ExoMars: 'giant nose' to sniff out life on Mars prepares for launch

Space engineers are making final preparations for the launch of a robot spacecraft designed to sniff out signs of life on Mars.

The probe, ExoMars 2016 – the first of a two-phase exploration of the Red Planet by European and Russian scientists – is scheduled to be blasted into space on a Proton rocket from Baikonour cosmodrome in Kazakhstan at 0931 GMT on Monday.

The spacecraft consists of a module called Schiaparelli that will test heat shields and parachutes in preparation for future probe landings on Mars and a second main component, the Trace Gas Orbiter or TGO, that will analyse the planet’s atmosphere. In particular it will seek out the presence of the gas methane which, on Earth, is produced by living organisms.

“Essentially our spacecraft is a giant nose in the sky,” said Jorge Vago, an ExoMars project scientist based with the European Space Agency (Esa). “We are going to use it to sniff out the presence of methane on Mars and determine if it is being produced by biological processes.”

Methane is normally destroyed by ultraviolet radiation within a few hundred years of its creation. Its presence on Mars would therefore suggest life had recently been active there. The US robot rover Curiosity, which landed on Mars in 2012, initially found no sign of methane. Subsequent analyses in 2014 did report the presence of methane in the Martian atmosphere in one area. However, some scientists have argued that it may have been created by non-biological means.

On Earth most methane is generated biologically, but it can be made by chemical processes under the surface. To differentiate between these two processes, the ExoMars trace gas detector will not only analyse methane levels in more detail than any previous mission but also study other gases that will provide information about its likely source. “If methane is found in the presence of other complex hydrocarbon gases, such as propane or ethane, that will be a strong indication that biological processes are involved,” said another project scientist, Manish Patel, of the Open University.

“However, if we find methane in the presence of gases such as sulphur dioxide, a chemical strongly associated with volcanic activity on Earth, that will be a pretty sure sign that we are dealing with methane that has come from the ground and is a byproduct of geological processes.”

By NASA, ESA, and The Hubble Heritage Team (STScI/AURA) [Public domain], via Wikimedia Commons

ExoMars is expected to arrive at the Red Planet on 19 October after a journey of 308m miles (496m km) across space, and will be followed by a second ExoMars mission, a Mars rover, scheduled for launch in 2018 – although Esa officials have warned that it may be delayed by budget problems.

On Friday, Russian engineers completed the rollout of the giant Proton rocket that will carry ExoMars to its destination, and on Saturday, staff at Esa’s mission control centre in Darmstadt, Germany – which will run the mission once in space – conducted a dress rehearsal for the launch. “We do a similar dress rehearsal for every launch,” said Paolo Ferri, head of mission operations for Esa. “It’s a milestone that caps off several years of preparation for any complex mission – designing, building and testing the ground systems, preparing the flight operations procedures and then finally an intensive period of team training.”

Finally, on Monday, the spacecraft is scheduled take off from Baikonour. Then, when it has reached orbit, the TGO, still linked to the Schiaparelli test lander, will separate from the fourth stage of its Proton launcher and begin its seven-month journey to the Red Planet.

For more information, visit:-

https://www.theguardian.com/science/2016/mar/13/exomars-giant-nose-life-on-mars-prepares-launch

http://www.prlabs.co.uk/lab-supplies.php?N=bisdiphenylphosphino-methane-for-sy&Id=38134

Celebrating women in science on International Women’s Day: Dorothy Mary Hodgkin

Dorothy Mary Hodgkin OM FRS (12 May 1910 – 29 July 1994), known professionally as Dorothy Crowfoot Hodgkin or simply Dorothy Hodgkin, was a British biochemist who developed protein crystallography, for which she won the Nobel Prize in Chemistry in 1964.

She advanced the technique of X-ray crystallography, a method used to determine the three-dimensional structures of biomolecules. Among her most influential discoveries are the confirmation of the structure of penicillin that Ernst Boris Chain and Edward Abraham had previously surmised, demonstrating (contrary to scientific opinion at the time) that it contains a β-lactam ring. She also confirmed the structure of vitamin B12, for which she became the third woman to win the Nobel Prize in Chemistry.  In 1945, working with C. H. (Harry) Carlisle, she published the first such structure of a steroid, cholesteryl iodide (having worked with cholesteryls since the days of her doctoral studies). 

In 1948, Hodgkin first encountered vitamin B12 and created new crystals. Vitamin B12 had first been discovered by Merck earlier that year. Vitamin B12 had a structure at the time that was almost completely unknown, and when Hodgkin discovered it contained cobalt, she realized the structure actualization may be determined by x-ray crystallography analysis. The large size of the molecule, and that the atoms were largely unaccounted for - aside from cobalt - posed a challenge in structure analysis that hadn't been previously explored.

Molecular structure of vitamin B12, by NEUROtiker (Own work) [Public domain], via Wikimedia Commons

From these crystals, she deduced the presence of a ring structure because the crystals were pleochroic, a finding which she later confirmed using X-ray crystallography. The B12 study published by Hodgkin was described by Lawrence Bragg as being as significant "as breaking the sound barrier." Scientists from Merck had previously crystallised B12, but had published only refractive indices of the substance. The final structure of B12, for which Hodgkin was later awarded the Nobel Prize, was published in 1955.

In 1969, after 35 years of work and five years after winning the Nobel Prize, Hodgkin was able to decipher the structure of insulin. X-ray crystallography became a widely used tool and was critical in later determining the structures of many biological molecules where knowledge of structure is critical to an understanding of function. She is regarded as one of the pioneer scientists in the field of X-ray crystallography studies of biomolecules.

For more information visit:-

https://en.wikipedia.org/wiki/Dorothy_Hodgkin

http://www.prlabs.co.uk/lab-supplies.php?N=300l-msia-darts-protein-ag&Id=19593

On this day in history - the Bikini H-Bomb test took place

In 1954, at Bikini, in the Pacific Ocean, the blast of the U.S. hydrogen bomb code-named Bravo was the most powerful of all U.S. thermonuclear bomb tests in the area.

The 15 megaton nuclear explosion far exceeded the expected yield of 4 to 8 megatons (6Mt predicted), and was about 1,000 times more powerful than each of the atomic bombs dropped on Hiroshima and Nagasaki during World War II. The scientists and military authorities were shocked by the size of the explosion and many of the instruments they had put in place to evaluate the effectiveness of the device were destroyed.

Bikini is a Pacific archipelago that is part of the Marshall Islands. In this test, one of the atolls was totally vaporized and disappeared in the over 100-mile wide mushroom cloud.

Fallout exceeded predictions. Earlier tests began in 1946 after the indigenous people were evacuated to an island believed to be a safe distance away. (They were moved again in 1949.)

Castle Bravo blast. By United States Department of Energy [Public domain], via Wikimedia Commons

The military authorities and scientists had promised the Bikini Atoll's native residents that they would be able to return home after the nuclear tests. A majority of the island's family heads agreed to leave the island, and most of the residents were moved to the Rongerik Atoll and later to Kili Island. Both locations proved unsuitable to sustaining life, resulting in starvation and requiring the residents to receive ongoing aid.

Despite the promises made by authorities, nuclear tests rendered Bikini unfit for habitation, contaminating the soil and water, making subsistence farming and fishing too dangerous. The United States later paid the islanders and their descendants $2 billion in compensation for damage caused by the nuclear testing program and their displacement from their home island.  

As of 2014, it may be technically possible for the former residents and their descendants to live on the atoll's islands, but virtually none of those alive today have ever lived on the atoll and very few want to move there.

For more information visit:

https://en.wikipedia.org/wiki/Nuclear_testing_at_Bikini_Atoll

http://www.todayinsci.com/3/3_01.htm

http://www.prlabs.co.uk/lab-supplies.php?N=urea-hydrogen-peroxide&Id=1606

Iron meteorites 'buried in Antarctica' by the Sun

New research suggests there could be a layer of iron-rich meteorites hidden just under the Antarctic ice.

The churning of glaciers spews many space rocks out on to the surface in Antarctica, but compared to elsewhere on Earth, few of them are made of iron.

Based on modelling and lab experiments, scientists say the missing metallic rocks might be burying themselves, by melting the ice as sunlight heats them.

To prove their idea, the team now wants to look for the rocks themselves.

"The study is proposing a hypothesis - these samples should be there. We just have to go and locate them," said Dr Katherine Joy from the University of Manchester, a co-author of the paper published in Nature Communications.

Antarctica is known by meteorite specialists as a fruitful hunting ground, because the rocks are collected from their landing sites by glacial flows and transported to concentrated dumping-grounds.

"The great thing about Antarctica is they fall on the ice, and then the ice progressively moves away from the plateau. And where it hits these barriers, along the Transantarctic Mountains, the ice gets moved up," Dr Joy told the BBC.

"So this continuous conveyor belt has delivered meteorites from the interior fall sites to the 'meteorite stranding zones' for the past couple of million years or so."

Iron meteorites. By Waifer X (originally posted to Flickr as 090423-1080887) [CC BY 2.0 (http://creativecommons.org/licenses/by/2.0)], via Wikimedia Commons

Among this Antarctic haul, however, researchers have noticed that iron-rich meteorites - whether partly or wholly made of the metal - are surprisingly scarce, compared to the percentage collected in other places around the world.

Dr Joy and her colleagues think they may have discovered why.

They froze two small meteorites of similar size and shape, one made of iron and the other rocky and non-metallic, inside blocks of ice. A special lamp was trained on the ice from above, to mimic the rays of the Sun.

Both meteorites, on repeated trials, melted their way downward through the ice block. But because the metal conducts heat more efficiently, the iron meteorite sank further, faster.

The researchers then expanded that observation using a mathematical simulation. Their model showed that this Sun-driven burrowing would be enough to cause iron-rich rocks to sink so much during the long summer days that, over the course of the year, it would account fairly precisely for the lack of iron space rocks welling their way to the surface of the Antarctic "stranding zones".

"The idea is, they never make it to the surface. They're forever trapped, 50-100cm or so below the ice," Dr Joy explained.

That means, if the team's findings are to be believed, that the hunt is on.

As Dr Joy's Manchester colleague Geoffrey Evatt put it: "The challenge is now set - to be the first team to locate this reserve of meteorites and retrieve samples from it."

Of all the meteorites gathered from Antarctica, only a handful - so far - have been pulled out from beneath the ice. This is mostly for practical reasons, Dr Joy said.

"When it's very cold... picking up the sample in a controlled way is difficult enough with things sitting on the surface. To access ones that are subsurface - nobody's really tried to do that so far."

So it will not be easy, but the team hopes that radar and metal detectors might help target the search. And the potential rewards are high.

"Every meteorite we find tells us something new about the Solar System," Dr Joy said.

Some are carbon-rich or rocky remnants from long before any planet clumped together; others - like iron and rocky-iron meteorites - offer clues from a more intermediate stage, when baby planets with cores, mantles and crusts were trying to form.

"The iron group represents meteorites that were once the cores and the internal structures of different planetesimals.

"We think there were probably hundreds of these early planets, that formed in the solar system but never really got big enough and were broken up in collision events."

For more information visit:-

http://www.bbc.co.uk/news/science-environment-35587680

http://www.prlabs.co.uk/lab-supplies.php?N=iron-1000ppm-for-icp&Id=60140

Rising sea levels will threaten residents of many countries, say researchers.

At the rate humans are emitting carbon into the atmosphere, Earth may suffer irreparable damage that could last tens of thousands of years, according to a new analysis published this week.

Rising sea levels will threaten residents of many countries, say researchers.

Too much of the climate change policy debate has focused on observations of the past 150 years and their impact on global warming and sea level rise by the end of this century, the authors say. Instead, policy-makers and the public should also be considering the longer-term impacts of climate change.

"Much of the carbon we are putting in the air from burning fossil fuels will stay there for thousands of years - and some of it will be there for more than 100,000 years," said Peter Clark, an Oregon State University paleoclimatologist and lead author on the article. "People need to understand that the effects of climate change on the planet won't go away, at least not for thousands of generations."

The researchers' analysis is being published this week in the journal Nature Climate Change.

Thomas Stocker of the University of Bern in Switzerland, who is past-co-chair of the IPCC's Working Group I, said the focus on climate change at the end of the 21st century needs to be shifted toward a much longer-term perspective.

"Our greenhouse gas emissions today produce climate-change commitments for many centuries to millennia," said Stocker, a climate modeler and co-author on the Nature Climate Change article. "It is high time that this essential irreversibility is placed into the focus of policy-makers.

"The long-term view sends the chilling message (about) what the real risks and consequences are of the fossil fuel era," Stocker added. "It will commit us to massive adaptation efforts so that for many, dislocation and migration becomes the only option."

Sea level rise is one of the most compelling impacts of global warming, yet its effects are just starting to be seen. The latest IPCC report, for example, calls for sea level rise of just one meter by the year 2100. In their analysis, however, the authors look at four difference sea level-rise scenarios based on different rates of warming, from a low end that could only be reached with massive efforts to eliminate fossil fuel use over the next few decades, to a higher rate based on the consumption of half the remaining fossil fuels over the next few centuries.

With just two degrees (Celsius) warming in the low-end scenario, sea levels are predicted to eventually rise by about 25 meters. With seven degrees warming at the high-end scenario, the rise is estimated at 50 meters, although over a period of several centuries to millennia.

"It takes sea level rise a very long time to react - on the order of centuries," Clark said. "It's like heating a pot of water on the stove; it doesn't boil for quite a while after the heat is turned on - but then it will continue to boil as long as the heat persists. Once carbon is in the atmosphere, it will stay there for tens or hundreds of thousands of years, and the warming, as well as the higher seas, will remain."

Clark said for the low-end scenario, an estimated 122 countries have at least 10 percent of their population in areas that will be directly affected by rising sea levels, and that some 1.3 billion - or 20 percent of the global population - live on lands that may be directly affected. The impacts become greater as the warming and sea level rise increases.

"We can't keep building seawalls that are 25 meters high," noted Clark, a professor in OSU's College of Earth, Ocean, and Atmospheric Sciences. "Entire populations of cities will eventually have to move."

Daniel Schrag, the Sturgis Hooper Professor of Geology at Harvard University, said there are moral questions about "what kind of environment we are passing along to future generations."

"Sea level rise may not seem like such a big deal today, but we are making choices that will affect our grandchildren's grandchildren - and beyond," said Schrag, a co-author on the analysis and director of Harvard's Center for the Environment. "We need to think carefully about the long time-scales of what we are unleashing."

The new paper makes the fundamental point that considering the long time scales of the carbon cycle and of climate change means that reducing emissions slightly or even significantly is not sufficient. "To spare future generations from the worst impacts of climate change, the target must be zero - or even negative carbon emissions - as soon as possible," Clark said.

"Taking the first steps is important, but it is essential to see these as the start of a path toward total decarbonization," Schrag pointed out. "This means continuing to invest in innovation that can someday replace fossil fuels altogether. Partial reductions are not going to do the job."

Stocker said that in the last 50 years alone, humans have changed the climate on a global scale, initiating the Anthropocene, a new geological era with fundamentally altered living conditions for the next many thousands of years.

"Because we do not know to what extent adaptation will be possible for humans and ecosystems, all our efforts must focus on a rapid and complete decarbonization -the only option to limit climate change," Stocker said.

For more information, visit:-

https://www.sciencedaily.com/releases/2016/02/160211143109.htm

https://www.prlabs.co.uk/lab-supplies.php?N=carbon-disulfide-for-spectroscopy-uvasol&Id=22853

On this day in history – an atom of the element 112 was created

In 1996, only a little more than a year after they created element 111, a team of German scientists led by Peter Armbruster at the Gesellschaft für schwerionenforschung (GSI) facility at Darmstadt, Germany, claimed to have created an atom of the element 112. Its nucleus has 112 protons and 166 neutrons, giving it a mass number of 277. As a new element it was named ununbium, symbol Uub, according to an internationally adopted system for naming new elements. This was based on the presence of one atom of the element made by accelerating zinc atoms to high speed and bombarding them into lead. When an atom of each fused to make the new nucleus, it lasted a fraction of a thousandth of a second before decaying, emitting an alpha particle to become a nucleus of element 110.

What is an element?

A chemical element or element is a species of atoms having the same number of protons in their atomic nuclei (i.e. the same atomic number, Z). There are 118 elements that have been identified, of which the first 94 occur naturally on Earth with the remaining 24 being synthetic elements. There are 80 elements that have at least one stable isotope and 38 that have exclusively radioactive isotopes, which decay over time into other elements. Iron is the most abundant element (by mass) making up the Earth, while oxygen is the most common element in the crust of the earth.

The Periodic Table, by Sandbh (Own work) via Wikimedia Commons

Chemical elements constitute all of the ordinary matter of the universe. However astronomical observations suggest that ordinary observable matter is only approximately 15% of the matter in the universe: the remainder is dark matter, the composition of which is unknown, but it is not composed of chemical elements. The two lightest elements, hydrogen and helium were mostly formed in the Big Bang and are the most common elements in the universe. The next three elements (lithium, beryllium and boron) were formed mostly by cosmic ray spallation, and are thus more rare than those that follow. Formation of elements with from six to twenty six protons occurred and continues to occur in main sequence stars via stellar nucleosynthesis. The high abundance of oxygen, silicon, and iron on Earth reflects their common production in such stars. Elements with greater than twenty-six protons are formed by supernova nucleosynthesis in supernovae, which, when they explode, blast these elements far into space as planetary nebulae, where they may become incorporated into planets when they are formed.

The term "element" is used for a kind of atom with a given number of protons (regardless of whether they are or they are not ionized or chemically bonded, e.g. hydrogen in water) as well as for a pure chemical substance consisting of a single element (e.g. hydrogen gas).

When different elements are chemically combined, with the atoms held together by chemical bonds, they form chemical compounds. Only a minority of elements are found uncombined as relatively pure minerals. Among the more common of such "native elements" are copper, silver, gold, carbon (as coal, graphite, or diamonds), and sulphur. All but a few of the most inert elements, such as noble gases and noble metals, are usually found on Earth in chemically combined form, as chemical compounds. While about 32 of the chemical elements occur on Earth in native uncombined forms, most of these occur as mixtures. For example, atmospheric air is primarily a mixture of nitrogen, oxygen, and argon, and native solid elements occur in alloys, such as that of iron and nickel.

The history of the discovery and use of the elements began with primitive human societies that found native elements like carbon, sulphur, copper and gold. Later civilizations extracted elemental copper, tin, lead and iron from their ores by smelting, using charcoal. Alchemists and chemists subsequently identified many more, with almost all of the naturally-occurring elements becoming known by 1900.

The properties of the chemical elements are summarized on the periodic table, which organizes the elements by increasing atomic number into rows ("periods") in which the columns ("groups") share recurring ("periodic") physical and chemical properties. Save for unstable radioactive elements with short half-lives, all of the elements are available industrially, most of them in high degrees of purity.

For more information visit:-

http://www.prlabs.co.uk/lab-supplies.php?N=zinc-hydroxide-carbonate-pure-zinc-carb&Id=40516

http://www.todayinsci.com/2/2_09.htm

https://en.wikipedia.org/wiki/Chemical_element

Moon was produced by a head-on collision between Earth and a forming planet

The moon was formed by a violent, head-on collision between the early Earth and a "planetary embryo" called Theia approximately 100 million years after the Earth formed, UCLA geochemists and colleagues report.

Scientists had already known about this high-speed crash, which occurred almost 4.5 billion years ago, but many thought the Earth collided with Theia (pronounced THAY-eh) at an angle of 45 degrees or more -- a powerful side-swipe (simulated in this 2012 YouTube video). New evidence reported Jan. 29 in the journal Science substantially strengthens the case for a head-on assault.

The researchers analyzed seven rocks brought to the Earth from the moon by the Apollo 12, 15 and 17 missions, as well as six volcanic rocks from the Earth's mantle - five from Hawaii and one from Arizona.

By Gregory H. Revera (Own work) [CC BY-SA 3.0 (http://creativecommons.org/licenses/by-sa/3.0) or GFDL (http://www.gnu.org/copyleft/fdl.html)], via Wikimedia Commons

The key to reconstructing the giant impact was a chemical signature revealed in the rocks' oxygen atoms. (Oxygen makes up 90 percent of rocks' volume and 50 percent of their weight.) More than 99.9 percent of Earth's oxygen is O-16, so called because each atom contains eight protons and eight neutrons. But there also are small quantities of heavier oxygen isotopes: O-17, which have one extra neutron, and O-18, which have two extra neutrons. Earth, Mars and other planetary bodies in our solar system each has a unique ratio of O-17 to O-16 - each one a distinctive "fingerprint."

In 2014, a team of German scientists reported in Science that the moon also has its own unique ratio of oxygen isotopes, different from Earth's. The new research finds that is not the case.

"We don't see any difference between the Earth's and the moon's oxygen isotopes; they're indistinguishable," said Edward Young, lead author of the new study and a UCLA professor of geochemistry and cosmochemistry.

Young's research team used state-of-the-art technology and techniques to make extraordinarily precise and careful measurements, and verified them with UCLA's new mass spectrometer.

The fact that oxygen in rocks on the Earth and our moon share chemical signatures was very telling, Young said. Had Earth and Theia collided in a glancing side blow, the vast majority of the moon would have been made mainly of Theia, and the Earth and moon should have different oxygen isotopes. A head-on collision, however, likely would have resulted in similar chemical composition of both Earth and the moon.

"Theia was thoroughly mixed into both the Earth and the moon, and evenly dispersed between them," Young said. "This explains why we don't see a different signature of Theia in the moon versus the Earth."

Theia, which did not survive the collision (except that it now makes up large parts of Earth and the moon) was growing and probably would have become a planet if the crash had not occurred, Young said. Young and some other scientists believe the planet was approximately the same size as the Earth; others believe it was smaller, perhaps more similar in size to Mars.

Another interesting question is whether the collision with Theia removed any water that the early Earth may have contained. After the collision - perhaps tens of millions of year later - small asteroids likely hit the Earth, including ones that may have been rich in water, Young said. Collisions of growing bodies occurred very frequently back then, he said, although Mars avoided large collisions.

A head-on collision was initially proposed in 2012 by Matija, now a research scientist with the SETI Institute, and Sarah Stewart, now a professor at UC Davis; and, separately during the same year by Robin Canup of the Southwest Research Institute.

Co-authors of the Science paper are Issaku Kohl, a researcher in Young's laboratory; Paul Warren, a researcher in the UCLA department of Earth, planetary, and space sciences; David Rubie, a research professor at Germany's Bayerisches Geoinstitut, University of Bayreuth; and Seth Jacobson and Alessandro Morbidelli, planetary scientists at France's Laboratoire Lagrange, Université de Nice.

The research was funded by NASA, the Deep Carbon Observatory and a European Research Council advanced grant (ACCRETE).

For more information visit:-

http://www.sciencedaily.com/releases/2016/01/160129090451.htm

http://www.prlabs.co.uk/lab-supplies.php?N=oxygen-sensor&Id=75102