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Meteorite points to asteroid Vesta’s dynamo

A team of scientists in the US says that the asteroid Vesta probably had a rotating liquid core in its early history. This, the researchers say, created a dynamo that produced a magnetic field strong enough to magnetize the rocks on its surface. As it was previously thought that only larger planets, such as Earth, had dynamos, the work suggests that protoplanets, like asteroids, may be more planet-like than previously thought. The findings could help researchers better understand the early history of the formation of the solar system.

Vesta is one of the most massive asteroids in the solar system, second only to the dwarf planet Ceres. The Dawn mission to study both Vesta and Ceres was launched by NASA in 2007. It entered orbit around Vesta on 16 July 2011 then on 5 September this year it left orbit and it is currently en route to Ceres, where it is scheduled to arrive in February 2015. Vesta is known to have lost about 1% of its mass in a collision that is thought to have occurred a billion years ago. This left a massive impact crater occupying much of Vesta’s southern hemisphere and debris from this event has fallen to Earth as howardite–eucrite–diogenite (HED) meteorites. These have been traced back to the asteroid by matching the unique oxygen-isotope “fingerprints”, which prove that the meteorites originated from Vesta.

Active cores

It is samples of one of these meteorites – an eucrite meteorite ALHA81001, found in Antartica – that Roger Fu and colleagues from the Paleomagnetism Laboratory at the Massachusetts Institute of Technology in the US have studied. “Our group studies magnetism in rocks – terrestrial rocks, lunar rocks and, now, we have been studying meteorites from Vesta,” explains Fu. He points out that the Dawn spacecraft does not have a magnetometer on-board, so the magnetic properties of the asteroid must be inferred from the HED meteorites that are being tested in the lab.

Vesta has a metallic core, which consists of 5–25% of its total planetary mass and is thought to have formed sometime within the first 1–4 million years of the solar system’s existence. Via remote sensing, Dawn has made the most accurate measurement yet of Vesta’s current size, and has approximated Vesta’s core to be about 107–113 km in radius.

Fu and colleagues now say that Vesta’s liquid metallic core once had a dynamo. This is the means by which a planetary body creates and maintains a magnetic field via a rotating, convecting and electrically conducting fluid at its core. “If a rock cools in a magnetic field, it records the magnetic properties of the field; so by studying it in the lab, we can deduce the strength of the field,” explains Fu. The team did other studies using argon–argon dating and concluded that the meteorite acquired its magnetic signature about 3.69 billion years ago from a surface magnetic field large enough to have been created by an ancient core dynamo. Because this period of magnetization was well before the impact in which the meteorite was created, the team can conclude that the magnetization could not have been induced as a result of the meteorite re-heating on Earth. “When the meteorite formed 3.7 billion years ago, Vesta did not have an active core dynamo. So, this means that there had to be a considerable surface magnetic field on Vesta – to induced magnetism in the rocks – that remained even after the core was not active,” says Fu.

Magnetic sunscreen?

In addition, other data show that the surface of Vesta seems to be less space-weathered than expected. If a sample of the Vesta meteorite is exposed to an ionized beam – representing ionized solar wind that causes weathering – the sample changes colour and mineralogical changes are seen too. “But what we actually see on Vesta is different – it is not as weathered. Something is preventing the solar wind from eroding it as much, and there is a good chance that it is the magnetic-field remnant that is doing so,” says Fu. He says that the strength of the field required to shield the Vestian surface from the solar wind matches that of the actual field strength deduced from the meteorite. “There is a linear relation between the strength of magnetism in the rocks and the strength of the field they were formed in, so we can calculate it. And the strength of the magnetic field corresponds to the size of the core dynamo, which depends on how big the core is, so it is all linked,” says Fu. These findings, combined with the Dawn data, have also provided the final evidence necessary to say that the HED meteorites do originate from Vesta. “There is no lingering doubt now,” explains Fu.

In the future, Fu and colleagues will consider magnetism in the early solar system; indeed, they hope to study magnetic fields in protoplanetary discs. “Theorists have not modelled magnetic fields in nebulae in decades, and we would like to do that,” says Fu.

The research is published in Science.

Carbon dioxide ‘corrodes’ ice, say scientists

The amount of carbon dioxide in the atmosphere has risen from roughly 280 ppm shortly before the industrial revolution to about 390 ppm today. Now researchers in the US have done atom-level simulations that suggest that increased concentrations of the gas causes ice to become more brittle, and so more likely to break up or crack. Although the work focussed on tiny “nanocrystals” of ice, the team believes that it could improve our understanding of cracking in much larger structures such as glaciers and ice caps.

“This result suggests that the chemical composition of the atmosphere can be critical to mediating the motion and/or melting of large volumes of ice, beyond the effect of global temperature,” Markus Buehler of the Massachusetts Institute of Technology (MIT) explains. “In some sense the fracture of ice due to carbon dioxide is similar to the breakdown of materials due to corrosion, e.g. the structure of a car, building or power plant where chemical agents ‘gnaw’ at the materials, which slowly deteriorate. In the case of ice, carbon dioxide can play the role of a corroding agent and lead to a destabilization of the structure.”

Glaciers and ice caps cover 7% of the Earth, an area greater than Europe and North America. They reflect 80–90% of incoming solar radiation and act as a carbon sink – this means that significant melting could create a feedback loop and boost warming further.

Breaking bonds

“Similarly to other materials, the fracture process of bulk ice, for example glaciers, is usually initiated by single cracks propagating in ice crystals by breaking the hydrogen bonds between water molecules,” says Buehler. “These cracks eventually grow and break down the entire glacier by propagating and branching over large distances. Very large-scale ice fractures occurred recently close to Pine Island Glacier [in Antarctica], which generated an iceberg with an area the same size as the city of Berlin.”

Buehler and colleague Zhao Qin used atomic simulations to examine the effect of carbon dioxide on crack growth in ice. They calculated that ice containing 2% carbon dioxide was less strong than pure ice and 38% less tough, with a fracture toughness of 12.0 kPam1/2 rather than 19.4 kPam1/2.

“It is difficult for experiments alone to directly measure the nanoscale properties of ice as a function of carbon-dioxide concentration,” says Buehler. “That is why we decided to use a series of first-principles-based atomistic-level computer simulations to investigate the very detailed mechanisms.”

Molecules move towards crack tip

The team found that carbon dioxide disrupts the hydrogen bonds between water molecules in the ice, since the oxygen atoms in the gas have a partial negative-charge and are attracted to the positively charged hydrogen atoms of the water. In the simulations, carbon-dioxide molecules attached to the crack surface and moved towards the crack tip, breaking hydrogen bonds between water molecules as they went.

“If ice caps and glaciers were to continue to crack and break into pieces, the surface area that is exposed to air would be significantly increased, which could lead to accelerated melting and much reduced coverage area on the Earth,” says Buehler. “The consequences of these changes remain to be explored by the experts, but they might contribute to changes of the global climate.”

Buehler says that the technique used in the study has also been applied to study the mechanical properties of protein materials and polymers, whose structures are typically stabilized by hydrogen bonds. “For these structures, we found that the chemical conditions, for example, pH, ion concentration and ion type, are very important in affecting the material structures and mechanical functions,” he says. “Our current result, which shows that carbon dioxide decreases the hydrogen-bond strength at the crack tip, agrees with the findings from our former work but makes an important contribution to the understanding of one of the most critical, and abundant, materials for our planet’s climate – frozen water, or ice.”

Buehler and Qin report their work in Journal of Physics D: Applied Physics. They say that more work is needed to link their microscopic insight to larger-scale properties of ice, glaciers and other geologically relevant structures.

Do you agree with this year's Nobel decision?

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By James Dacey

So another year goes by and we have two new Nobel physics laureates who join the pantheon of scientific idols. Just in case you have been confined in the Utah desert in some kind of Mars-simulation experiment for the past couple of days, this year’s prize went to Serge Haroche and David Wineland for their nifty experimental work on trapping and manipulating quantum systems.

What do you make of the choice? Let us know by visiting our Facebook page and taking part in our poll.

In truth, the decision of the Nobel committee has proved largely uncontroversial in the physics community, with tributes to the pair flying in from all quarters. Among the congratulators was Sir Peter Knight, president of the UK Institute of Physics, who hailed Haroche and Wineland for bringing “tremendous advances in our understanding of quantum entanglement, with beautiful experiments to show how atomic systems can be manipulated to exhibit the most extraordinary coherence properties”.

The only murmuring of a controversy is the suggestion that the Caltech researcher Jeff Kimble was overlooked as a third recipient of the prize. Kimble was one of the pioneers of cavity quantum electrodynamics (CQED) – a technique whereby the properties of an atom are controlled by placing it in an optical or microwave cavity. It was for developing the field of CQED that Haroche won his half of this year’s prize.

Interestingly, there has been no official congratulation from CERN on either its homepage or Twitter feed. Some people, including the editor of physicsworld.com Hamish Johnston, had argued that the confirmed discovery of a new boson at the LHC was enough to secure this year’s Nobel prize. That was also the sentiment of Physics World readers who took part in last week’s poll, with 63% of them selecting the discovery of the Higgs boson as their choice for the prize.

In fairness, though, Wineland and Haroche’s work on quantum optics was not one of the options in our poll. In customary style, the Nobel committee managed to identify a perfectly sensible choice of winner that had not been widely predicted beforehand.

So let us know what you think of this year’s prize by taking part in this week’s poll.

Cornering the Higgs boson

In one sense, the Large Electron–Positron (LEP) collider at CERN could have been considered a failure. Although LEP had cost about a billion Swiss francs (CHF) to build, and even more than that to operate from 1989 to 2000, researchers did not discover a single new elementary particle using it. Sure, they made tremendous refinements of the properties of the massive W and Z bosons – the weak-force-bearing particles that had been discovered at CERN in the early 1980s – as well as precision measurements of other important parameters of the Standard Model of particle physics. But during that 12-year period, only Fermilab could claim a fundamental particle discovery – of the top quark in 1995.

In another sense, however, LEP was a major success. For physicists had excluded a huge range of masses in which any Higgs bosons would have been almost impossible to discover by experiments at proton colliders. A particle that remotely resembled the Higgs boson predicted by the Standard Model should have appeared in electron-positron collisions at LEP had its mass been up to as high as 114 billion electron volts (114 GeV), according to a combined analysis of the four LEP experiments published in 2003 (Phys. Lett. B 565 61). But nothing new had cropped up in this range. And the precision LEP measurements, taken together with the top-quark mass as determined at Fermilab, required that any Standard Model Higgs boson had to show up at a mass below 193 GeV (at a confidence level of 95%). As nobody could have said anything much about its mass before 1989, LEP researchers had thus taken a giant step on the long road to cornering the Higgs boson.

And many physicists on the ALEPH experiment at LEP, which had recorded the most telling candidate events, argued that they had witnessed good evidence for it at 115 GeV. In December 2000 they published a paper entitled “Observation of an excess in the search for the Standard Model Higgs boson at ALEPH” (Phys. Lett. B 495 1), claiming a 3σ excess of Higgs-like events at this energy. But the other three LEP experiments did not confirm these results. Therefore the combined analysis allowed only that such a signal might have occurred – in other words, the signal-plus-background hypothesis fitted all the data better than no signal at all, but not by much. In late 2000 CERN finally shut LEP down after a heated debate and began construction of the Large Hadron Collider (LHC).

Focus on Fermilab

As the new century dawned, physicists at Fermilab could look forward to more than five fruitful years during which they had no competition at all in the Higgs search. It would take at least that long (and as it turned out, much longer) to build and install the LHC in the 27?km LEP tunnel. Boasting a collision energy of almost 2 × 1012 eV (2 TeV), Fermilab’s Tevatron proton–antiproton collider was then the most powerful machine on Earth – and the only one able to generate exotic new particles with masses above 100 GeV. But would it have a sufficiently high collision rate, or luminosity, to create enough of the expectedly rare Higgs events?

A daunting problem with hadron colliders such as the Tevatron or the LHC is that they also produce lots of extraneous debris because protons and antiprotons are not elementary but composite particles made of quarks and gluons. Indeed, Caltech theorist Richard Feynman once compared proton collisions to “smashing garbage cans into garbage cans”. A lot of garbage comes bursting out, some of it looking a lot like the expected decay products of Higgs bosons. At LEP this was not a problem because it collided electrons and positrons, which are essentially point particles with well-understood electromagnetic interactions. Its candidate Higgs events had only two or four tightly packed “jets” of hadrons, corresponding to emerging quarks, and little else. These events could be recognized rather easily.

But at the Tevatron and the LHC, such Higgs-like signals would be swamped by the immense backgrounds of ordinary hadron events. It is not unlike trying to detect a fire-fighter smoking a cigarette in the midst of a forest fire from the two different smoke patterns emitted. If you happen to have a strong, distinctive signal, digging it out from such backgrounds is easier. But if not, experimenters must try to accumulate a tremendous number of events to be certain they can convincingly extract a meaningful signal from the smothering background. And that takes luminosity or time. Or both.

At the lower masses where the Higgs boson was thought most likely to lurk after the LEP shutdown, from 115 GeV to 193 GeV, there was one possible strong, distinctive signal – at just above 155 GeV, where a Standard Model Higgs boson should often decay into an obvious pair of W bosons. Below that it had a bewildering variety of pathways by which to break up. And at masses of less than 135 GeV, it should disintegrate preferentially into pairs of bottom quarks, the next-heaviest link in the great elementary chain of being, as well as gluons and tau leptons. But what these kinds of particles themselves transform into looks much like all the other debris clobbering the detectors. And when an individual W or tau decay involves an easy-to-identify electron or muon, it must also produce a neutrino that exits the detector leaving no track or energy deposit, which makes it more difficult to establish the mass and hence identity of the parent particle. Even if a Higgs boson actually existed at 115 GeV, as the ALEPH experiment had seemed to suggest, it was going to be a long, hard slog to hunt it down amidst such a mess. Finding the Higgs boson at Fermilab was not going to be a piece of cake.

While the Tevatron had plenty of time, it attained insufficient luminosity, especially during the first half a decade. Due to construction and commissioning delays, the LHC experiments did not in fact begin logging data until 2010; the big CDF and D0 experiments at the Tevatron therefore had almost the entire decade all to themselves. A brief flurry of excitement erupted in early 2007 when a group of CDF researchers reportedly observed a small surfeit of events around 160 GeV, disintegrating into tau leptons rather than W bosons. Some interpreted the bump in the graphs of data as evidence of a Higgs boson as predicted by supersymmetric theories, which would decay preferentially in this manner. But interest faded a month later, after the D0 experiment could find nothing similar. And as the data continued trickling in at CDF that year, the intriguing excess withered away – as had so many others.

When the two experiments reported combined results in September 2011, just before the aging, 26-year-old Tevatron was to be shut down forever, there were only small, barely 1σ excesses of Higgs-like events at masses between 115 GeV and 155 GeV – not nearly enough to claim anything significant. Above that level they found too few events decaying via W pairs, so Fermilab could at least take satisfaction in ruling out any Higgs bosons between 156 GeV and 177 GeV. But that was little to show for 10 years of difficult, frustrating research. And it was not enough to convince Fermilab director Pier Oddone to grant the Tevatron a brief stay of execution. As CDF researcher John Conway of the University of California, Davis, lamented, “We’ve gone a very long time with no truly new discovery in particle physics, no observation that truly changes the paradigm.”

Ups and downs at CERN

Fermilab had enjoyed extra time all to itself in the Higgs search due to teething problems at the LHC, the construction of which was delayed by two years because of cost overruns and schedule stretch-outs. In September 2001 CERN director-general Luciano Maiani dropped a bombshell in its council meeting, announcing that the LHC costs were going to grow by almost 20% to CHF 3.34bn, including detector costs. And another CHF 120m would be needed for computing infrastructure. Further cost overruns and delays came later in the decade as a result of problems with the superconducting magnet systems, which had to be cooled with truckloads of liquid helium to just 1.9 K, or –271 ° . When all the expenses were totalled up in 2006, including materials and labour, the final LHC price tag came to about CHF 6bn, more than double its initial advertised cost. Contributions from Canada, China, India, Japan, Russia and the US – the Americans alone having supplied more than half a billion dollars’ worth of equipment – helped ease these financial growing pains. But everything finally seemed to be coming together. On 10 September 2008, with the whole world listening and watching via the BBC, CERN accelerator physicists successfully circulated twin 450 GeV proton beams in both directions through the huge machine without incident. Corks popped. Champagne flowed.

But nine days later, LHC project manager Lyn Evans took a panicky phone call from the control room telling him to come quickly. When he arrived, flashing alarms warned that many magnets had failed and helium gas was filling the tunnel. Later analyses indicated that an electrical splice between two of its 1232 dipole magnets had warmed and “gone normal”, losing superconducting properties. After it melted, an intense spark surged through the magnet vessel, puncturing it and releasing tonnes of helium. When workers later entered the tunnel, they found dozens of magnets damaged, some ripped from their mounts. Soot covered the carnage. Evans called the disaster “a real kick in the teeth for everyone”.

It took more than a year and over CHF 100m to get the LHC back on its feet, and then it was only hobbling. Many splices were found to have additional flaws and would have to be replaced, as did several superconducting dipole magnets. It would be impossible to run the LHC at its design energy of 14 TeV until all the defective splices could be fixed, but that would only happen a few years later. Physicists began to lament that perhaps – after this disaster and the death of the Superconducting Super Collider – God did not want her particle to be discovered, after all.

Cue the collisions

The LHC finally collided protons at 900 GeV on 23 November 2009, with two detectors – ATLAS and CMS – recording the initial events. Four months later, operators gingerly ramped beam energies up to 3.5 TeV, achieving collisions at 7 TeV – but at low intensity. Chastened by the 2008 disaster, researchers became resigned to logging data at only half the original LHC design energy. “It was time to do some physics,” reflected the new director-general Rolf-Dieter Heuer, and making the needed repairs all at once would delay the start of research for at least another year. Wary of a second disaster, CERN accelerator physicists and engineers led by Steve Myers concentrated on improving the collider’s reliability and preparing it for the 2011 run.

The immense, cathedral-sized 7000 tonne ATLAS detector and 12,500 tonne CMS detector had been thoroughly checked out and were ready to begin taking data in their vast underground caverns. It had been a long wait for both 3000-member collaborations – especially the PhD students and postdoctoral researchers, for many of whom this was to be their first experience of a real live particle-physics experiment. These two general-purpose detectors were optimized to be especially sensitive to weighty particles such as a Higgs boson and others expected to occur in supersymmetric theories. They both have excellent energy and momentum resolution (about 1–2%) for electrons, muons and photons. Although a Higgs boson was expected to decay predominantly into pairs of bottom quarks or W bosons, most of which would affect the detectors as jets of hadrons, these decay modes would likely be buried under suffocating backgrounds billions of times larger – and thus nearly impossible to dig out. By concentrating on rare decays in which these leptons or photons appeared, researchers had much better hopes of discerning a signal.

Serious data-taking began in 2011, as operators nudged the luminosity steadily upwards, and proton collisions began rolling in. There were the usual false alarms and overreactions of bloggers, reporters and other scoop chasers who were hovering over the action the entire year. Sau Lan Wu’s group at the University of Wisconsin, for example, circulated an excited internal report in late April of a potential 115 GeV Higgs boson (reminiscent of the final 2000 ALEPH events) decaying into a duo of high-energy photons; it quickly found its way into the blogosphere and went viral, forcing researchers to cancel their Easter vacations to check it out. This “Easter bump”, recalled then CMS spokesperson Guido Tonelli, helped focus his colleagues’ attention on this rare but (soon-to-be) important decay channel. However, the effect proved to be a random fluctuation that withered away in early May after more data came in.

Rumours flew that candidate Higgs boson events might be revealed at the summer 2011 physics conferences. The ATLAS and CMS experiments showed modest excesses of events between 115 and 145 GeV but little else worthy of a press release. CERN could rule out Higgs masses down to 145 GeV and beyond 177 GeV, improving significantly upon the existing Fermilab limits. The Higgs boson was running out of places to hide. If it indeed existed, it now had to be confined to a narrowing range of possible masses between 114 GeV and 145 GeV.

Data deluge

That autumn LHC operators steadily prodded its luminosity to new heights. By the end of the 2011 runs, both experiments had accumulated almost half of what the Fermilab experiments had managed over the previous decade – and at 3.5 times the energy. Events flooded in almost too fast to be recorded. And a small fraction of them looked just as expected for a Higgs boson with a mass close to 125 GeV. In a proton collider such as the LHC, the dominant production mechanism for such a particle is “gluon fusion”, in which gluons in two colliding protons merge to create a Higgs boson, which should quickly break up mainly into two bottom quarks, the most massive final state readily accessible. But that signal would be buried under a huge, burdensome mountain of noise; it is thus very difficult to extract, due to the detectors’ poor energy resolution for hadron jets.

ATLAS and CMS Higgs hunters therefore focused instead on final states with two photons or four charged leptons (electrons or muons), for which they did have good energy resolution and could observe all of the decay products. Although these are rare decay modes, occurring much less than 1% of the time, the narrow peaks that result from plotting such events versus their total energy (or, more accurately, invariant mass) should jut up above the smooth continua of two-photon and four-lepton background events. And that indeed seemed to be the case – especially for the two-photon final state, for which both experiments witnessed more than 70 excess events near 125 GeV. In addition, ATLAS physicists unearthed a few extra four-lepton events at the same energy, while CMS found a similar surfeit near 120 GeV. Something new and Higgs-like was happening in this vicinity.

CERN went cautiously public with these preliminary results in a dual seminar on 13 December 2011, viewed on webcast by thousands of particle physicists and science reporters around the globe. Expectations were high, as rumours of a discovery had been percolating for over a week. But nobody (except some in the press) claimed a discovery. “We have restricted the most likely mass region for the Higgs boson to 116–130 GeV, and over the last few weeks we have started to see an intriguing excess around 125 GeV,” noted ATLAS spokesperson Fabiola Gianotti. Tonelli agreed with her assessment, admitting that CMS physicists “cannot exclude the presence of the Standard Model Higgs between 115 and 127 GeV because of a modest excess of events in this mass region”.

What was new and strikingly different this time was how ATLAS and CMS corroborated one another, revealing intriguing peaks beginning to emerge near 125 GeV. In addition, the CMS experiment had found Higgs-like events in a few other decay modes at about the expected rates. When the combined analyses of these two experiments were published the following February, both the ATLAS and CMS experiments claimed to be observing better than 3σ effects near 125 GeV. But after further data analysis, the statistical significance fell below that level in results presented at the March 2012 Moriond Conference in La Thuile, Italy, considered the principal winter gathering for particle physics. And when the “look-elsewhere effect” (see Physics World August p26) was included, the significance dropped to just above 2σ. These were not yet robust results.

Down but not out, CDF and D0 physicists – many of whom also worked in the ATLAS and CMS experiments – were preparing their comeback. Using sophisticated techniques, they reanalysed both of their full data sets, struggling to wring out every possible Higgs boson event. The Tevatron should have been particularly effective at generating “associated production” events in which a quark within a proton merges with an antiquark from a colliding antiproton to yield a W or Z particle plus a Higgs boson. CDF and D0 physicists sought events in which the W or Z decayed into an easily identified lepton pair and the Higgs boson into two bottom-quark jets; in such events they had much better chances of discerning a Higgs-like signal from noise. And indeed, they succeeded.

At the Moriond conference, both Tevatron experiments revealed new data with broad bumps between 110 GeV and 140 GeV. Combined into a single result, the CDF and D0 data had a bulging 2.2σ excess between 115 GeV and 135 GeV (figure 1), much as expected for a 125 GeV Higgs boson disintegrating into bottom quarks; but the events were spread out over a much wider mass range as a result of the detectors’ poor energy resolution for hadron jets. These Fermilab data clearly reinforced the 2011 CERN results.

Endgame in sight

It looked like the elusive Higgs boson had finally been cornered. While none of the individual results was convincing by itself, four separate experiments had witnessed intriguing excesses in the vicinity of 125 GeV. And the decays of whatever it might turn out to be accorded pretty well with the Standard Model prescriptions for a Higgs boson (but at only moderate significance). Moreover, the indirect limits on such a particle based on precision measurements had long suggested that a lower-mass Higgs boson should in fact exist.

Some theorists were already convinced it had indeed been discovered. “I’m willing to bet a year’s salary!” exclaimed Nima Arkani-Hamed of the Institute for Advanced Study in Princeton, New Jersey, in a panel discussion in March. Gordon Kane, a co-author of the 1990s classic book, The Higgs Hunter’s Guide, thought so, too. “When you have four independent signals, they almost never go away,” he argued at a press conference in April, suggesting that one could get a 5σ result just by combining all the data from the four experiments. But Kane had an obvious theoretical axe to hone, too, having co-authored a paper the previous December, only days before the CERN seminar, predicting a 122–129 GeV Higgs boson based on considerations of supersymmetry and string theory.

Cautious experimenters, wary of getting too far ahead of the data, however suggested everybody take a deep breath and sit tight until after this year’s LHC runs, which began in April with protons colliding at 8 TeV and machine operators aiming to double the luminosity. By the end of 2012, predicted CERN officials, ATLAS and CMS physicists should have the final answer – and be able to put an end to Peter Higgs’ long, long wait.

And his wait turned out to be shorter, as the official discovery of a Higgs-like particle near 125 GeV was announced on 4 July (see “CERN discovers Higgs-like boson”). The decades-long search for a Higgs boson was finally over.

Neil Turok looks forward to living a quantum life

Neil Turok


An analogue Neil Turok dreams of a quantum life. (Courtesy: Perimeter Institute)

By Hamish Johnston

Years ago when I lived in Canada I used to love listening to a CBC radio programme called Ideas, which devotes one hour to the in-depth discussion of a concept, event or idea. Incredibly, there are five episodes a week and the show has been running for 47 years – and still hasn’t run out of ideas!

Recently, the programme’s host Paul Kennedy was at the Perimeter Institute for Theoretical Physics in Waterloo, Ontario to chat with its director, the mathematical physicist Neil Turok.

Turok has just written a book called The Universe Within: From Quantum to Cosmos, which is based on his series of Massey Lectures that form part of the Ideas schedule (if you are in the UK, think Reith Lectures).

You can watch Kennedy and Turok talk about the book here – and find out why he thinks we can look forward to living a quantum life.

And stay tuned for a review of The Universe Within in our upcoming Christmas books special.

A Casimir force for life

The Casimir effect is perhaps best known as a quantum phenomenon, in which vacuum fluctuations can give rise to an attractive force between two parallel mirrors. But there is also a thermodynamic equivalent, caused by fluctuations in the composition of a fluid close to its critical point. New research by physicists in the US suggests that these “critical Casimir” forces act on the proteins inside cellular membranes, allowing proteins to communicate with one another and stimulating cells’ responses to allergens such as pollen.

All cells are surrounded by a membrane that controls the flow of substances into and out of the organism. Membranes are made up of molecules called lipids within which proteins are embedded. They were once thought to be essentially uniform, but a number of experiments starting in the 1970s and 1980s indicated that the lipids in fact cluster to form distinct structures tens or hundreds of times larger than the lipid molecules themselves. Scientists did not understand, however, where the energy needed to maintain such structures came from.

In 2008 biophysicist Sarah Veatch at Cornell University in upstate New York and colleagues found a solution. It was known that above 25 °C membranes isolated from live mammal cells exist in a single liquid phase, whereas below that temperature they separate out into two distinct phases, composed of different kinds of lipids and proteins – a bit like oil and water refusing to mix when brought together. What Veatch’s group discovered was that as they lowered the temperature of the membranes close to that at which the phases separate out, known as the critical point, small fluctuating patches of the second phase started to appear. Such fluctuations – which measured several microns across and were visible in an optical microscope – do not require large amounts of energy to form.

Critical look at criticality

Veatch has since moved to the University of Michigan but for the current research teamed up with two physicists back at Cornell, Benjamin Machta and James Sethna, to understand the purpose of this criticality. The researchers reckoned that certain kinds of proteins are attracted to one of the phases while other kinds are attracted to the second phase, so tending to draw like proteins together and separate out unlike proteins. As Veatch explains, these interacting proteins would form “signalling cascades” to transmit information regarding the identity of compounds in a cell’s vicinity from receptor proteins in the membrane to the inside of the cell. Such information could be used, for example, to decide whether it is a good time to divide or whether it is safe to crawl towards food. “We think that one reason cell membranes contain critical fluctuations is to help facilitate some of the early steps in these signalling pathways,” she says.

To calculate the strength and form of the Casimir forces between proteins, Machta used mathematics developed originally for string theory. He found that, as expected, the forces are attractive for like proteins and repulsive for unlike ones, and that they yield a potential energy several times that of the proteins’ thermal energy, over distances of tens of nanometres. Much stronger electrostatic interactions, he explains, are limited to ranges of about a nanometre by the screening effects of ions inside the cell. “We have found that by tuning close to criticality, cells have arranged for a long-ranged force to act between proteins,” he says.

Sethna adds a broader perspective. “It is amazing how many reactions in cells all involve energies of the same size as thermal fluctuations,” he says. “We think that it is the cell being economical – why pay more?”

Something to sneeze at

The researchers suspect that the existence of these critical Casimir forces explains why cells low on cholesterol do not function as they should – the removal of the cholesterol, they reckon, taking the membrane away from its critical point. They also speculate that the forces are involved in the sneezing process. Sethna explains that when the receptor proteins in immune cells detect an allergen such as pollen they cluster together, and this clustering somehow triggers the histamines that cause sneezing. He says that perhaps an allergen simply changes the preference of the receptor proteins for one of the two liquid phases in the membrane, hence drawing them together.

The team is hopeful that its work could lead to medical applications. Veatch explains that defects in lipids are thought to contribute to a large number of diseases, including cancer, auto-immunity diseases, and inflammation. “This work may shed light on how lipids could impact some aspects of these diseases,” she says. “In the future, I can imagine drugs that specifically target lipids to regulate interactions between proteins in order to treat human disease.”

Sethna adds, however, that the time scale for such applications is likely to be long. “Our work is more like figuring out how to make better concrete to build the subbasement of the skyscraper that eventually would house the penthouse of health applications,” he says.

Theory explains behaviour

But in addition to any future applications, Sethna argues that the existence of criticality within cells lessens the reliance on purely evolutionary mechanisms when trying to understand how cells operate. “There are lots of things about cells that biologists assume happen because ‘evolution made it so’,” he says. “Here, I guess, evolution allowed the cell to find this critical point. But once the cell is at the critical point, we can use systematic, cool theory to explain lots of the behaviour, without repeatedly accounting for everything using evolution.”

However, some independent experts feel that Veatch’s experimental results must be treated with caution because they were not obtained using intact cells. One, who asked to remain anonymous, argues that the separation of the membrane from the rest of the cell might have removed certain relevant components from the membrane and that the body of the cell itself might influence the critical fluctuations in some way. “I am not yet convinced that the theory presented is applicable to in vivo biological membranes,” he says. “I therefore think that much more experimental work has to be done to investigate this phenomenon.”

The research is described in Physical Review Letters.

Keeping ahead: a look at physics in Japan

With a string of new high-profile international research facilities, Japan is maintaining its world-leading status in physics and astronomy. Yet there remain both challenges and opportunities for physicists from abroad to go and work in Japan or to collaborate with Japanese researchers.

In this lecture, Adarsh Sandhu, who has worked in the country for more than 25 years, gives his personal take on physics in Japan.

Date: Wednesday 10 October 2012

Speaker: Adarsh Sandhu, Toyohashi University of Technology, Japan
Professor Adarsh Sandhu has been a faculty member of the Quantum Nanoelectronics Research Centre at Tokyo Institute of Technology since 2002, and director of research at the Advanced Interdisciplinary Electronics Research Institute, Toyohashi University of Technology since April 2010. His research activities include scanning Hall probe microscopy and the development of biosensors based on magnetic labels for rapid medical diagnosis. He is also a visiting professor at Tsinghua University in Beijing and IIT Delhi.

Moderator: Dr Michael Banks, news editor, Physics World

Free access to Nobel winners' papers

Serge Haroche's cat states


The time evolution of a Schrödinger’s cat state realized by Serge Haroche and colleagues.

By Hamish Johnston

To celebrate the 2012 Nobel Prize for Physics, IOP Publishing has collected 30 papers published in its journals by winners Serge Haroche and David Wineland. Articles in this collection are free to read until the end of February 2013.

The above image is taken from a paper by Haroche and colleagues entitled “Manipulating and probing microwave fields in a cavity by quantum non-demolition photon counting” (Phys. Scr. T137 014014). You can read it here.

Quantum-control pioneers bag 2012 Nobel Prize for Physics

The 2012 Nobel Prize for Physics has been awarded to Serge Haroche and David Wineland for their work on controlling quantum systems. The prize is worth SEK 8m (£750,000) and will be shared by the pair, who will receive their medals at a ceremony in Stockholm on 10 December.

According to the prize citation, Haroche and Wineland won “for ground-breaking experimental methods that enable measuring and manipulation of individual quantum systems”.

Haroche is a French citizen and works at Collège de France in Paris. Wineland is a US citizen and works at the National Institute of Standards and Technology in Boulder, Colorado.

In a statement, the Royal Swedish Academy of Sciences said “Serge Haroche and David Wineland have independently invented and developed methods for measuring and manipulating individual particles while preserving their quantum-mechanical nature, in ways that were previously thought unattainable”.

According to Nobel committee member Anne L’Huillier, the pair’s work represents “the first tiny steps towards building a quantum computer”.

Quantum-optics pioneer Alain Aspect of Laboratoire Charles Fabry in Paris told physicsworld.com “Observing, manipulating and controlling individual quantum systems has been a major breakthrough of the last few decades. Schrödinger doubted that it might ever be possible, but this year’s laureates have done it.”

CQED pioneer

Haroche was born 1944 in Casablanca, Morocco, and in 1971 gained a PhD from Université Pierre et Marie Curie in Paris. He shares half of the prize for developing a new field called cavity quantum electrodynamics (CQED) – whereby the properties of an atom are controlled by placing it in an optical or microwave cavity. Haroche focused on microwave experiments and turned the technique on its head – using CQED to control the properties of individual photons.

In a series of ground-breaking experiments, Haroche used CQED to realize Schrödinger’s famous cat experiment in which a system is in a superposition of two very different quantum states until a measurement is made on the system. Such states are extremely fragile, and the techniques developed to create and measure CQED states are now being applied to the development of quantum computers.

Had to sit down

In a telephone interview with Swedish journalists shortly after the announcement was made, Haroche said that he knew that he had won the prize when his mobile phone rang this morning as he was out walking and a Swedish number was on the display. “I sat down on a bench before I answered,” he said. Although Haroche knew that he was in the running for the prize, he was overwhelmed upon hearing the news. He said that he will enjoy a glass of champagne at lunch with family and friends then “go back to the office to celebrate with colleagues”.

Haroche also said that he was “glad to share the prize with Dave Wineland – he is a fantastic physicist and to be in his company is certainly a great pleasure for me and a great recognition”.

Wineland returned the compliment by saying, “[Haroche] and I have been friends for a long time, so it’s nice to share it with him”.

Master of ion control

David Wineland was born in 1944 in Milwaukee, Wisconsin, and received his PhD in 1970 from Harvard University. As well as being Group Leader and NIST Fellow at the National Institute of Standards and Technology, he also has an appointment with the University of Colorado at Boulder.

Wineland bagged his half of the Nobel for his ground-breaking work on the quantum control of ions. One of his many achievements was the creation and transfer of a single ion in a Schrödinger’s cat state using trapping techniques developed at NIST. Ion traps are created in ultrahigh vacuum using carefully controlled electric fields and a trap can hold just one ion or several in a row.

Ions vibrate as they are held in a trap, and this vibrational energy must be removed in order to cool the ion to its lowest energy state. To achieve this cooling, Wineland developed a laser-based technique to remove quanta of vibrational energy from ions. This “sideband” technique of cooling can also be used to put an ion into a superposition of states – including a Schrödinger’s cat state.

Wineland has also used ion-control techniques to develop extremely accurate optical clocks, as well as circuits for quantum computers.

Groundwork for quantum information

Rainer Blatt of the University of Innsbruck in Austria does experiments in both CQED and ion trapping, and he told physicsworld.com that the Nobel committee chose well in awarding the prize to Haroche and Wineland. Blatt points out that the pair developed similar quantum-control techniques for use on different physical systems – techniques that have laid the groundwork for many of today’s nascent quantum-information systems.

Blatt cites Wineland’s 2008 development of “quantum-logic spectroscopy” – which allows a single ion to be used as an optical clock – as an important application of the control techniques, along with the creation in 2009 of a small-scale device that performs all the functions required in large-scale ion-based quantum processing.

Haroche’s work provides a framework for controlling the interaction between a single atom and a single photon – something that Blatt says is currently being used to develop ways of exchanging quantum information between atoms and photons. This could allow physicists to create quantum computers in which data are stored in stationary quantum bits (qubits) based on atoms, which are relatively stable over long periods of time. Data could then be transmitted between atoms using photons, which can preserve their quantum information while travelling relatively large distances.

The hue of alien Earths

An international team of researchers claims that the link between the colour of a planet and its surface features can be used to prioritize which newly found exoplanets, especially rocky planets with clear atmospheres, should be studied in-depth for signs of life. The work provides an important link between Earth-based geomicrobiology and observational astronomy.

A huge number of exoplanets have been discovered in recent times – just over 800 confirmed examples are known today, with more than 2000 candidates waiting to be confirmed. Of the candidate exoplanets, it is difficult to decide which ones are the most likely to harbour life.

Home sweet home?

“What is now observed is that smaller Neptune-sized planets are, in fact, far more abundant than larger Jupiter-sized ones. This is exciting and one feels that it is only a matter of time before the same can be said for Earth-sized planets around other stars. The question then naturally arises as to how one could characterize these rocky planets to check for their potentially habitability,” explains Siddharth Hegde of the Max Planck Institute for Astronomy in Germany. He and colleague Lisa Kaltenegger from the Harvard-Smithsonian Center for Astrophysics in Cambridge, Massachusetts, in the US have explored how filter photometry can be used to pinpoint Earth-like exoplanets and study their atmospheric bio-signatures – whether they have aerobic or anaerobic atmospheres. Looking at the diversity of life on Earth, even under extreme conditions, the researchers wonder whether planets around other stars with extreme surroundings could also harbour some form of life.

In astronomy, photometry is a way of measuring the flux of the electromagnetic radiation of an astronomical object. “Filter photometry basically means that you split the collected light [from a celestial object] only into a few wavelength bins that are defined here by the commonly used filters in the visible called ‘B, V, I Johnson–Cousins filters’ [or blue, green and red colour bins],” explains Hegde. The advantage of this approach is that lots of photons are gathered per bin, meaning a good signal-to-noise ratio is achieved – which, in turn, means that it may be possible to characterize dimmer planets. The researchers use this method to identify planets that have surfaces similar to those on Earth that harbour life. This is done by plotting the blue–green versus blue–red bins using customized filters, creating what is known as a “colour–colour diagram”. While the technique does not provide the finer details of a planet, it can very easily be used to put together a follow-up prioritized “target list” of planets that should be studied in detail with spectroscopy.

True colours

A way of looking for these extreme environments is to study the “albedo” of a planet – its reflectivity as a function of wavelength. For example, snow has a high albedo, meaning that it reflects well, while water has a low albedo and so does not reflect as well. A previous study, conducted in 2003, compared the colour–colour diagrams of rocky and Jupiter-like planets in our solar system to see whether they were the same – they were not. That study concluded that a colour–colour diagram can be used to make a first-order basic characterization of a planet’s nature. Hegde and Kaltenegger extended this idea to rocky exoplanets based on the assumption that these habitats best determine the environmental limits for harbouring Earth-type extremophiles.

Going to extremes

An extremophile is an organism that exists in physically or geochemically extreme conditions – such as extreme temperature, radiation, pressure, dryness, salinity or pH – that are detrimental to most other life-forms on Earth. “By splitting the light from a hypothetical planet, with a surface covered with a material that can harbour extremophiles on Earth, into the three filter bins, we found that those planets fall into a tight band when plotting a colour–colour diagram,” says Hegde.

The method is similar to another already used by exoplanet hunters who look for the “red-edge” – a telltale sign of vegetation – in the spectra of planets. This is a large and abrupt change in the absorption of light by plants that occurs at about 700 nm. At shorter wavelengths, chlorophyll absorbs very strongly and therefore plants reflect little light; above 700 nm, chlorophyll does not absorb light, which means that leaves are able to reflect much more sunlight back into space. Combining such spectral readings with colour–colour diagrams could clearly indicate if a planet has any Earth-like life, or is capable of harbouring it.

In the future, the researchers are keen to study possible changes in a planet’s atmosphere caused by different kinds of extremophiles that might inhabit its surface – for the moment, their model assumes the extremophiles do not affect the atmosphere significantly. “Maybe, with the help of biologists who culture such extremophiles in the lab, we can find out if there are gases in the atmosphere that can tell us whether such surfaces really harbour life,” muses Hegde.

A paper on the work is available on the arXiv preprint server.

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