Students find cosmic rays in DC museum

May 4, 2010 | 5:13 pm

How cosmic rays collide with the Earth's atmosphere. Courtesy CERN.

How cosmic rays collide with the Earth's atmosphere. Courtesy CERN.

If you happen to be in the Washington, DC, area today, stop in at the Smithsonian’s Air and Space Museum to see cosmic rays in action in honor of National Lab Day.

Four teams of high school students and their teachers will display classroom cosmic ray detectors set up throughout the museum’s Milestones of Flight Gallery. The detectors will  record the particle remnants of the sun’s energy that collide with the Earth’s atmosphere and send secondary particle showers raining down through the roof. In fact, about a hundred of these secondary particles will pass through the bodies of museum visitors every second.

Visitors will get to learn about these cosmic rays, detectors, and the particle physics behind them from the students and a team of physicists from Fermilab and the QuarkNet education outreach program based at the Illinois laboratory.

“We wouldn’t teach football from a textbook,” says John Holdren, President Obama’s science advisor in a press release announcing National Lab Day. “It is even more important that America’s youth have the opportunity to learn math and science by doing. The President and I strongly support efforts to raise the level of project-based learning, to help cultivate the next generation of doers and makers.”

National Lab Day, being celebrated in many places this week, focuses on the need to improve science, technology, engineering, and math skills in middle and high school students as well as connect students with professionals in those fields.

QuarkNet’s unique ability to partner students and teachers with ongoing research at national laboratories provides just that type of real-world experience that developers of National Lab Day say is needed to reinvigorate science education and foster future increased US competitiveness.

The particle collision data collected  in the Smithsonian by the teens from Illinois, Ohio, Maryland, and Virginia will complement data from 311 other cosmic ray detectors operated by high school students across the country. QuarkNet staff design and produce the sophisticated detectors, which students assemble and operate themselves.

The simultaneous two-days of data taking, May 4 and 5, will supplement the 2700 days of data already available for study and query in the public  Cosmic Ray e-Lab operated by QuarkNet.

Teachers can tap into the e-Lab to formulate individualized lessons plans to teach about particle physics and working in national and international collaborations. More than 1200 teachers have taken advantage of the QuarkNet program since 1999.

“It’s their data. It is not being handed to them by anyone, “ says Robert Peterson, QuarkNet education program leader. “They go out and do the experiments.”

The size of the Smithsonian gallery will enable students to locate detectors 100 feet apart from one another, creating a wide enough umbrella to look for cosmic ray showers and compare that analysis to the real-world research on cosmic rays being done by the Pierre Auger Observatory in Argentina.

“Our children deserve a world class science and math education that includes exciting, hands-on lab experiences,” says Jack Hidary, chairman of National Lab Day. “Whether you are a Nobel-prize winning scientist, a Mythbusters fan, a tinkerer, or a parent, you can help bring students the enjoyment of learning through real challenges.”

Tona Kunz

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Peer-reviewed physics at the speed of light

April 30, 2010 | 6:01 am

In the April issue of symmetry, Daisy Yuhas writes about the long path from the first hint of a discovery at the Large Hadron Collider to the published paper that makes the claim official.  Yet in the four weeks since the LHC’s first collision, four papers have already been published and 15 more are in the pipeline.  In this interview with Sergio Bertolucci, the head of research and computing at CERN, Dan Drollette of iSGTW, International Science Grid This Week, sorts things out.  This article is reprinted from their April 28 issue.


Sergio Bertolucci. Photo: CERN

Director for Research and Scientific Computing at CERN, Sergio Bertolucci. Photo: CERN

iSGTW: We have heard that a lot of papers have already been published in the time since the start-up of the LHC. Is that right?

Bertolucci: Four papers on high-energy physics have already published, and 15 are in preparation as of today, April 14, all based on the collisions that just happened. One week after the first collisions, the first papers were published electronically. And these were all peer-reviewed. 

iSGTW: That’s very fast, compared to the sometimes years-long process of traditional print journals. How was the peer-review done?

Bertolucci: Each experiment is not a monolith, but consists of 3,000 people working in teams on separate projects within it. When a paper is about to be produced, it passes through different teams for internal review, then is reviewed by teams on other experiments, then reviewed by CERN. So, there have been five layers of review before it even goes to the external publication, which has its own, independent review system. The whole system sounds complex, but nonetheless is fast, as seen by one week between observation and publication.

iSGTW: Where have these papers appeared?

Bertolucci: Open-access journals, such as the Journal of High Energy Physics. Our paradigm has always been open access, and this is a good place to practice it.

iSGTW: What was the content of what was published?

Bertolucci: For one thing, the number of charged particles per unit angle at different energies in the LHC was much higher than predicted. It did not conform to the model.

iSGTW: Why is this important?

Bertolucci: This is new knowledge, which may be leading to new physics. And on a more immediate, pragmatic level, the material in these papers is important for tuning and for simulation.

iSGTW: Why publish so fast?

Bertolucci: The watchwords of science are collaboration and competition. Everyone wants to work together, but there’s also a sense  of healthy competition — everyone wants to be first.  Everyone wants to be the first to say “I found it.” And that’s good — it keeps people on their toes.  At the same time, there is collaboration, which benefits from publishing quickly. We can compare and contrast what is happening between experiments, for example. So, ATLAS and CMS can exchange information, look at each other and confirm that they are each on the right track. So far, the results nicely fit, and publishing quickly really helps make that happen. And the technology is pushing for fast publication as well. We have the capability to do it, so why not take advantage of it.?

iSGTW: Obviously, it’s still early, but would you care to make any speculations about what the LHC will find, and what kinds of papers we will see?

Bertolucci: It depends on how kind nature  is to us. But at the level at which we’re operating — 7 TeV — if supersymmetry is there, we’ll find it. The Standard Model predicts that at 800 GeV, evidence of it should start to show up. And at this 7 TeV energy level, we should pick up any hints for B-Mesons as well. What’s more, all this is just the known unknowns — that’s not counting the ‘unknown unknowns.’

iSGTW: Any last comments you would like to make?

Bertolucci: This is a very long-term project. The LHC will be around for a while, and there will be a lot of papers coming out of it. I was there when the Tevatron in Illinois first started up in 1985 — and that machine is still going strong today. So, the LHC ought to be around for several decades as well.

This is a very good time to be in the high-energy physics community. This kind of global collaboration means we can do things which would otherwise be impossible; each individual project would otherwise not have the resources, the staff or the funding to undertake these endeavors.

The kind of global collaboration that we are doing here in this community could hopefully someday become a model for others to follow. Where else do you find people from Palestine and Israel, Pakistan and India, or America and Iran working side-by-side ?

by Dan Drollette, iSGTW

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Opinion: An African computing grid?

April 29, 2010 | 11:06 am

At the EGEE User Forum in Uppsala, the author, Bruce Becker of the Meraka Institute and coordinator of the South African National Grid, called for making an AfricaGrid a reality. Here he outlines the reasons why now is the opportune time for work on this to be starting in earnest.

Official ribbon-cutting for “Blue Gene for Africa” last year. This supercomputer is the fastest scientific computer on the African continent, capable of 11.5 teraflops (11.5 trillion floating point operations per second). Image courtesy Center for High-Performance Computing

Official ribbon-cutting for “Blue Gene for Africa” last year. This supercomputer is the fastest scientific computer on the African continent, capable of 11.5 teraflops (11.5 trillion floating point operations per second). Image courtesy Center for High-Performance Computing

For some years now, many have been hinting at an “AfricaGrid.”

In the Mediterranean basin, we have seen many African countries participating directly in EUMedGrid (and more recently EUMedSupport).

In the southern region of Africa, we have seen much activity over the last couple of years that allows to envisage at least a “Sub-Saharan Grid.”

This prospect is very appealing to the researchers in our region, not least for the benefits of collaboration and openness that it can bring. It is appealing as well, to those involved in the deployment of research infrastructure, especially e-Infrastructure, who would see these large investments efficiently and effectively used.

Many fundamental aspects of the organizational landscape which are needed to embark on such a regional project were not in place until recently — not least the networking. However, we have seen some major changes in the networking and e-Science landscape in South Africa and in the wider region, which is starting to signal that we are approaching a credible goal. Apart from the various projects aimed at studying the state of the art and making concrete recommendations, we have a reassuring list of achievements in place so far, including HPC site deployment, inter-site networking, scientific collaborations, technical training, dissemination at all levels, etc.

Current and proposed projects focusing on e-Infrastructure development in the region (South Africa’s Cyberinfrastructure program, EPIKH project, proposed CHAIN project, EUMed Support, HP-UNESCO Brain Gain, UbuntuNet Alliance, EUMEDCONNECT2, FEAST, and so on) are crucial. Adding to this the experience of similar activities in Latin America (EELA, EELA-2) and India, (EUIndiaGrid) — not to mention regional and international projects in the EU with which we already have strong technical and scientific collaborations — and we see that we have the expertise, confidence and experience to construct something fairly rapidly which could change the lives of researchers in the region.

Seacom, the 15,000 kilometer-long undersea fiber-optic cable that links East Africa to Europe and south Asia, made landfall in Kenya in the summer of 2009. Image courtesy SEACOM

Seacom, the 15,000 kilometer-long undersea fiber-optic cable that links East Africa to Europe and south Asia, made landfall in Kenya in the summer of 2009. Image courtesy SEACOM

A sub-Saharan EUMedGrid?

In South Africa, universities and national laboratories have agreed to form a Joint Research Unit, and support the development of this infrastructure, encouraged by the national cyberinfrastructure initiative

With the combined experience and support of EGEE and partner projects, (notably INFN Grid and IGI as well as CNRS and IdG), including the crucial training and dissemination services provided by GILDA, we have been able to reach production-level services in just over a year. Work is now starting in earnest in developing user communities to exploit the services provided, in close collaboration with over 20 institutes all over Africa through the HP-UNESCO project.

The SANReN and SEACOM fiber optic lines have or will soon enable services which we could only envy in other parts of the world. The experience in South Africa is thus of direct relevance to the region, where our prototype and evolution to full production service will serve as a blueprint for other countries, easing their work and providing guidance and trusted partners.

With this in mind, I would like to call for the formation of a regional task force for e-Infrastructure deployment, in order to bring this long line of development and study to a point where it is on a par with the rest of the world. This is of course not a new idea and I by no means take credit for it — I would like to acknowledge the efforts by everyone, and stress that my call is an open one.

I would like know whether readers would endorse such a task force and whether you could take some role in it. This would allow us to tackle the myriad of simultaneous issues which need to be addressed while coordinating them towards the goal of a federal, fully interoperable regional infrastructure. I believe that this also has the potential to evolve into the sub-saharan version of, say, EUMedGrid, if we take the collective responsibility of defining our region’s way forward.

by Bruce Becker, Meraka Institute – Coordinator, South African National Grid

You can see Bruce Becker’s personal thoughts on what this means for the ‘Fifth Freedom’ (the removal of barriers to the free movement of ideas and knowledge) at his blogpost on GridCast.

This story first appeared in International Science Grid This Week.

You can read more about physics in Africa in this issue’s commentary in symmetry.

Guest author

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April 2010 issue of symmetry now online

April 28, 2010 | 12:38 pm

hp-photo-cover April 10

In this issue:

Jobs go begging in accelerator science

– The slow, careful path to discovery at the Large Hadron Collider — aptly titled “Are we there yet?”

– A science-fiction story written especially for SLAC by John Gilbey, featuring an interview with the author.

Plus: A new school of physics in Africa; the now-you-see-it, now-you-don’t quantum art of Julian Voss-Andreae; a little-known product of particle accelerators that lives inside your house, your office and your car;  a giddy fan collects physics autographs; the neutrino explained in 60 seconds; and more.

A pdf of the issue is available for download here.

As always, we love to hear from readers.  Send us your thoughts at letters@symmetrymagazine.org or use the handy links at the bottom of each article.

Glennda Chui

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Protons not as “strange” as expected

April 27, 2010 | 5:29 am

This ferris wheel is part of a system that helped determine just how strange the ordinary stuff around us can be. In the G-Zero experiment, researchers carried out a precisely tuned survey for ephemeral particles that appear only briefly inside matter.

This ferris wheel is part of a system that helped determine just how strange the ordinary stuff around us can be. In the G-Zero experiment, researchers carried out a precisely tuned survey for ephemeral particles that appear only briefly inside matter.

It’s been said that anything worth doing takes time – just ask those scientists involved in what’s known as the G-Zero experiment. Nearly two decades ago, an international coterie of more than 100 scientists came together with the goal of pinpointing just how strange the ordinary stuff around us can be. The G-Zero collaboration proposed a precisely tuned survey for ephemeral particles that appear only briefly inside matter. Specifically, they wanted to measure the effect of strange particles in the proton, the sub-atomic particle found deep inside the nucleus of every atom in our universe.

It was a massive undertaking. The full experiment would take more than 15 years to accomplish, with tons of new equipment and exclusive use of one third of Jefferson Lab’s experimental space for over two years. In addition, it would benefit from the assistance of nearly 50 undergraduates, graduate students and postdoctoral researchers and hundreds of support personnel.

Now, the G-Zero experiment is publishing the first of several of papers detailing its final conclusions. Its findings were published in the January 8 issue of Physical Review Letters.

Peeking Into the Proton

It took humankind a full two thousand years from the first recorded suggestion of the atom’s existence until one would actually be pried apart for a glimpse inside. Democritus, a Greek philosopher in the third century B.C., spoke of the “a-tom” as the smallest component of matter, from the Greek meaning “cannot be split.”

What we now think of as the atom – consisting of a nucleus and its electrons – was first described by John Dalton in the early 1800s. Later that century, scientists found that they could strip electrons out of the atom. Then, in the early twentieth century, they found that the nucleus contained even heavier particles, which were dubbed protons and neutrons.

Fast forward to the 1960s, when theoretical physicists proposed that protons and neutrons have building blocks of their own – particles called quarks. Shortly thereafter, researchers at SLAC National Accelerator Laboratory conducted experiments that demonstrated that quarks really did exist.

Decades of research have confirmed that a proton contains three permanent quarks. But that’s not all. There is also the force that binds the quarks together to make a proton. This “strong force” binding the quarks is an integral part of the structure of the proton.

A Hotbed of Activity

“Protons and neutrons are very unusual objects,” says Doug Beck, a professor at the University of Illinois at Urbana-Champaign and spokesman for the G-Zero collaboration. “Their matter constituents, the three quarks, account for so little of their overall mass. Most of their mass is actually energy: the energy of the fields generated by the strongly interacting quarks and the energy of motion of the quarks themselves.”

The G-Zero researchers were particularly interested in these strong force energy fields. The energy from these fields appears in the form of particles inside the proton called “sea particles.” These particles bubble up for the briefest of moments before melting back into energy fields.

The sea particles, also called virtual particles, can take the form of quark pairs. Pairs of up quarks and pairs of down quarks are the most likely pairs to appear briefly in this sea, because they are the lightest of quarks. The proton’s permanent quarks consist of two up quarks and a down quark.

The next-heaviest quarks, strange quarks, are also thought to be present in the sea as virtual particles. G-Zero scientists proposed their experiment in 1993 to measure what effect these temporary residents of the proton have deep inside the proton.

“In the paper, we report what we have seen of the virtual quarks spawned by the energy fields,” Beck asserts.

 The G-Zero custom detector system (left) is installed and ready to run in Jefferson Lab's Hall C.

The G-Zero custom detector system (left) is installed and ready to run in Jefferson Lab's Hall C.

Proton Knockouts

The proton is not a rigid object that can be laid out on a lab table to be weighed, observed and otherwise poked and prodded. If you were somehow able to isolate a proton and plop it onto a slide under a light microscope, you still wouldn’t be able to see it. The visible light that bounces off ordinary small objects and into the microscope lens and your eye would simply pass by the proton.

To “see” the proton, scientists need a different kind of probe. At Jefferson Lab, electrons are used instead of visible light. An electron is small enough to interact with the proton. A properly prepared electron can bounce off of the proton, knock it about or blow it apart.

Jefferson Lab prepares electrons for experiments using the Continuous Electron Beam Accelerator Facility, or CEBAF, accelerator. In the accelerator, electrons that have been freed of their atoms are pumped up to high energy. They are then sent into one of CEBAF’s experimental halls and into a target material. There, the electrons may interact with the protons inside the target.

With a little energy, an electron bounces off a proton. Add a bit more energy, and the electron knocks a proton out of the nucleus in which it resides. In G-Zero, scientists were interested in bouncing electrons off the nuclei of hydrogen atoms. Two types of hydrogen were used – ordinary hydrogen, the simplest nucleus consisting of a single proton, and deuterium, which has both a proton and a neutron.

In particular, the G-Zero scientists wanted to measure the protons that came flying out of the target or the electrons that succeeded in bouncing off the protons and neutrons. The particles were intercepted by detector systems that recorded their flight path. A flight path of a proton or electron can either directly or ultimately provide information about the protons that were knocked out.

Describing the Proton’s Properties

Probing the proton with electrons isn’t going to provide the same information that you’d get by looking at something with a grade-school microscope. The proton is too small to have a visible color, nor can it be described by how rough or smooth its surface appears or how squishy or solid it feels.

Instead, physicists have a different set of properties they can measure. For instance, the proton has an electric charge. The quarks inside the proton each have an electric charge, which gives the proton its overall positive charge.

By scattering electrons from the proton, physicists can tell how much of the total charge participates. That allows them to peer inside the proton to see variations of charge inside the proton – its so-called charge distribution. The distribution of electric charge gives physicists a handle on where the quarks are in the proton.

“And so a proton is not an object that’s a point, it’s an object of some size. And it’s made up of some quarks that are charged. And so you can ask how are those quarks distributed inside the proton,” Beck explains.

The quarks’ electric charges also provide scientists a way to measure how quarks are moving around inside the proton.

“When charged objects move around, they can create a magnetic field. And so we measure what we call the magnetization,” Beck says.

Specifically, just as the G-Zero scientists are measuring the distribution of charge in the proton, by looking at the proton from different angles, they’re also measuring the distribution of magnetization.

“We have opened a new window on this structure, separately measuring the contributions of virtual strange quarks to the electric and magnetic properties of the nucleon,” Beck says.

Researchers assemble one of eight detector segments for installation in the ferris wheel-shaped G-Zero apparatus.

Researchers assemble one of eight detector segments for installation in the ferris wheel-shaped G-Zero apparatus.

Strange Quarks at Work

The result from this years-long effort to measure strange matter in the proton has revealed that strange quarks don’t charge up or magnetize the proton all that much, at least at low resolution.

“These results indicate strange quarks make small, less than 10 percent contributions, to the charge/magnetization distributions. Ten percent compared to the total charge and magnetization distribution,” says David Armstrong, a G-Zero collaborator and professor at The College of William and Mary. “The extra quarks that we measured in the sea are not significantly changing the size or shape and the magnetic strength.”

So although the researchers did measure the virtual strange quarks in the proton, it appears that these quarks either don’t dally long enough inside the proton to have a significant effect on its properties before melting back into strong force energy or don’t get far enough away from each other to be seen (i.e. they could have an effect separately, but as a close pair, any effect they would have cancels out).

The G-Zero scientists say that this is surprising, since other experiments give strong indications that there are a significant number of strange quarks in the proton, and early theoretical calculations suggested that the strange quarks could contribute significantly more than 10% of the proton’s charge or magnetization at the level they measured.

“What G0 shows is that there seems to be a strong tendency to be in close pairs,” Beck adds. “Observations are often a strong reminder that things are not quite so simple as we might have thought. Although the lightest virtual quarks [up and down quarks in the sea] appear to interact with their surroundings in the proton, there is little evidence in our results that the strange quarks do so. But we are, of course, still thinking about what is going on.”

Two Forces, Two Tools

Of the four forces of nature, the strong force isn’t the only force that can be probed using electrons from Jefferson Lab’s CEBAF accelerator. Two other forces that can be quantified are the electromagnetic force and the weak force.

The electromagnetic force is the primary force that governs how most of the electrons interact with the protons they encounter. The weak force, on the other hand, can also dictate how electrons interact with protons, but it does so in a slightly different way.

G-Zero researchers exploited the difference to get their result. They used electrons that are polarized – or spinning – in a particular direction. The electromagnetic force is unfazed by the fact that the electrons are polarized one way versus another. So scientists will count roughly the same number of protons coming from interactions with electrons spinning in either direction. Not so for the weak force.

“The relative difference in those counting rates tells us how big the weak interaction piece is in this scattering of electrons from protons. We compare it to the strength of the electromagnetic interaction between electrons and protons, and that gives us the answer that we’re looking for,” Beck says.

Further, the scientists also counted the electron/proton interactions that they observed from two different angles: those that were knocked forward out of the target and those that splashed backward. This allowed the scientists to better separate the electric and magnetic contributions.

Another Bonus of the Weak Force

The G-Zero researchers also had one other goal, and it was the trickiest part of the experiment yet. They wanted to see if they could get an extra measurement of the weak force inside the proton.

As already mentioned, the scientists were sure they could measure the weak force mediating the interaction of the electron probe with the proton. But it was also possible that they could catch a glimpse of an extremely rare process: the weak force between the proton’s own quarks.

This measurement of the proton’s so-called “anapole moment” requires the electron to scatter from a quark while that quark is interacting with a neighboring quark through the weak interaction.

“They’re talking to each other, not through the strong interaction, but through the weak, which is incredibly hard to measure in other ways,” Armstrong explains.

While the scientists did get a peek at this process, they didn’t get enough information to make any bold statements about what they saw.

However, they have reported their result in the recent paper in hopes it can provide a starting point for future research.

G-Zero Wraps Up

The G-Zero experiment was conducted in numerous sessions in Hall C, beginning in 2002 and concluding in 2007. The recent result was a culmination of these running periods followed by intense data analysis by a team of faculty, JLab staff members and students. More results are expected from other aspects from the G-Zero data.

For now, the G-Zero experimenters are happy that they have some of their primary results published and are finally nearing completion of the massive effort it took to carry it out.

“The early proposal said we want to measure strange quark effects at the level of about ten percent of the total. We reached our goal, and we’re saying any strange quark effects amount to less than that,” Armstrong said.

G-Zero was financed by the U.S. Department of Energy and the National Science Foundation. In addition, significant contributions of hardware and scientific/engineering resources were also made by CNRS in France and NSERC in Canada.

Several other electron scattering experiments, including the SAMPLE experiment at MIT-Bates, the A4 experiment at the Mainz Laboratory in Germany, and HAPPEx at Jefferson Lab were also designed to study strange quarks in the proton.

by Kandice Carter

Guest author

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A long-lost object on the Moon will help test general relativity

April 26, 2010 | 3:26 pm

In 1971, a Soviet moon lander called Lunokhod 1 sent its last signal back to Earth. Since that time, scientists have been keeping an eye out for it but not had any luck. Now, says a press release from the University of California, San Diego, the lander has been found, and a simple but important piece of cargo on it is intact. Different teams contributed to the process with an Arizona State University team analyzing images from NASA Lunar Reconnaissance Orbiter. The San Diego team went the next step to find a key object.

The object sought is a corner reflector. It’s just three mirrors at right angles to each other forming a corner. The beauty of this device is that it reflects any light that hits it back along the path it came from, no matter which direction it came from. That means you can just put one in place, not worry too much about its orientation, and know that it will reflect back to you. I’ve made them myself using a few foot-square mirror tiles from IKEA that cost about $1 each, and it works really well and is definitely worth playing with for the unusual sight of yourself in a mirror the way other people see you, not seeming flipped left to right. The ones on the Moon aren’t actually three mirrors mounted that way but a transparent prism, with the surfaces well polished and acting as mirrors.

There are a few sets of corner reflectors on the Moon. Three were left by Apollo missions, and there is another on Lunokhod 2. Scientists routinely send laser pulses to these corner reflectors knowing that they will come back to the source. By timing the pulses, they can work out the distance to the Moon with astonishing precision–potentially to the nearest millimeter. By using three corner reflectors, scientists can work out the orientation of the Moon precisely, and a fourth can give information on the tidal distortions of the Moon.

By piecing together all this information, physicists such as Tom Murphy and his colleagues from UCSD, who found the missing Soviet reflector, can test Einstein’s General Theory of Relativity. They can compare the detailed orbit of the Moon with what theory predicts and see if it all checks out. It’s a relatively cheap and simple way to do an experiment that gives nice results. Along the way, lunar geologists can learn more about the structure and changes of the Moon.

Finding the additional corner reflector has extra importance at this time, as the same physicists who found this old lander had concluded a few weeks ago that the known corner reflectors were started to be covered in moon dust, degrading their usefulness.

Spend a few minutes to read the intriguing and fun story of how they found the lander.

David Harris

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Superconducting cavities could help reduce nuclear waste radiotoxicity

April 22, 2010 | 10:36 am

Accelerator-driven system cavity prototype embedded in its cryomodule. Image: Perrine Royole-Degieux.

Accelerator-driven system cavity prototype embedded in its cryomodule. Image: Perrine Royole-Degieux.

What do the proposed International Linear Collider and environmental protection have in common? The answer is: superconducting cavities. The European MYRRHA is an experimental facility aimed to demonstrate the technical feasibility of nuclear waste transmutation in an accelerator-driven system. The main part of the accelerator will consist in a series of superconducting cavities. At INFN Milano, Italy, a group has transferred all its experience from the TESLA Technology Collaboration and ILC for the development of elliptical proton cavities for this application. Last month, a prototype cryomodule containing one low-beta elliptical cavity was installed in dedicated test stand at the IPNO/Supratech technological platform in Orsay, France.

The general objective of transmutation is the reduction of radiotoxicity, volume and heat load of high-level nuclear waste, which has to be put into final repositories. The question is: how to dispose of nuclear waste? Parts of radionuclides remain hazardous for more than a million years. Transmutation roughly means “burning” these isotopes to obtain waste products whose lifetime is in the order of about a few hundred years. The European accelerator-driven machine concept (ADS) requires a high-power proton accelerator, which delivers a proton beam onto a spallation target. The outcoming high-intensity neutron flux then feeds a sub-critical core (see image 2). The MYRRHA project (Multipurpose hybrid research reactor for high-tech applications), whose construction is foreseen in the years to come at Mol, Belgium, is aimed to demonstrate that coupling an accelerator with a nuclear reactor works.

The European MYRRHA accelerator reference scheme. Image: Jean-Luc Biarrotte.

The European MYRRHA accelerator reference scheme. Image: Jean-Luc Biarrotte.

Two European labs, INFN/LASA (Laboratorio Acceleratori e Superconduttività Applicata) in Milano, Italy and IPNO (Institute of Nuclear Physics) a CNRS/IN2P3 lab at Orsay, France, worked on the design and construction of a 700-megahertz prototypical cryomodule for the ADS proton linear accelerator, within the European Union Framework 6 Project EUROTRANS. Last month, a team of INFN scientists and technicians arrived at Orsay to install the complete cryomodule prototype containing a so called “low-β(beta)” elliptical cavity in the IPNO/Supratech plateform test stand. The Italian team contributed to the design and fabrication of the superconducting cavity and ILC-type blade tuner (read more in ILC NewsLine about the installation of these tuners at KEK for ILC S1-global project). They also designed the cryomodule itself. The French team at IPNO developed the radiofrequency-power source, the cavity couplers and cryogenic components for the installation. EUROTRANS successfully finished this March with the delivery of the cryomodule prototype. “After years spent in meetings agreeing on blueprints and layouts, I’m happy to see all the pieces of our jigsaw ready to make our prototype design a reality,” said Paolo Pierini, researcher at INFN/LASA.

The MYRRHA demonstrator. Image: SCK*CEN/Mol & CNRS/IN2P3/IPN Orsay.

The MYRRHA demonstrator. Image: SCK*CEN/Mol & CNRS/IN2P3/IPN Orsay.

The 100 to 200 cavities superconducting elliptical cavities used at the end of the European ADS will be very different from the ILC’s. The beam energy is relatively small — 600 MeV maximum (hence the use of “low-β” cavities, β being the velocity divided by the speed of light). They work at 700 megahertz (1.3 gigahertz for TESLA-type ILC cavities). However, much of the knowledge learned from the TESLA Technology Collaboration (TTC), the European XFEL and the ILC, in which INFN/LASA and IPNO has been involved for many years now was exploited to build the EUROTRANS cavity. First these cavities have the same elliptical shape as the Tesla-type ILC cavities and are also made of niobium. The cavity surface treatment recipes were copied from the FLASH Facility (at DESY) and ILC experiences. They used electron-beam welding, cleaning and chemical treatments. However, since the desired gradient is only eight megavolts per metre (compared to 31.5 megavolts per metre for the ILC), a “standard” buffered chemical polishing treatment was sufficient to guarantee the performance levels, sparing the difficult task to adapt the electropolishing technique – which has a greater potentiality in terms of high gradients – to the low-β structures.

The INFN/LASA and IPNO teams celebrating the end of installation of the ADS cryomodule prototype at Orsay on 19 March 2010. Image: Paolo Pierini.

The INFN/LASA and IPNO teams celebrating the end of installation of the ADS cryomodule prototype at Orsay on 19 March 2010. Image: Paolo Pierini.

The ADS accelerator also brought specific issues to the IPNO and LASA experts. The fact that the neutron beam finally fires on sub-critical reactor requires that the proton beam function is a continuous mode with a very limited number of interruptions: less than five stops of more than one second per year. “As accelerator experts, we discovered a new culture while working in close collaboration with nuclear plants teams,” said Jean-Luc Biarrotte, an engineer working at the Accelerator Division of IPNO. “We were used to design accelerators without such stringent requirements on reliability.” To reach the extremely ambitious reliability goals, the accelerator engineers had to work hard to follow new reliability-oriented practice. Final tests of the prototype are being performed at Orsay this month and they hope to conclude soon on promising results towards the realisation of the MYRRHA demonstrator.

“This project is a nice by-product of the FLASH/ILC technology driven by high-energy physics, and an application of superconducting radiofrequency to contribute to live in a cleaner world, as we need more and more energy to maintain our lifestyle, and sustain the development of emerging countries,” concluded Pierini. “High radio-toxicity waste production remains a major environment topic and the ADS represents one possibility to reduce the production of spent fuel. Our collaborative activity is a small step towards this direction.”

by Perrine Royole-Degieux

This story first appeared in ILC Newsline on April 22, 2010.

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Wanna routinely win March Madness? Bet on science

April 20, 2010 | 1:09 pm

When most people think of March Madness, they think of  precision and brawn. But they ought to throw brains into that list.

Basketball teams from universities involved in the particle-physics outreach program QuarkNet routinely swoosh their way through the brackets in the annual National Collegiate Athletic Association tournament.

Since QuarkNet’s inception 12 years ago,  a dozen of the 64 competing teams, on average, have had QuarkNet ties. In 2004, all of the teams in the national finals, known as the Final Four, claimed QuarkNet allegiance.

QuarkNet-participating schools consistently have a higher proportion of men’s teams advancing to the Final Four and women’s teams advancing to the Sweet 16.  Based on the number of QuarkNet teams that have participated in the NCAA tournament during the past 12 years, statistically 4.3 men’s teams should have been in the finals, yet 10 teams made it. Only two QuarkNet men’s teams should have become national champions, but five did. For the Women’s teams, 4.3 should have made it to the finals, while 5 teams did and two should have claimed the national championship, which is what has happened.

Five of the last 11 national champion men’s teams claim QuarkNet membership: Michigan State in 2000, Maryland in 2002, Florida in 2006 and 2007 and Kansas in 2008. Last year, Michigan State made it to the national finals.

While QuarkNet-related men’s teams tend to play better throughout the tournament than their non-QuarkNet competitors, the women’s teams play better in the first two rounds and then fall off. QuarkNet women’s teams have made it to the national finals twice: Maryland in 2006 and Notre Dame in 2001. Last year, Oklahoma made it to the national semi-finals. In 2008 the women’s championship went to Stanford University, a QuarkNet alumni.

While QuarkNet teams didn’t bring home trophies this year, they did well, as shown by the final standings for the men’s bracket and the women’s bracket.

Whether QuarkNet affiliation brings luck to the basketball court or not, the science outreach program has proven its national value. The DOE-and NSF-sponsored QuarkNet program brings high school students and teachers to the frontier of 21st century research by involving them in research programs at the world’s major particle physics laboratories.

High school students and teachers connect with Fermilab and other particle physics research centers through university scientists working on experiments. At Fermilab, they work on the largest US particle detectors, DZero and CDF, and build the smallest classroom cosmic ray detectors.

Tona Kunz

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Neutrinos: Clues to the most energetic cosmic rays

April 19, 2010 | 1:13 pm

Spencer Klein with the prototype ARIANNA station, Ross Ice Shelf.

Spencer Klein with the prototype ARIANNA station, Ross Ice Shelf.

We’re constantly being peppered by showers of debris from cosmic rays colliding with atoms in the atmosphere. Cosmic rays aren’t actually rays, of course, they’re particles; ninety percent are protons, the nuclei of hydrogen atoms, and most of the rest are heavier nuclei like iron. Some originate from our own sun but most come from farther off, from the Milky Way or beyond.

“The most energetic cosmic rays are the rarest, and they pose the biggest mystery,” says Spencer Klein of Berkeley Lab’s Nuclear Science Division. He compares the energy of an ultra-high-energy (UHE) cosmic ray to a well-hit tennis ball or a boxer’s punch – all packed into a single atomic nucleus.

“If they’re protons, they have about 40 million times the energy of the protons accelerated at the Large Hadron Collider,” Klein says. “With present technology we’d need to build an accelerator around the sun to produce protons that energetic. Not only do we not know how these cosmic accelerators work, we don’t even know where they are.”

Being electrically charged, even the most energetic cosmic rays are forced to bend when they traverse interstellar magnetic fields, so it’s not possible to extrapolate where they came from by looking back along their paths when they arrive on Earth.

Yet they can’t come from too far away. Klein explains that because cosmic rays lose energy by plowing into the photons of the cosmic microwave background as they travel, “the ones that we observe must come from the ‘local’ universe, within about 225 million light years of Earth. This sounds like a long distance, but, on cosmic scales, it isn’t very far.”

In all that volume of “nearby” space, sources capable of producing such high-energy nuclei have not been clearly identified. One clue to the origin of the highest-energy cosmic rays is the neutrinos they produce when they interact with the very cosmic microwave photons that slow them down.

How to find a cosmic accelerator

“Neutrinos have important advantages as observational tools,” says Klein. “The only way they interact is through the weak interaction, so they aren’t deflected by magnetic fields in flight, and they easily slip through dense matter like stars that would stop the cosmic rays themselves.”

The flip side is that it’s quite a trick to catch neutrinos, especially those produced by rare events. Locating neutrinos produced by UHE cosmic rays needs a detector covering a huge area.

Which is how Klein came to find himself tent-camping on the Ross Ice Shelf last December (the middle of summer in Antarctica), along with his colleague Thorsten Stezelberger of the Lab’s Engineering Division and camp manager Martha Story from the Berg Field Center, a support service at McMurdo Station, the main U.S. base in Antarctica. Klein and Stezelberger were setting up a prototype station for the proposed ARIANNA array of neutrino detectors (ARIANNA stands for the Antarctic Ross Ice Shelf Antenna Neutrino Array).

Unlike such neutrino detectors as SNO in Canada, Daya Bay in China, Super-Kamiokande in Japan, or IceCube, the huge neutrino telescope under construction deep in the ice at the South Pole, ARIANNA doesn’t need miles of rock or the Earth itself to filter out background events. That’s because ARIANNA will be looking for an unusual kind of neutrino signal known as the Askaryan effect.

ARIANNA will observe the shower of electrons, positrons, and other particles produced when a neutrino interacts in the ice below the ARIANNA detectors. In 1962, Gurgen Askaryan, an Armenian physicist, pointed out that these showers contain more electrons than positrons, so have a net electric charge. When a shower develops in ice, this moving charge is an electrical current which produces a powerful pulse of radio waves, emitted in a cone around the neutrino direction.

The energy shed by particles moving faster than the speed of light in a medium like glass or water (light moves through water at only three-quarters of its speed in vacuum) is called Cherenkov radiation, and is perhaps most familiar as the blue glow made by fast-moving electrons in a pool surrounding a nuclear reactor. The same visible-light-wavelength Cherenkov radiation is used to detect charged-particle events created by neutrinos in detectors like IceCube.

Instead of optical wavelengths, ARIANNA observes Cherenkov radiation at radio wavelengths; the strength of the radio signal is proportional to the square of the energy of the neutrino that gave rise to it. To capture these signals, ARIANNA will use radio antennas buried in the snow on top of the ice.

An energetic neutrino striking the upper atmosphere creates a shower of particles in which electrons predominate. When the shower enters the ice, it sheds Cherenkov radiation in the form of radio waves, which reflect from the interface of ice and water and are detected by antennas buried in the snow.

An energetic neutrino striking the upper atmosphere creates a shower of particles in which electrons predominate. When the shower enters the ice, it sheds Cherenkov radiation in the form of radio waves, which reflect from the interface of ice and water and are detected by antennas buried in the snow.

The Ross Ice Shelf makes an ideal component of the ARIANNA detector – not least because the interface where the ice, hundreds of meters thick, meets the liquid water below is an excellent mirror for reflecting radio waves. Signals from neutrino events overhead can be detected by looking for radio waves that have been reflected from this mirror. For neutrinos arriving horizontally, some of the radio waves will be directly detected, and some will be detected after being reflected.

As envisaged by its principal investigator, Steven Barwick of UC Irvine – who visited the Ross Ice Shelf in 2008 – ARIANNA would eventually be comprised of up to 10,000 stations covering a square expanse of ice 30 kilometers on a side.

Neutrinos on ice

Ten thousand stations is the eventual goal, but the first step is to see whether just one station can work. During the Antarctic summer, solar panels will provide power for the radio antennas under the snow and the internet tower that sends data back to McMurdo Station, via a repeater tower on nearby Mt. Discovery. During the long, dark winter, it’s hoped that the power will come from wind turbines or a generator.

Thorsten Stezelberger buries a radio antenna six feet deep in the snow.

Thorsten Stezelberger buries a radio antenna six feet deep in the snow.

When the temperature is mostly below freezing even summer camping is a challenge, as Klein and Stezelberger found. With all supplies brought in by helicopter, the team set up three tents for sleeping, a larger (10 foot by 20 foot) tent as a kitchen, dining room, laboratory and office, and a small tent for a toilet. Instead of tent pegs, the tents are held down by guy ropes tied to “deadman anchors.”

“For each rope, we dug a two-foot-deep hole and buried a long bamboo stake with the rope tied to it,” Stezelberger explains. “When it was taut, we refilled the hole with snow – a fair bit of work.”

On the second day the team unpacked and assembled the six-foot tall station tower, made of metal pipes anchored to plywood feet under the snow. The tower holds four solar panels, a wind turbine, and antennas for receiving time signals from global positioning satellites, and for communicating via Iridium communications satellites.

Klein, Stezelberger and Story spent the third day assembling, testing, and burying the neutrino-detecting antennas in six-foot-deep trenches in the snow. On the fourth day an internet tower – network communications were invaluable for sending data north, and for allowing people to work remotely on the station computer – was brought in by helicopter and erected by a four-person crew, who stayed for lunch. “Fortunately they brought their own,” Klein remarks. “We were wondering how we’d feed everyone with only four forks, four spoons, and four knives.”

After another week, which was mostly spent testing instruments, including bouncing radio signals off the water-ice interface, plus two days waiting for the weather to clear so that helicopters could pick them up, the team finally struck camp. After packaging their gear in slings to be picked up by subsequent flights, they climbed aboard a chopper and returned to base, leaving behind a functioning station intended to survive the oncoming winter.

Klein and Stezelberger made it back to Berkeley Lab by the last day of December. Klein, aided by UC Irvine’s Barwick and graduate student Jordan Hanson, neutrino physicist Ryan Nichol of University College London, and Lisa Gerhardt of Berkeley Lab’s Nuclear Science Division (herself recently returned from work on IceCube at the South Pole), spent the next weeks analyzing the data from the ARIANNA prototype station on the ice, as it continued to report via the internet. The stream of information included housekeeping data and scientific data in the form of antenna signals.

“Wind had generally been so calm during the week and a half we spent on the ice, we were afraid the wind generator wasn’t going to be sufficient for the station’s power needs during the winter,” Klein says. “But after we left, the wind picked up and the wind turbine started functioning, which encouraged us.”

The antenna data was also instructive, and there was a lot of it – signals from natural background noise and from man-made sources. An event every 60 seconds was the “heartbeat” pulse emitted by the station itself, which the team had set up to check the detector.

“But there were other, unexpected periodic signals, pairs separated by almost exactly six seconds, their rate varying over 24 hours,” Gerhardt says. Periodic signals strongly hint at man-made sources. “We think they’re probably from the switching of the power supplies for the internet hardware.”

Thorsten Stezelberger and camp manager Martha Story at dinner.

Thorsten Stezelberger and camp manager Martha Story at dinner.

Other events, aperiodic, were part of the irreducible background, including thermal noise due to molecular motion in the equipment. This set a natural limit to the detector’s performance but should be improved with better equipment.

One thing the prototype station hasn’t seen is an energetic neutrino, and Klein doesn’t expect it to catch one. If the prototype survives the winter, the next step will be a group of five to seven such stations with equipment custom-designed to do the job. The full array is far in the future.

“One real event would be an accomplishment,” says Klein, “and it might take a hundred stations to achieve even that. UHE cosmic rays are extremely rare. If we can track just one back to its origin, we’ll have made a tremendous advance in neutrino astronomy.”

By Paul Preuss

This story first appeared at Berkeley Lab’s News Center.

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Dark Matter: Can you hear me now?

April 16, 2010 | 1:48 pm

COUPP collaborator Andrew Sonnenschein checks on the 4kg bubble chamber in in the MINOS hall at Fermilab in 2005.

COUPP collaborator Andrew Sonnenschein checks on the 4kg bubble chamber in in the MINOS hall at Fermilab in 2005.

Pockets of dark matter litter roughly 25 percent of the universe like patches of static you hit while surfing the radio dial: definitely there but of unclear origin.

Through a process of elimination, Chicagoland Observatory for Underground Particle Physics collaborators say they have found a way to use sound to tune in dark matter passing through an underground bubble chamber and tune out imposter particles. This acoustic discrimination works if that dark matter consists of Weakly Interacting Massive Particles, or WIMPs, one of the leading theoretical candidates for this mysterious gravitational subatomic material.

Based on the theories of the makeup of WIMPs and data about how particles with similar masses and no electric charge behave, physicists can estimate the type of bubble and vibration noise that a WIMP would generate when striking the nucleus of a liquid particle in a detector. Unfortunately, in COUPP’s bubble chamber that simulated WIMP bubble looks much like the bubble caused by common alpha particles such as radon. These unstable particles decay emitting an alpha particle and a secondary particle that collide and causes a recoil like a battleship firing a large shell. Differentiating between these two particle interactions had researchers stymied until they learned to listen, not look.

Collaborators from Fermilab, University of Chicago and Indiana University at South Bend, targeted this last remaining particle that could mimic the nuclear recoil of a WIMP dark matter particle by listening to the sound vibrations its recoil causes. Program the detector to rule out that sound, collaborators decided, and any other recoil sound would likely signal the arrival of a dark matter particle.

This past winter that realization literally caused the jaw of COUPP collaborator Mike Crisler to drop when during a simple R&D test to get rid of radon noise in a 4kg bubble chamber showed that simulated WIMPS and alpha particles make distinctive noises.

“This is really one of the more stunning moments I have had at Fermilab,” Crisler said. “And I have been here for 30 years.”

When a charged particle zips through the liquid, it triggers boiling along its path, which is visible as a series of small bubbles. Scientists expect a WIMP to leave a single bubble in contrast to the multi-bubble tracks left by many other particles.

When a charged particle zips through the liquid, it triggers boiling along its path, which is visible as a series of small bubbles. Scientists expect a WIMP to leave a single bubble in contrast to the multi-bubble tracks left by many other particles.

That deep ping, sounding somewhat like a submarine’s sonar, caused by a vibration at the edge of the bubble chamber was generated by pressure changes after a charged particle zipped through the chamber. It was a game-changing moment for COUPP and, the collaborators hope, for the search for dark matter.

Theorists predict the discovery of what particle composes dark matter within the next five to 10 years, and experiments across the globe are vying to claim that prize by creating unique and larger detectors.

How well these detectors “hear” could help determine who finds dark matter first. COUPP and the Italian experiment PICASSO located in SNOLAB in Canada, both make bubbles in super-heated liquid-type detectors, and listen for the indirect sound of vibrations from the particle collisions that cause the bubbles. The pair have been jockeying for leadership in the search for spin-dependent WIMPs, where the WIMPS’ interaction depends on the spin of the nucleus of the particle with which it collides. PICASSO first initiated the use of sound to differentiate dark matter from alpha particles, but, at least for the moment, COUPP has made the most use of this tool.

During an initial four-month test in Fermilab’s 350-foot deep NUMI tunnel, COUPP validated the use of alpha discrimination and set new spin-dependent WIMP limits. At a Wine and Cheese lecture March 19 at Fermilab, COUPP collaborators highlighted these results.

The leaders in the search for spin-independent WIMPs are CDMS II, which records the direct sound vibrations in a detector in Minnesota, and XENON 100, which uses light and electric charge in its Italian detector.

COUPP’s addition of acoustic discrimination could make it more competitive with CDMS II and XENON 100, Crisler said. The addition of a larger detector and deeper home will reveal how much more competitive.

Collaborators plan to test a larger 60 kg chamber this month in the NUMI

COUPP collaborators install a 60 kg bubble chamber for testing in the DZero building at Fermilab in September 2009.

COUPP collaborators install a 60 kg bubble chamber for testing in the DZero building at Fermilab in September 2009.

tunnel and possibly relocate it to the 2-kilometer deep SNOLAB as early as fall. They hope to eventually partner with the PICASSO experiment.

“There have been concerns that even with its spectacular rejection of gamma and beta background, COUPP might always be limited by alpha background events,” Crisler said. “But COUPP with robust alpha rejection has the potential to move well ahead of the competition.”

It was PICASSO that gave COUPP the idea of using acoustic discrimination when it discovered in 2008 less noise from nuclear recoils from simulated WIMP particles than from alpha decays. The alpha decay emits both a recoil and an alpha particle, making it sound louder. PICASSO found the alphas produced vibrations that were roughly twice as loud, which can be seen as higher frequency signals in the detector readouts. COUPP got an even clearer signal when it adapted what PICASSO had done with its superheated gel droplets to COUPP’s water-like CF3I, a fire-extinguishing liquid. Looking for bubbles previously had ruled out most particles that could be confused for dark matter, and now, listening to bubbles has ruled out the last remaining potential imposter, the alpha particle.

“The alpha and potential dark matter signals may sound roughly the same,” said COUPP collaborator Jeter Hall. “But the alpha backgrounds are significantly louder, making discrimination easier.”

Hear the difference here:

A sound clip of an alpha bubble in the COUPP experiment.

A sound clip of a simulated WIMP bubble in the COUPP experiment.

Tona Kunz

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