Tammy Plotner, Author at Universe Today

November 15, 2011December 24, 2015 by Tammy Plotner

Goldilocks And The Habitable Zone – The Increased Place In Space

Artist's impression of a planet orbiting red dwarf GJ1214.

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It’s referred to as the “Goldilock’s Zone”, but this area in space isn’t meant for sleepy or hungry bears – it’s the relative area in which life can evolve and sustain. This habitable region has some fairly strict parameters, such as certain star types and rigid distance limits, but new research shows it could be considerably larger than estimated.

In a study done by Manoj Joshi and Robert Haberle, the team considered the relationship which occurs between the radiation for red dwarf stars and a possible planet’s reflective qualities. Known as albedo, this ability to “bounce back” light waves has a great deal to do with surface layers, such as ice and snow. Unlike our G-type Sun, the M-class red dwarf is much cooler and produces energy at longer wavelengths. This means a great deal of the radiation is absorbed – rather than reflected – turning the ice and snow into possible liquid water. And, as we know, water is considered to be a primary requirement for life.

“We knew that red dwarfs emit energy at a different wavelength, and we wanted to find out exactly what that might mean for the albedo of planets orbiting these stars.” explained Dr. Joshi from the National Centre for Atmospheric Science, who carried out the research in collaboration with Robert Haberle from the NASA Ames Research Centre.

What makes this theory even more charming is that M-class stars make up a very substantial portion of our galaxy’s total population – meaning there’s even more possible Goldilock’s Zones yet to be discovered. Considering the lifespan of a red dwarf star also increases the chances – as well as the distance a planet would need to be located for these properties to happen.

“M-stars comprise 80% of main-sequence stars, and so their planetary systems provide the best chance for finding habitable planets, i.e.: those with surface liquid water. We have modelled the broadband albedo or reflectivity of water ice and snow for simulated planetary surfaces orbiting two observed red dwarf stars (or M-stars) using spectrally resolved data of the Earth’s cryosphere.” explains Joshi. “In addition, planets with significant ice and snow cover will have significantly higher surface temperatures for a given stellar flux if the spectral variation of cryospheric albedo is considered, which in turn implies that the outer edge of the habitable zone around M-stars may be 10-30% further away from the parent star than previously thought.”

Have we discovered planets around red dwarf stars? The answer is yes. In order to calculate the effects of radiation and albedo, the team chose to use similar M-class stars, Gliese 436 and GJ 1214, and applied it to a simulated planet with an average surface temperature of 200 K. Why that particular temperature? In this circumstance, it’s the temperature at which one bar of carbon-dioxide condenses – a rough indicator of the outer edge of a habitable zone. It is theorized that anything registering below this temperature is too cold to harbor life.

What the team found was high albedo planets register a higher surface temperature when exposed to longer wavelength radiation. This means ice and snow covered planets could exist much further away from a red dwarf parent star – as much as one third more the distance.

“Previous studies haven’t included such detailed calculations of the different albedo effects of ice and snow.” explains Joshi. “But we were a little surprised how big the effect was.”

Original Story Source: Planet Earth OnLine. Further Reading: Suppression of the Water Ice and Snow Albedo Feedback on Planets Orbiting Red Dwarf Stars and the Subsequent Widening of the Habitable Zone.

November 15, 2011December 24, 2015 by Tammy Plotner

Happy Birthday, Sir William Herschel!

On this day in 1738, an astronomy legend was born – Sir William Herschel. Among this British astronomer and musician’s many accomplishments, Herschel was credited with the discovery of the planet Uranus in 1781; detecting the motion of the Sun in the Milky Way in 1785; finding Castor’s binary companion in 1804 – and he was the first to record infrared radiation. Herschel was well known as the discoverer of many clusters, nebulae, and galaxies. This came through his countless nights studying the sky and writing catalogs whose information we still use today. Let’s take a brief, closer look at just who he was…

Born as Frederick William Herschel, this Hanover, Germany native had nine brothers and sisters. During his teenage years, he and his brother, Jakob, were oboists in a military band. When war ensued, his father sent the pair to England to escape. Once there, Herschel continued his musical career by playing cello and harpsichord – eventually composing 24 symphonies, a handful of concertos and religious music. He continued to be a musician, with many appointments, until middle age. Most of his family also migrated to England, the most famous of which is his sister Caroline, who came to live with him in 1772.

But it wasn’t music that was Herschel’s passion. After he met English Astronomer Royal Nevil Maskelyne, he began construction on his own reflector telescope, spending up to 16 hours a day grinding and polishing the speculum metal primary mirrors. By age 35 he’d begun his astronomical journey in earnest – and a year later he began recording his observations from the Great Orion Nebula to the rings of Saturn. Sir William’s interest was taken by the study of double stars and with a 160mm telescope of his own construction, he began a systematic search for binaries among “every star in the Heavens” in October, 1779 and continued listing discoveries through 1792, eventually compiling three catalogs.

During this time he continued to support himself and his sister with his music. In her biography, Caroline recounts how he would rush home between acts to scan the skies – and how she often had to clean pitch from mirror-making from his clothes to make him presentable. From 1782 to 1802, Sir William swept the skies, recording all he saw and sharing his discoveries with other astronomers. So devoted was he, that he even gave Caroline her own telescope in 1783, encouraging her to also make her own observations and discoveries. Herschel published his discoveries as three catalogues, a walloping 2400 entries, filled with distant nebulae and cosmic wonders. Over the time of his astronomical career, Herschel constructed more than four hundred telescopes – the most famous of which had an almost 50 inch diameter mirror and a 40 foot focal length!

In later years, he and Caroline moved on to Windsor Road in Slough… a residence which would eventually be come to known as “Observatory House”. It was during this time he married and eventually had a son – John. Caroline also moved on, yet continued to be his secretarial assistant. Sir William’s astronomical career was quite illustrious – so much so that this article only highlights a few of his accomplishments. He observed and recorded the satellites of his discovery, Uranus, along with more obscure moons belonging to Saturn. He did work with infrared radiation, popularized the term “asteroid”, studied the martian polar caps – revealing them as seasonal – and may very well have been the first to discover the rings of Uranus. His lack of a formal “astronomical education” never slowed Sir William Herschel down!

“I have looked further into space than ever human being did before me. I have observed stars of which the light, it can be proved, must take two million years to reach the Earth.”

Herschel’s life ended at a ripe old age of 84… Passing on at his beloved Observatory House. His son, John Herschel, would carry on in his father’s footsteps and also became a famous astronomer. While few of us will ever be able to match Herschel’s passion for astronomy, at least we can take a moment to look at the stars and wish this astronomy “great” a very happy birthday!

November 15, 2011December 24, 2015 by Tammy Plotner

Unifying The Quantum Principle – Flowing Along In Four Dimensions

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In 1988, John Cardy asked if there was a c-theorem in four dimensions. At the time, he reasonably expected his work on theories of quantum particles and fields to be professionally put to the test… But it never happened. Now – a quarter of a century later – it seems he was right.

“It is shown that, for d even, the one-point function of the trace of the stress tensor on the sphere, Sd, when suitably regularized, defines a c-function, which, at least to one loop order, is decreasing along RG trajectories and is stationary at RG fixed points, where it is proportional to the usual conformal anomaly.” said Cardy. “It is shown that the existence of such a c-function, if it satisfies these properties to all orders, is consistent with the expected behavior of QCD in four dimensions.”

His speculation is the a-theorem… a multitude of avenues in which quantum fields can be energetically excited (a) is always greater at high energies than at low energies. If this theory is correct, then it likely will explain physics beyond the current model and shed light on any possible unknown particles yet to be revealed by the Large Hadron Collider (LHC) at CERN, Europe’s particle physics lab near Geneva, Switzerland.

“I’m pleased if the proof turns out to be correct,” says Cardy, a theoretical physicist at the University of Oxford, UK. “I’m quite amazed the conjecture I made in 1988 stood up.”

According to theorists Zohar Komargodski and Adam Schwimmer of the Weizmann Institute of Science in Rehovot, Israel, the proof of Cardy’s theories was presented July 2011, and is slowly gaining notoriety among the scientific community as other theoretical physicists take note of his work.

“I think it’s quite likely to be right,” says Nathan Seiberg, a theoretical physicist at the Institute of Advanced Study in Princeton, New Jersey.

The field of quantum theory always stands on shaky ground… it seems that no one can be 100% accurate on their guesses of how particles should behave. According to the Nature news release, one example is quantum chromodynamics — the theory of the strong nuclear force that describes the interactions between quarks and gluons. That lack leaves physicists struggling to relate physics at the high-energy, short-distance scale of quarks to the physics at longer-distance, lower-energy scales, such as that of protons and neutrons.

“Although lots of work has gone into relating short- and long-distance scales for particular quantum field theories, there are relatively few general principles that do this for all theories that can exist,” says Robert Myers, a theoretical physicist at the Perimeter Institute in Waterloo, Canada.

However, Cardy’s a-theorem just might be the answer – in four dimensions – the three dimensions of space and the dimension of time. However, in 2008, two physicists found a counter-example of a quantum field theory that didn’t obey the rule. But don’t stop there. Two years later Seiberg and his colleagues re-evaluated the counter-example and discovered errors. These findings led to more studies of Cardy’s work and allowed Schwimmer and Komargodski to state their conjecture. Again, it’s not perfect and some areas need further clarification. But Myers thinks that the proof is correct. “If this is a complete proof then this becomes a very powerful principle,” he says. “If it isn’t, it’s still a general idea that holds most of the time.”

According to Nature, Ken Intriligator, a theoretical physicist at the University of California, San Diego, agrees, adding that whereas mathematicians require proofs to be watertight, physicists tend to be satisfied by proofs that seem mostly right, and intrigued by any avenues to be pursued in more depth. Writing on his blog on November 9, Matt Strassler, a theoretical physicist at Rutgers University in New Brunswick, New Jersey, described the proof as “striking” because the whole argument follows once one elegant technical idea has been established.

With Cardy’s theory more thoroughly tested, chances are it will be applied more universally in the areas of quantum field theories. This may unify physics, including the area of supersymmetry and aid the findings with the LHC. The a-theorem “will be a guiding tool for theorists trying to understand the physics”, predicts Myers.

Pehaps Cardy’s work will even expand into condensed matter physics, an area where quantum field theories are used to elucidate on new states of materials. The only problem is the a-theorem has only had proof in two and four dimensions – where a few areas of condensed matter physics embrace layers containing just three dimensions – two in space and one in time. However, Myers states that they’ll continue to work on a version of the theorem in odd numbers of dimensions. “I’m just hoping it won’t take another 20 years,” he says.

Original Story Source: Nature News Release. For Further Reading: On Renormalization Group Flows in Four Dimensions.

November 14, 2011December 24, 2015 by Tammy Plotner

LISA Pathfinder – Surfing Gravity Waves

LISA Pathfinder about to enter the space environment vacuum test. Credit: ESA

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Do you remember the LISA mission? I do! The proposed launch for this unique vision is slated for 2014 and the latest sensor technology is making its own waves… by being far more accurate than expected. Now ESA’s LISA Pathfinder mission is better than ever, and ready to tackle the vast ocean of space in search of elusive gravitational waves…

So what’s new? By employing a near complete version of LISA, the Optical Meteorology Subsystem passed its first test under space-like temperature and vacuum conditions. Not only did it make the grade, but it went far beyond. It surpassed the precision requirement needed to detect gravitational waves by 300%!

Einstein predicted them, but to physically record this phenomenon in space, the LISA Pathfinder will utilize a laser to measure the distance between two free-floating gold–platinum cubes. Here on the ground, the team in Ottobrunn, Germany, are performing the tests using mirrors instead of cubes. Not only will the distance between them be cataloged, but their angles with respect to the laser beams. Is LISA good? Darn right. She had an accuracy rating of 10 billionths of a degree!

LISA2 — LISA Pathfinder with scientists in the clean room test environment. Credits: Astrium UK

“This is equivalent to the angle subtended by an astronaut’s footprint on the Moon!” notes Paul McNamara, Project Scientist for the LISA Pathfinder mission.

So how are gravitational waves detected? If perfect conditions do exist in space, then the free-floating cubes should mirror each other’s motions. Now, enter Einstein’s general theory of relativity. If some gravitational event should occur – such as the collision of two black holes – this should cause a minute distortion in the fabric of space. These tiny changes should be detectable. However, the accuracy needed to record such an event would need to be about one hundredth the size of an atom… a size called a “picometre”. Originally, LISA was optimized at 6 picometres measured over a timeline of 1000 seconds. But she bettered her record in 2010 and has now reached an amazing accuracy level of 2 picometres.

“The whole team has worked extremely hard to make this measurement possible,” said Dr McNamara. “When LISA Pathfinder is launched and we’re in the quiet environment of space some 1.5 million km from Earth, we expect that performance will be even better.”

LISA3 — Final preparation work on LISA Pathfinder ahead of the space environment testing. Credits: Astrium UK

The instrument team from Astrium GmbH, the Albert Einstein Institute and ESA are testing the Optical Metrology Subsystem during LISA Pathfinder thermal vacuum tests in Ottobrunn by spacecraft prime contractor Astrium (UK) Ltd. Tentatively set to launch in mid-2014, the LISA Pathfinder is well on its way to ride the gravitational waves and set the pace for ESA’s New Gravitational Wave Observatory. Perhaps within the next 10 years we’ll see even more advancements in finding the “final piece in Einstein’s cosmic puzzle.”

Way to go, LISA!

Original Story Source: ESA News Release.

November 14, 2011December 24, 2015 by Tammy Plotner

Leonid Meteor Shower Peaks – November 17-19, 2011

Leonid meteors seen from 39,000 feet aboard an aircraft during the 1999 Leonids Multi-Instrument Aircraft Campaign (Leonid-MAC). Comet Tempel-Tuttle provides the cometary debris for the Leonid meteor storm, which takes place in mid-November. Credit: NASA/ISAS/Shinsuke Abe and Hajime Yano

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Are you ready for a good, predictable meteor shower? Then break out your favorite skywatching gear because the 2011 Leonid meteor shower is already sparkling the skies…

In the pre-dawn hours on the mornings of November 17-19th, the offspring of Comet Temple/Tuttle will be flashing through our atmosphere at speeds of up to 72 kilometers per second – and enticing you to test your meteor watching skills against partially moonlit skies. Although the waning Moon will greatly interfere with fainter meteor trails, don’t let that stop you from enjoying early evening observations, or enjoying your morning coffee with a handful of “shooting stars” which will be emanating outward from the constellation of Leo.

Where in the skies do you look? For all observers the constellation of Leo is along the ecliptic plane and will be near its peak height during best viewing times. When? Because of the Moon, earlier evening observations are favored (before local midnight), but just a couple of hours before local dawn is the best time to watch. Why? Read on!

Although it has been a couple of years since Temple/Tuttle was at perihelion, don’t forget that meteor showers are wonderfully unpredictable and the Leonids are sure to please with fall rate of around 20 (average) per hour. Who knows what surprises it may bring! Each time the comet swings around our Sun it loses some of its material in the debris trail. Of course, we all know that is the source of a meteor shower, but what we don’t know is just how much debris was shed and where it may lay.

“The Moon is going to be a major interference, but we could see a rate of about 20 per hour,” said Bill Cooke, head of NASA’s Meteoroid Environments Office at NASA’s Marshall Space Flight Center in Huntsville, Alabama. “Some models, including ours, indicate that particles may encounter Earth on November 16 at around 5:30 p.m. EST [2230 GMT], where we could see anywhere from 100 to 200 meteors per hour. So, we could get a Leonid outburst, but unfortunately it is not favorably placed for viewing from the United States.”

As our Earth passes through the dusty matter, it may encounter a place where the comet let loose with a large amount of its payload – or it may pass through an area where the “comet stuff” is thin. We might even pass through an area which produces an exciting “meteor storm” like the Leonids produced in 1883! For those in the know, the Leonid meteor shower also made a rather incredible appearance in 1866 and 1867 – dumping up to 1000 (not a typo, folks) shooting stars recorded even with a Moon present! It erupted again in 1966 and in 1998 and produced 3000 (yep. 3000!) video recorded meteors during the years of 2001 and 2002. But remember, human eyes may only be able to detect just a few. So what’s a realistic guess?

According to Cooke; “We could see rates of about five meteors per hour,” he explained. “If people want to see the Leonids, it might be good to watch the nights of November 16th and 17th. Instead of just going out one night, you might want to go out twice.”

MoonMarsLeonids — Chart Courtesy of "Your Sky"

And to make this year’s show twice as nice, you’ll have a hard time not being distracted with the Moon and Mars being right on the radiant! You won’t be able to miss the Red Planet as the Moon slides along south… First to Mars’ west and then to the east on the nights of November 18th and 19th.

What a terrific show!

November 12, 2011December 24, 2015 by Tammy Plotner

Asteroid Lutetia… A Piece Of Earth?

This image of the unusual asteroid Lutetia was taken by ESA’s Rosetta probe during its closest approach in July 2010. Lutetia, which is about 100 kilometres across, seems to be a leftover fragment of the same original material that formed the Earth, Venus and Mercury. It is now part of the main asteroid belt, between the orbits of Mars and Jupiter, but its composition suggests that it was originally much closer to the Sun. Credit: ESA 2010 MPS for OSIRIS Team MPS/UPD/LAM/IAA/RSSD/INTA/UPM/DASP/IDA

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According to data received from ESA’s Rosetta spacecraft, ESO’s New Technology Telescope, and NASA telescopes, strange asteroid Lutetia could be a real piece of the rock… the original material that formed the Earth, Venus and Mercury! By examining precious meteors which may have formed at the time of the inner Solar System, scientists have found matching properties which indicate a relationship. Independent Lutetia must have just moved its way out to join in the main asteroid belt…

A team of astronomers from French and North American universities have been hard at work studying asteroid Lutetia spectroscopically. Data sets from the OSIRIS camera on ESA’s Rosetta spacecraft, ESO’s New Technology Telescope (NTT) at the La Silla Observatory in Chile, and NASA’s Infrared Telescope Facility in Hawaii and Spitzer Space Telescope have been combined to give us a multi-wavelength look at this very different space rock. What they found was a very specific type of meteorite called an enstatite chondrite displayed similar content which matched Lutetia… and what is theorized as the material which dates back to the early Solar System. Chances are very good that enstatite chondrites are the same “stuff” which formed the rocky planets – Earth, Mars and Venus.

“But how did Lutetia escape from the inner Solar System and reach the main asteroid belt?” asks Pierre Vernazza (ESO), the lead author of the paper.

It’s a very good question considering that an estimated less than 2% of the material which formed in the same region of Earth migrated to the main asteroid belt. Within a few million years of formation, this type of “debris” had either been incorporated into the gelling planets or else larger pieces had escaped to a safer, more distant orbit from the Sun. At about 100 kilometers across, Lutetia may have been gravitationally influenced by a close pass to the rocky planets and then further affected by a young Jupiter.

“We think that such an ejection must have happened to Lutetia. It ended up as an interloper in the main asteroid belt and it has been preserved there for four billion years,” continues Pierre Vernazza.

Asteroid Lutetia is a “real looker” and has long been a source of speculation due to its unusual color and surface properties. Only 1% of the asteroids located in the main belt share its rare characteristics.

“Lutetia seems to be the largest, and one of the very few, remnants of such material in the main asteroid belt. For this reason, asteroids like Lutetia represent ideal targets for future sample return missions. We could then study in detail the origin of the rocky planets, including our Earth,” concludes Pierre Vernazza.

Original Story Source: ESO News Release.

November 12, 2011December 24, 2015 by Tammy Plotner

Tarantula Nebula Is Growing!

Don’t like spiders? Well, here’s one that will grow on you! Located about 160,000 light years in the web of the Large Magellanic Cloud, star-forming region 30 Doradus is best known as the “Tarantula Nebula”. But don’t let it “bug” you… this space-born arachnid is home to giant stars whose intense radiation causes stellar winds to blast through surrounding gases to give us an incredible view!

When seen through the eyes of the Chandra X-ray Observatory, these huge shockwaves of x-ray energy heat the encompassing gaseous environment up to multi-millions of degrees and show up as blue. The supernovae detonations blast their way outward… gouging out “bubbles” in the cooler gas and dust. They show up hued as orange when observed through infra-red emissions and recorded by the Spitzer Space Telescope.

What’s so special about the Tarantula? Because it is so close, it’s a prime candidate for studying an active HII region. This stellar nursery is the largest in our Local Group and a perfect laboratory for monitoring stellar evolution. Right now astronomers are intensely interested in what causes growth on such a large scale – and their curent findings show it doesn’t have anything to do with pressure and radiation from the massive stars. However, an earlier study had opposing conclusions when it came to 30 Doradus’ central regions. By employing the Chandra Observatory observations, we may just find different opinions!

“Observations show that star formation is an inefficient and slow process. This result can be attributed to the injection of energy and momentum by stars that prevents free-fall collapse of molecular clouds. The mechanism of this stellar feedback is debated theoretically; possible sources of pressure include the classical warm H II gas, the hot gas generated by shock heating from stellar winds and supernovae, direct radiation of stars, and the dust-processed radiation field trapped inside the H II shell.” says Laura Lopez (et al). “By contrast, the dust-processed radiation pressure and hot gas pressure are generally weak and not dynamically important, although the hot gas pressure may have played a more significant role at early times.”

Original Story Source: Chandra News Release. For Further Reading: What Drives the Expansion of Giant H II Regions?: A Study of Stellar Feedback in 30 Doradus.

November 12, 2011April 26, 2016 by Tammy Plotner

Keck Observatory Locates Two Clouds Of Pristine Gas From The Beginning of Time

Credit: Simulation by Ceverino, Dekel & Primack

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Is there any place in space which hasn’t been affected by time? The answer is yes. Thanks to some very awesome research, the W. M. Keck Observatory and a team of scientists have recently located two clumps of primordial gas which may very well have had its origin within minutes of the Big Bang.

How do we know these gas clouds are so special? In this case, they are simply too disseminated to enable stellar birth and contain no heavy metals which would support it. These diaphanous regions are pure hydrogen and helium… along with a heavier isotope, deuterium. This combination could mean the two billion year old regions are pure – never involved in the star-forming process. An exciting discovery? You bet. The clouds could have possibly survived in an unchanged state – giving us a look at what may have occurred at the dawn of time.

“Despite decades of effort to find anything metal-free in the universe, Nature has previously set a limit to enrichment at no less than one-thousandth that found in the Sun,” said astronomer J. Xavier Prochaska of the University of California Observatories-Lick Observatory, U.C. Santa Cruz. “These clouds are at least 10 times lower than that limit and are the most pristine gas discovered in our universe.”

Prochaska is part of the Keck team and has coauthored a paper reporting on the discovery with Michele Fumagalli of the U.C. Santa Cruz and John O’Meara of Saint Michael’s College in Vermont. “We’ve searched carefully for oxygen, carbon, nitrogen and silicon – the things that are found on Earth and the Sun in abundance,” Fumagalli said. “We don’t find a trace of anything other than hydrogen and deuterium.”

According to the Keck Observatory news release exactly how they can detect dark, cold, diffuse gas about 12 billion light-years away is a story in itself.

“In this case we actually have to do a bit of a trick,” Prochaska explained. “We study the gas in silhouette.” A more distant quasar provides the light for this. The quasar light shines though the gas and the elements in the gas absorb very specific wavelengths of light, which can only be found by splitting the light into very detailed spectra to reveal the dark lines of missing light.

In other words, said Fumagalli, “All of the analysis is on the light we didn’t get.” The clouds absorb only a small fraction of the quasar light that makes it to Earth. “But the signatures of hydrogen absorption are obvious, so there’s no doubt there’s a lot of gas there.”

While some folks might not get excited over the location of immaculate gases, astronomers think differently. This revelation supports their theories of what may have occurred within moments after the Big Bang and what formed at the time of nucleosynthesis. It’s a look back at when hydrogen, helium, lithium and boron originated.

fumagalli_simB-(3) — The two pristine gas clouds found by astronomers could sit in one of the filamentary regions visible around galaxies in this image, which are from computer simulations. Credit: Simulation by Ceverino, Dekel & Primack

“That theory has been very well tested at Keck as regards to hydrogen and its isotope deuterium,” said O’Meara. “One of the conundrums of that previous work, however, is that the gas also showed at least trace amounts of oxygen and carbon. The clouds that we have discovered are the first to match the full predictions of BBN.”

What’s more, Keck’s two 10-meter optical/infrared telescopes have shown us what the early universe may have been like. This is the very first time that science has been able to peer into regions where no metals have influenced the environment and no stars have formed.

“What excites me about this discovery is that there is an almost a range of 1,000,000 in the metallicity in gases at that time in the universe,” said Fumagalli. In other words, there were places like our Solar system – where metals are very abundant – and there were also places very unlike today, where metals were still virtually non-existent and the gases were unchanged since almost the beginning of time.”

Original Story Source: Keck Observatory News Release. For Further Reading: Detection of Pristine Gas Two Billion Years After the Big Bang.

November 10, 2011February 2, 2021 by Tammy Plotner

The Expanding Universe – Credit To Hubble Or Lemaitre?

This illustration shows American astronomer Edwin Hubble (1889-1953) on the right and Belgian priest and cosmologist Georges Lemaître (1894-1966) on the left. Based on new evidence, both scientists should share credit for independently uncovering evidence for the expanding universe in the late 1920s. Lemaître is also credited with proposing a theory for the origin of the universe that would later be called the "big bang." The telescope on the left is the 100-inch Hooker Telescope on Mt. Wilson in California. The Hubble Space Telescope is on the right. Credit: NASA, ESA, and A. Feild (STScI)

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Perhaps one of the greatest astronomical discoveries of the 20th century may have gone down in the history books as credited to the wrong person. Now known as the Hubble Constant, the theory of an expanding Universe was first speculated by Belgian priest and cosmologist, Father Georges Lemaitre. How did this oversight occur? It may very well be the hand of the man himself who was unpretentious enough to pass on his findings.

According to the the November 10th issue of the journal Nature, astrophysicist Mario Livio of the Space Telescope Science Institute is calling for closure about a conspiracy theory of who should be properly credited for the discovery of the expansion theory. For almost a hundred years we’ve been led to believe American astronomer Edwin P. Hubble was the man who explained the universal expansion in 1929 – although he never won a Nobel prize for his work. His findings were based on the achievements of Vesto Slipher, who – through the use of redshift – calculated recessional velocities and paired them with distances to the same galaxies as Hubble’s work. This led Hubble to demonstrate that the further away a galaxy was, the faster it would recede… the Hubble Constant.

However, two years before Hubble published his work, a quiet man called Georges Lemaitre published the same conclusions based on Slipher’s same redshift data and Hubble’s calculated distances.

Father Georges Lemaitre and Albert Einstein – Historical Image

How did this happen and why didn’t Father Lemaitre get credit? According to news release, it may have been because the original paper was published in French, in a rather obscure Belgian science journal called the Annales de la Societe Scientifique de Bruxelles (Annals of the Brussels Scientific Society). Chances are, we never would have known except for a later translation which was published in the Monthly Notices of the Royal Astronomical Society in 1931… a paper which just “left out” Lemaitre’s 1927 calculations! Of course, there were people who knew these passages had been omitted since 1984 and the ensuing debate accused not only the editors of the Monthly Notices, but Hubble as well.

However, before any accusations can be made, let it be noted that astrophysicist Mario Livio combed through an exhaustive archive of hundreds of letters to the Royal Astronomical Society and the RAS meeting minutes – as well as Father Lemaitre’s Archive. What he found was the good Father had simply omitted the passages himself when he translated the papers to English. In one of two “smoking-gun letters” uncovered by Livio, Lemaitre wrote to the editors: “I did not find advisable to reprint the provisional discussion of radial velocities which is clearly of no actual interest, and also the geometrical note, which could be replaced by a small bibliography of ancient and new papers on the subject.”

What is left for us to ponder is “why” Georges Lemaitre didn’t want to take credit for this discovery. Can there really be an altruistic scientist? One who puts the simple act of discovery above himself?

Livio concludes, “Lemaitre’s letter also provides an interesting insight into the scientific psychology of some of the scientists of the 1920s. Lemaitre was not at all obsessed with establishing priority for his original discovery. Given that Hubble’s results had already been published in 1929, he saw no point in repeating his more tentative earlier findings again in 1931.”

Excuse me, folks… After having read the original news release, I think we should rename the Hubble Telescope to read the “Humble Telescope”.

Original Story Source: Hubblesite News Release.

November 10, 2011December 24, 2015 by Tammy Plotner

New NASA Mission Hunts Down Zombie Stars

This is an artist's concept of a pulsar (blue-white disk in center) pulling in matter from a nearby star (red disk at upper right). The stellar material forms a disk around the pulsar (multicolored ring) before falling on to the surface at the magnetic poles. The pulsar's intense magnetic field is represented by faint blue outlines surrounding the pulsar. Credit: NASA

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Neutron stars have been classed as “undead”… real zombie stars. Even though technically defunct, the neutron star continues to shine – and occasionally feed on a neighbor if it gets too close. They are born when a massive star collapses under its gravity and its outer layers are blown far and wide, outshining a billion suns, in a supernova event. What’s left is a stellar corpse… a core of inconceivable density… where one teaspoon would weigh about a billion tons on Earth. How would we study such a curiosity? NASA has proposed a mission called the Neutron Star Interior Composition Explorer (NICER) that would detect the zombie and allow us to see into the dark heart of a neutron star.

The core of a neutron star is pretty incredible. Despite the fact that it has blown away most of its exterior and stopped nuclear fusion, it still radiates heat from the explosion and exudes a magnetic field which tips the scales. This intense form of radiation caused by core collapse measures out at over a trillion times stronger than Earth’s magnetic field. If you don’t think that impressive, then think of the size. Originally the star could have been a trillion miles or more in diameter, yet now is compressed to the size of an average city. That makes a neutron star a tiny dynamo – capable of condensing matter into itself at more than 1.4 times the content of the Sun, or at least 460,000 Earths.

“A neutron star is right at the threshold of matter as it can exist – if it gets any denser, it becomes a black hole,” says Dr. Zaven Arzoumanian of NASA’s Goddard Space Flight Center in Greenbelt, Maryland. “We have no way of creating neutron star interiors on Earth, so what happens to matter under such incredible pressure is a mystery – there are many theories about how it behaves. The closest we come to simulating these conditions is in particle accelerators that smash atoms together at almost the speed of light. However, these collisions are not an exact substitute – they only last a split second, and they generate temperatures that are much higher than what’s inside neutron stars.”

If approved, the NICER mission will be launched by the summer of 2016 and attached robotically to the International Space Station. In September 2011, NASA selected NICER for study as a potential Explorer Mission of Opportunity. The mission will receive $250,000 to conduct an 11-month implementation concept study. Five Mission of Opportunity proposals were selected from 20 submissions. Following the detailed studies, NASA plans to select for development one or more of the five Mission of Opportunity proposals in February 2013.

What will NICER do? First off, an array of 56 telescopes will gather X-ray information from a neutron stars magnetic poles and hotspots. It is from these areas that our zombie stars release X-rays, and as they rotate create a pulse of light – thereby the term “pulsar”. As the neutron star shrinks, it spins faster and the resultant intense gravity can pull in material from a closely orbiting star. Some of these pulsars spin so fast they can reach speeds of several hundred of rotations per second! What scientists are itching to understand is how matter behaves inside a neutron star and “pinning down the correct Equation Of State (EOS) that most accurately describes how matter responds to increasing pressure. Currently, there are many suggested EOSs, each proposing that matter can be compressed by different amounts inside neutron stars. Suppose you held two balls of the same size, but one was made of foam and the other was made of wood. You could squeeze the foam ball down to a smaller size than the wooden one. In the same way, an EOS that says matter is highly compressible will predict a smaller neutron star for a given mass than an EOS that says matter is less compressible.”

Now all NICER will need to do is help us to measure a pulsar’s mass. Once it is determined, we can get a correct EOS and unlock the mystery of how matter behaves under intense gravity. “The problem is that neutron stars are small, and much too far away to allow their sizes to be measured directly,” says NICER Principal Investigator Dr. Keith Gendreau of NASA Goddard. “However, NICER will be the first mission that has enough sensitivity and time-resolution to figure out a neutron star’s size indirectly. The key is to precisely measure how much the brightness of the X-rays changes as the neutron star rotates.”

So what else does our zombie star do that’s impressive? Because of their extreme gravity in such small volume, they distort space/time in accordance with Einstein’s theory of General Relativity. It is this space “warp” that allows astronomers to reveal the presence of a companion star. It also produces effects like an orbital shift called precession, allowing the pair to orbit around each other causing gravitational waves and producing measurable orbital energy. One of the goals of NICER is to detect these effects. The warp itself will allow the team to determine the neutron star’s size. How? Imagine pushing your finger into a stretchy material – then imagine pushing your whole hand against it. The smaller the neutron star, the more it will warp space and light.

Here light curves become very important. When a neutron star’s hotspots are aligned with our observations, the brightness increases as one rotates into view and dims as it rotates away. This results in a light curve with large waves. But, when space is distorted we’re allowed to view around the curve and see the second hotspot – resulting in a light curve with smoother, smaller waves. The team has models that produce “unique light curves for the various sizes predicted by different EOSs. By choosing the light curve that best matches the observed one, they will get the correct EOS and solve the riddle of matter on the edge of oblivion.”

And breathe life into zombie stars…

Original Story Source: NASA Mission News.