravitational interaction with its planets. For example, if you looked at the position of our own Sun from a distant point, it would look like it’s wobbling around thanks to the gravity of Jupiter, Saturn, and even the Earth. SIM will be able to detect a star’s interactions with planets down to the size of a few times the mass of the Earth. That’s precise.

Terrestrial Planet Finder – 2012-2015
Unlike the previous missions, which will detect Earth-sized planets indirectly, the Terrestrial Planet Finder (TPF) will “see” them. It’s scheduled for launch in 2012 and will nullify the light from distant stars by a factor of 100,000 times, revealing their planets. The final design is still in the works, but it could end up being a group of spacecraft flying in close formation, merging their light together to form a much larger virtual space telescope.

The TPF will pick up where SIM leaves off, surveying the habitable zone of stars 50 light years away from the Earth. Not only will it be able to see Earth-sized planets in these zones, it’ll be able to analyze the composition of their atmospheres. Here’s the key: the TPF will be able to spot the presence of oxygen, water vapour, methane and carbon dioxide in Earth-sized planets in the habitable zone of other stars. If could find the fingerprint for life in the atmospheres of these planets.

Find life on other planets, and you can assume that it’s probably common throughout our Milky Way galaxy, and maybe even the entire Universe.

Darwin – 2014
Shortly after the TPF gets to work, the European Space Agency is planning to launch Darwin; a flotilla of 8 spacecraft working together to find Earth-sized planets and search for the chemical signatures of life. Darwin will be the most powerful space-based observatory, providing images 10-times more detailed than even the James Webb Space Telescope (due for launch 2009).

Stars are billions of times brighter than the planets that orbit them, so Darwin will solve this problem by observing in the infrared spectrum, where this difference is much smaller. It’ll also be capable of canceling out starlight to reveal the much dimmer planets.

Darwin is similar enough to the Terrestrial Planet Finder, that the two agencies are considering combining their designs into a single mission funded by both groups.

Maybe we aren’t alone after all.
In just a decade, and less than 20 years after the discovery of the first planets orbiting other stars, astronomers should be able to supply us with an answer to one of the most fundamental questions humans have asked themselves… are we alone? If the Terrestrial Planet Finder hasn’t turned up evidence of life yet, then the answer will still be, “not yet”. But there’s a chance that in 10 years, you’ll be reading news that that life has been discovered orbiting another star.

But that won’t be the end of it. The scientists will press on, with new equipment, observatories and techniques to search even deeper into space. And the philosophers and theologians will get to work considering our place in a very crowded Universe.

Posted on by Fraser Cain

Zubrin on Terraforming Mars

As a former Martin-Marietta aerospace engineer, prolific author and founder of the non-profit Mars Society (1998), Robert Zubrin is regarded as the driving force behind the proposed Mars Direct mission to reduce the cost and complexity of interplanetary travel. The flight plan calls for a return journey fueled by rocket propellant harvested in situ, from the martian atmosphere itself.

As described in Zubrin’s book, The Case for Mars: The Plan to Settle the Red Planet, the Mars Direct concept eventually became a cornerstone of a frugal ‘living off the land’ approach to travel in NASA’s Design Reference Mission. 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 stashed supplies once on Mars.

“For our generation and many that will follow, Mars is the New World,” writes Zubrin. The New York Times Book Review (Dennis Overbye) indicated how such an outline initially was greeted as breaking conventional wisdom about martian mission plans: “Part history, part call to arms, part technical manual, part wishful thinking, The Case for Mars … lays out an ingenious plan. ……one of the most provocative and hopeful documents I have read about the space program in 20 years.”

The Mars Society continues to grow across many countries with thousands of members interested in space advocacy, particularly how best to encourage the exploration and settlement of Mars. Notable among the Society’s members are science-fiction author, Greg Benford, and Academy Award winning director, James Cameron.

Astrobiology Magazine had the opportunity to talk with Robert Zubrin about the possibilities for terraforming Mars.

Astrobiology Magazine (AM): First off, should Mars be terraformed?

Robert Zubrin (RZ): Yes.

AM: Does Mars contain all of the elements needed to make the planet habitable, or will we have to import gases, chemicals, etc., from elsewhere? If so, then will Mars always need constant inputs to achieve habitability, or do you think that given enough inputs Mars would reach a tipping point and planetary processes would create a self-sustaining feed-back loop?

RZ: It appears that Mars does have all the elements needed for terraforming. The one outstanding question is nitrogen, whose inventory remains unknown. However theory suggests that Mars should have had an initial supply of nitrogen comparable to the Earth, and it seems likely that much of this is still there.

AM: How long will terraforming take? When you envision a terraformed Mars, what do you see?

RZ: If one considers the problem of terraforming Mars from the point of view of current technology, the scenario looks like this:

1. A century to settle Mars and create a substantial local industrial capability and population.
2. A half century producing fluorocarbon gases (like CF4) to warm the planet by ~10 C.
3. A half century for CO2 to outgas from the soil under the impetus of the fluorocarbon gases, thickening the atmosphere to 0.2 to 0.3 bar, and raising the planetary temperature a further 40 C. This will cause water to melt out of the permafrost, and rivers to flow and rain to fall. Radiation doses on the surface will also be greatly reduced. Under these conditions, with active human help, first photosynthetic microbes and then ever more complex plants could be spread over the planet, as they would be able to grow in the open. Humans on Mars in this stage would no longer need pressure suits, just oxygen masks, and very large domed cities could be built, as the domes would no longer need to contain pressure greater than the outside environment.
4. Over a period of about a thousand years, human-disseminated and harvested plants would be able to put ~150 mbar (millibars) of oxygen in the Martian atmosphere. Once this occurs, humans and other animals will be able to live on Mars in the open, and the world will become fully alive.

That’s the scenario, using current technological approaches. However technology is advancing, and 23rd Century humans will not conduct their projects using 21st Century means. They will use 23rd Century means and accomplish the job much faster than anyone today can suppose.

So if someone in the 24th Century, living on a fully terraformed Mars, should discover this interview, I believe that she will view it in much the same way as we today look at Jules Verne’s lunar mission design. We today look at Verne’s ideas and say “Amazing, a man living a hundred years before Apollo foresaw it — and not only that– launched his crew of three from Florida, and returned them in a capsule landing in the Pacific Ocean where they were picked up by a US warship, all as things actually happened. But launching people with heavy artillery – how 19th Century can you get?” So our 24th Century Martian historian studying this interview will smile and say; “Incredible. Here are people 300 years ago talking about terraforming Mars. But doing it with fluorocarbon gases and green plants –how 20th century can you get?”

AM: Who should the first human colonists to Mars be and how should they be chosen? Since Martian gravity is one-third of Earth’s, wouldn’t bone and muscle loss, along with radiation, make colonization a one-way journey? What are the implications of what, from an Earth-perspective, is exile?

RZ: Life is a one-way trip, and we are all permanently exiled from our past. In that sense Mars colonists, and all colonists, are no different from anyone else. It is just more apparent in their case, as in addition to leaving behind the time of their past, they also leave behind the place. But in so doing, they gain the opportunity to create a world where none existed before, and thus gain a form of immortality that is denied to those who are content to accept the world they are born in.

AM: If there’s life on Mars, how do we balance the Martian right to life with the human impulse to explore and extend our borders?

RZ: The basis of ethics needs to be of benefit to humanity. If there is life on Mars, it is microbial, and its interests can in no way be considered as commensurate with human interests. Those who argue otherwise strike a fashionable pose, but deny their arguments every day through their actions. If bacterial interests trump human interests, then mouthwash should be banned, chlorination of water supplies should be banned, and antibiotics should be banned. If bacterial interests trump human interests, then Albert Schweitzer and Louis Pasteur should be denounced for crimes against bacteria.

Now, in saying that ethics must be based in human benefit, we need not deny that preserving valuable environments in important. It is important to save the amazon rain forest, for example, because a world without an amazon rain forest would be a poorer inheritance for our descendants than one with one, and the degree of the impoverishment exceeds whatever value might be obtained in the short term from slash and burn agriculture. However, in the case of Mars, the calculation votes the other way, as a terraformed Mars, filled with life, cities, universities, used book stores, and yes, rain forests, would be a vastly richer gift to posterity than the current barren Red Planet. Clearly, just as anyone who proposed transforming the current Earth into a place like Mars would be considered mad, so those who, given the choice, would keep Mars dead rather than make it a place as wonderful as the Earth must have their sanity doubted.

There remains only the question of science. Surely we should avail ourselves of the opportunity to study native Martian life before we terraform the place. We surely will. Terraforming Mars will be a long term project, and should native Martian microbes exist, there will be ample opportunity to study it before terraforming takes place. There will also be opportunity to study how it adapts to warmer, wetter conditions and the presence of terrestrial microbes after terraforming takes place. Furthermore, if Mars actually is terraformed, there will be much more people on Mars to study every aspect of Mars, including both its native and immigrant life. So in fact, our knowledge of Martian biota will be increased by terraforming, not decreased.

AM: Humans sent to live on Mars will bring with them ideas on how to govern themselves, rules of conduct for living in society, economic motivations, and personality conflicts. How should the colonization of Mars be managed, and how should Mars be governed? Should the colonization of Mars be a cooperative effort among every nation, or should only those that financial contribute be in charge of the operation?

RZ: The Founding Fathers of the United States called our infant republic a “Noble Experiment,” a place where the grand liberal ideas of the Enlightenment could be given a run, and the idea of a government based on the rights on man could be tested to see if it could succeed in practice. Their Noble Experiment did succeed, and as a result became the model for a new and better form of human social organization worldwide.

Mars can, should, and will be a place for numerous new Noble Experiments. The well of human social thought has not yet run dry, nor do I believe that we have yet discovered the ultimate and most humanistic form of society possible. In the 22nd Century, as in the 18th, there will always be people who think they have discovered a better way, and need a place to go where the rules haven’t been written yet so they can give their ideas a try. For these, the Martian frontier will beckon. Many of their ideas will prove impractical, and their colonies will fail. But some of those who really have a better idea will succeed, and in doing so, light the way forward for all humanity.

So, to answer your question, I say that the colonization of Mars should not be managed at all, but be done through the joyful chaos of human freedom.

AM: Taking a leap into the future, let’s assume the technology, biology, sociology, and politics have all combined to create a unique sub-race of humanity on Mars. Generations of human beings have now been born, grown, bred and died on Mars. Who are these Martians?

RZ: In 1893, the great historian Frederick Jackson Turner wrote:

“To the frontier the American intellect owes its striking characteristics. That coarseness of strength combined with acuteness and inquisitiveness; that practical inventive turn of mind, quick to find expedients; that masterful grasp of material things, lacking in the artistic but powerful to effect great ends; that restless, nervous energy; that dominant individualism, working for good and evil, and withal that buoyancy and exuberance that comes from freedom — these are the traits of the frontier.”

I think that says it all. The pioneers of the Martian frontier will be the Americans of the future.

Original Source: Astrobiology Magazine

Posted on by Fraser Cain

Observatory Finds Its First Planet

McDonald Observatory astronomers Bill Cochran, Michael Endl, and Barbara McArthur have exploited the Hobby-Eberly Telescope’s (HET’s) capabilities to rapidly find and confirm, with great precision, the giant telescope’s first planet outside our solar system. The event serves as proof-of-concept that HET, combined with its High Resolution Spectrograph instrument, is on track to become a major player in the hunt for other worlds. The research has been accepted for publication in an upcoming edition of Astrophysical Journal Letters.

With a mass 2.84 times that of Jupiter, the newly discovered planet orbits the star HD 37605 every 54.23 days. HD 37605 is a little smaller and little cooler than the Sun. The star, which is of a type called “K0” or “K-zero,” is rich in heavy chemical elements compared to the Sun.

Of the approximately 120 extrasolar planets found to date, this new planet has the third most eccentric orbit bringing it in close in to its parent star like a “hot Jupiter,” and swinging it back out. The planet’s average distance from its star is 0.26 Astronomical Units (AU). One AU is the Earth-Sun distance.

The team used the “radial velocity” technique, a common planet-search method, to find the planet. By measuring changes in the star’s velocity toward and away from Earth –its wobble– they deduced that HD 37605 is orbiting the center of mass of a star-planet system.

“In 100 days of observations –less than two full orbits– we were able to get a very good solution for this planet’s orbit,” Cochran said. The quick results were due to HET’s “queue scheduling” system. Astronomers do not travel to the observatory to operate the telescope themselves. Rather, a telescope operator at McDonald Observatory has a list of all HET research projects and selects the ones best suited to any given night’s weather conditions and Moon phase. This way, many targets for different research projects can be observed each night, and any particular target can be observed dozens of nights in a row. According to Cochran, “queue scheduling is the ideal way to do planet searching. If the HET had a normal scheduling system, it would have taken us a year or two to confirm this planet.”

Endl added that “with the queue scheduling mode, we can put every candidate star BACK into the queue at a high priority to secure follow-up telescope observations immediately.”

Cochran added that the high precision of the team’s radial velocity measurements “proves that the HET and the High Resolution Spectrograph have met their design specs.” He explained that the total error (called “root-mean-square deviation”) in the team’s velocity measurements was 3 meters per second — state of the art for planet searching. Many of the team’s measurements had even lower errors. The High Resolution Spectrograph that made this research possible was built by Phillip MacQueen, Robert Tull, and John Good of The University of Texas at Austin.

The Hobby-Eberly Telescope is a joint project of The University of Texas at Austin, The Pennsylvania State University (Penn State), Stanford University, Ludwig-Maximilians-Universitat Muenchen, and Georg-August- Universitat Goettingen.

This planet detection research is supported by the National Aeronautics and Space Administration.”

Original Source: University of Texas at Austin News Release

Posted on by Fraser Cain

Blue Moon on July 31

When you hear someone say “Once in a Blue Moon?” you know what they mean: Rare. Seldom. Maybe even absurd. After all, when was the last time you saw the moon turn blue?

On July 31st, you should look, because there’s going to be a Blue Moon.

According to modern folklore, a Blue Moon is the second full moon in a calendar month. Usually months have only one full moon, but occasionally a second one sneaks in. Full moons are separated by 29 days, while most months are 30 or 31 days long; so it is possible to fit two full moons in a single month. This happens every two and a half years, on average.

July has already had one full moon on July 2nd. The next, on July 31st, is by definition a Blue Moon.

But will it really be blue? Probably not. The date of a full moon, all by itself, doesn’t affect the moon’s color. The moon on July 31st will be pearly-gray, as usual. Unless….

There was a time, not long ago, when people saw blue moons almost every night. Full moons, half moons, crescent moons–they were all blue, except some nights when they were green.

The time was 1883, the year an Indonesian volcano named Krakatoa exploded. Scientists liken the blast to a 100-megaton nuclear bomb. Fully 600 km away, people heard the noise as loud as a cannon shot. Plumes of ash rose to the very top of Earth’s atmosphere. And the moon turned blue.

Krakatoa’s ash is the reason. Some of the ash-clouds were filled with particles about 1 micron (one millionth of a meter) wide–the right size to strongly scatter red light, while allowing other colors to pass. White moonbeams shining through the clouds emerged blue, and sometimes green.

Blue moons persisted for years after the eruption. People also saw lavender suns and, for the first time, noctilucent clouds. The ash caused “such vivid red sunsets that fire engines were called out in New York, Poughkeepsie, and New Haven to quench the apparent conflagration,” according to volcanologist Scott Rowland at the University of Hawaii.

Other less potent volcanos have turned the moon blue, too. People saw blue moons in 1983, for instance, after the eruption of the El Chichon volcano in Mexico. And there are reports of blue moons caused by Mt. St. Helens in 1980 and Mount Pinatubo in 1991.

The key to a blue moon is having in the air lots of particles slightly wider than the wavelength of red light (0.7 micron)–and no other sizes present. This is rare, but volcanoes sometimes spit out such clouds, as do forest fires:

“On September 23, 1950, several muskeg fires that had been quietly smoldering for several years in Alberta suddenly blew up into major–and very smoky–fires,” writes physics professor Sue Ann Bowling of the University of Alaska. “Winds carried the smoke eastward and southward with unusual speed, and the conditions of the fire produced large quantities of oily droplets of just the right size (about 1 micron in diameter) to scatter red and yellow light. Wherever the smoke cleared enough so that the sun was visible, it was lavender or blue. Ontario and much of the east coast of the U.S. were affected by the following day, but the smoke kept going. Two days later, observers in England reported an indigo sun in smoke-dimmed skies, followed by an equally blue moon that evening.”

In the western U.S., there will be wildfires burning on July 31st. If any of those fires produce ash or oily-smoke containing lots of 1-micron particles, the Blue Moon there could be blue.

More likely, it’ll be red. Ash and dust clouds thrown into the atmosphere by fires and storms usually contain a mixture of particles with a wide range of sizes. Most are smaller than 1 micron, and they tend to scatter blue light. This kind of cloud makes the Moon turn red; indeed, red Blue Moons are far more common than blue Blue Moons.

Absurd? Yes, but that’s what a Blue Moon is all about. Step outside at sunset on July 31st, look east, and see for yourself.

Original Source: NASA Science Article

Posted on by Fraser Cain

Forum Reaches its First Birthday

Exactly one year today I was nagged into setting up the Universe Today forum as a way for space enthusiasts to come together and discuss all things space and astronomy. Despite my initial reluctance, it’s been incredibly successful, becoming one of the larger communities of this topic on the Internet – I wish I’d done it sooner. As I’m looking right now, we have 2422 members who’ve written 34354 posts. So, I’d like to make a special thanks to all the contributors, moderators, and experts who have participated so far, I really appreciate all your hard work.

If you have questions about space, want to explore any topic deeper, or just make friends who share your interests in space, come and join us.

Fraser Cain
Publisher
Universe Today

P.S. If you’ve had problems accessing the forum, or setting up an account, let me know, and I’d be happy to help you out. I know it can be a little confusing if you’ve never joined one before.

Posted on by Fraser Cain

Wallpaper: Saturn’s Rings in Ultraviolet

The best view ever of Saturn’s rings in the ultraviolet indicates there is more ice toward the outer part of the rings, hinting at ring origin and evolution, say two University of Colorado at Boulder researchers involved in the Cassini mission.

Researchers from CU-Boulder’s Laboratory for Atmospheric and Space Physics, Joshua Colwell and Larry Esposito, said the UV spectra taken during the Cassini spacecraft’s orbital insertion June 30 show definite compositional variation in the A, B and C rings.

Esposito, who discovered the F ring around Saturn in 1979 using Pioneer 11 data, is the team leader for Cassini’s Ultraviolet Imaging Spectrograph, or UVIS, a $12.5 million instrument riding on the spacecraft. A UVIS team member and ring expert, Colwell created the color-enhanced images from the spectra.

The CU-Boulder built UVIS instrument is capable of resolving the rings to show features up to 60 miles across, roughly 10 times the resolution obtained by the Voyager 2 spacecraft. The instrument was able to resolve the “Cassini division,” discovered by Giovanni Domenico Cassini in the 17th century, which separates the A and B rings of Saturn, proving the rings are not one contiguous feature.

The ring system begins from the inside out with the D, C, B and A rings followed by the F, G and E rings. The red in both images indicates sparser ringlets likely made of “dirty,” and possibly smaller, particles than in the denser, icier turquoise ringlets.

Original Source: University of Colorado News Release