Lunar Eclipse Images From Around the World, Dec. 21, 2010

Looking like a holiday card, this view of the lunar eclipse was taken by Stu Atkinson in the UK

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For the first time in almost four centuries a total lunar eclipse coincided with the solstice – mid-winter for northern hemisphere skywatchers and mid-summer for the southern hemisphere. For those with a clear view of the sky (I was not that lucky!), the entire event was visible from North America, Greenland and Iceland, while western Europe saw the beginning stages before moonset and western Asia got the later stages after moonrise. Australia also saw the late stages of the eclipse.

People with clear skies in the northern hemisphere saw the Moon transformed into a “coppery orb,” as Tony Hoffman from Queens, New York called it (see his image below.) The Moon didn’t disappear completely, as the residual light from its surface is refracted by our atmosphere, resulting in the Moon turning a coppery, red or brown color. The eclipse lasted for about three and a half hours. See some images and videos from around the world, below. Clicking on each image will bring you to the original source.

The Washington Monument is seen as the full moon is shadowed by the Earth during a total lunar eclipse on the arrival of the winter solstice, Tuesday, December 21, 2010 in Washington. From beginning to end, the eclipse lasted about three hours and twenty-eight minutes. Photo Credit: (NASA/Bill Ingalls)
A 'Coppery Orb' as seen by Tony Hoffman in Queens, NY. 'Well worth braving the cold and wind to catch,' Tony said, 'Relatively bright totality with Moon beautifully situated by the horns of Taurus.'
'Even with high cloud, a 7 second exposure brought out the beauty of the eclipsed Moon,' said Mark Zaugg from Calgary, Alberta, Canada.
The ruddy totally eclipsed Moon as seen by Nick Bramhill in Aberdeen, UK.
The Earth's shadow starts to creep across the Moon in this image by Stu Atkinson near Kendal in the UK

You can see the more pictures and the write-up Stu did about the eclipse on his website, Cumbrian Sky: Eclipse-Watching from Narnia.

Astronomer Amanda Bauer took several images of the eclipsed Moon rising over Sydney, Australia, as seen below. See her website, Astropixie, for more images she took of the event.

Astronomer Amanda Bauer took this image of the eclipsed Moon from the Harbour Bridge in Sydney, Australia.
Efrain Morales from the Jaicoa Observatory in Puerto Rico took this sequence of images. 'The weather was not under under optimum conditions,' he wrote, 'but managed to take this sequence thru the cloud gaps until it finally covered it up.
This view of the red Moon was taken by Pete Riesett in Baltmore, Maryland.
An animation made from 60 images taken by an all-sky telescope in New Mexico
This image was taken by Jen Scheer (aka @flyingjenny on Twitter) from Merritt Island in Florida.

Former space shuttle technician Jen Scheer (@flyingjenny on Twitter) got up earlier than usual (she takes a daily sunrise picture from around Kennedy Space Center each morning) to capture some great shots of the eclipse. You can see more of her images at her Flickr page.

A total lunar eclipse begins as the full moon is shadowed by the Earth on the arrival of the winter solstice, Tuesday, December 21, 2010 in Arlington, VA. Photo Credit: (NASA/Bill Ingalls)
This was taken by Phil Plait, the Bad Astronomer, in Boulder Colorado. 'Deep into totality,' Phil said.

Here’s a video taken from Savannah, Georgia in the US:

And another video from UT frequenter, Brent (aka Hellobozos) from Orlando Florida. He took 6 second avi’s every 5 minutes for 6 hours, from 12:30am to 6am EST:

And one more from Carl Hamilton from Bowie, Maryland:

You can also see a great collection of images on JPL’s I’m There Flickr Group, this collection at a German astronomy website called ASTROTREFF, this amazing set of images from Slovakia, Carolyn Collins Petersen has a bunch of images she took from near Boulder Colorado, and this NASA Flickr page.

Here are some more images sent in by readers:

Lunar eclipse from Fair Lawn. NJ. 'Wish I had a more powerful lens but it was well worth waiting up for,' said Universe Today reader Mary Durante Youtt.
Here's one from Lancaster County, Pennsylvania. 'We had to dodge clouds, cold, and wind that jiggled the tripod,' said Beth Katz.
The eclipse as seen by photographer John O'Connor near Kennedy Space Center.

This image was taken by photographer John O’Connor, who normally takes images of rockets and spacecraft (see his website NASATech, for amazing virtual tours of spacecraft, launchpads and more). He was up in the middle of the night to take images of space shuttle Discovery’s intended rollback from the launchpad to the Vehicle Assembly Building, but the rollback was delayed because of a technical problem.

“I intended to take a couple of quick shots of totality before heading out but ended up spending 45 minutes shooting the moon, as they say,” John wrote me. “This is my first attempt at astrophotography. I shot it with a 300 mm fixed focal length lens with a doubler on it. With the 1.5 multiplier factor on the 2/3 size sensor, it was about 900 mm focal length. It was 4 second shot at 100 ISO with an f4.5 aperture, as wide as the lens would let me go. Note the smudged stars. Even at a 4 second exposure the Earth’s rotation is evident, blurring, ever-so-slightly, the lunar disk.”

Magnetic Fields on O-Class Stars

Star classifications. Image credit: Kieff

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The primary method by which astronomers can measure magnetic field strength on stars is the Zeeman effect. This effect is the splitting of spectral lines into two due to the magnetic field’s effect on the quantum structure of the orbitals. For massive O-class stars, their spectra are largely featureless in the visual portion of the spectra due to an insufficient number of atoms with electrons in the necessary orbitals to undergo transitions which can produce visual spectral lines. Thus, determining whether or not these stars have magnetic fields has been a unique challenge. A new paper from researchers at the University of Amsterdam, led by Roald Schnerr, looks for evidence of these fields in the form of synchrotron radiation.

Synchrotron radiation is a form of light produced when relativistic, charged particles move through a magnetic field. The light emitted can be generated in any portion of the spectra from radio to gamma rays, depending on the strength of the field. Astronomically, this was first detected in 1956 by Geoffrey Burbidge in the jets of M87 and has since been used to explain emission in planetary magnetospheres, supernovae, near black holes, and around pulsars.

This form of energy distinguishes itself from other forms of light in two main fashions. The first is that it is highly polarized. This property is generated by the electric and magnetic components always being in the same planes and can be studied with filters that only allow light with its fields in appropriate planes to pass. The second is that the radiation created is “non-thermal”. In other words, it doesn’t match the distribution of wavelengths generated by a blackbody.

Models of massive, O-class stars suggest they should contain magnetic fields. Some evidence has seemed to confirm this. Previous studies have also shown that the stellar winds from some of these stars varies with timescales similar to the rotation rates of the stars which could be interpreted as winds being slowed on some faces by the magnetic field as it swept by.

Schnerr’s team attempted to bolster the evidence for magnetic fields by detecting the non-thermal radiation from these stars. The team selected 5 stars which have been shown to have strongly variable winds, some with cyclic variations and used the Westerbork Synthesis Radio Telescope, in the Netherlands to search for non-blackbody signals. The radio range was selected due to the predicted magnetic field strength.

Ultimately, only three of the five selected targets could be observed with the chosen telescope and only one of those, ξ Persei, showed evidence of a non-thermal spectrum. But while this strengthens the case for magnetic fields on the star, it raises another question: From where do the relativistic particles originate? Although O-class stars have strong stellar winds, their speeds are well studied and well below the necessary velocity.

One clue could come from the fact that ξ Persei is a “runaway star”. These stars have velocities and plunge through the interstellar medium at 30-200 km/sec. The team suggests that a bow shock created by this motion could result in sufficiently high velocities. Whether or not ξ Per has such a bow shock is something that could be determined with additional observations.

While this research provides some interesting clues to the nature of these magnetic fields on these stars, it still relies on a small sample. This technique can certainly be expanded to a larger number of stars in the future and may help astronomers better constrain their models of stellar workings.

M33’s “Object-X”

Often times, objects that are unremarkable in one portion of the spectra, can often be vivid in others. In M33, the Triangulum Galaxy, a star that’s barely visible in the optical, stands out as the second brightest source (and single brightest single star) in the mid-infrared. This unusual star has been the target of a recent study, led by Rubab Khan at the Ohio State University and may help astronomers to understand an unusual supernova from 2008.

The supernova 2008S occurred February first in NGC 6946, the Fireworks Galaxy. Since it happened in a galaxy that is relatively nearby, astronomers seized the opportunity to explore the progenitor star in archival images. Yet images from the Large Binocular Telescope and other optical observatories could not find a star that could be identified as a parent. Instead, the detection of the star responsible came from Spitzer, an infrared observatory. Observations from this instrument indicated that the star responsible may have been unexpectedly low mass for such a powerful explosion leading other astronomers to question whether or not SN 2008S was a true supernova, or merely an impostor in the form of an eruption of a Luminous Blue Variable (LBV), which tend to be more massive stars and would be in stark contradiction to the Spitzer findings.

Yet, regardless of the nature of the nature of SN 2008S, teams all seemed to agree that the progenitor had only been detected in the infrared because it was veiled by a thick curtain of dust. So to help better understand this class of dusty stars, astronomers have been working to uncover more of them, against which they can test their hypotheses.

To find these objects, astronomers have been searching the infrared portion of the spectrum for objects that are exceptionally bright yet lack optical counterparts. The brightest of the stellar sources in M33 features faint star in the red portion of the optical spectrum from the Local Group Galaxies Survey published in 2007, but no star at all in archival records with similar limiting magnitudes from 1949 and 1991. The authors of the new study have dubbed this odd source, Object-X.

The team rules out the possibility that the object could be a young stellar object (YSO), blocked by a thick dust disc along the line of sight, noting that models of even the thickest dust discs still predict more light to be scattered back along the line of sight. Instead, the team concludes that Object-X must be a self-obscured star that has undergone relatively recent mass loss which has cooled to form either graphite or silicate dust. Depending on which type of dust is predominant, the team was able to fit the data to two wildly different temperatures for the star: either 5000 K for graphite, or 20,000 K for the silicate. In all cases, the predicted mass for the central star was always greater than 30 solar masses.

In general, there are two mechanisms by which a star can eject material to form such a curtain. The first is through stellar winds, which increase as the star enters the red giant phase, swelling up and lowering the force of gravity near the surface. The second is “impulsive mass ejections” in which stars shudder and throw mass off that way. A classical example of this is Eta Carinae. The team predicts from the features they found, that Object-X is most likely a cool hypergiant. The fact that the star was completely obscured until very recently hints that the mass loss is not constant (as stellar wind), but patchy, coming from frequent eruptions. As the shell of dust expands, the star should reemerge in the optical, becoming visible again in the next few decades.

Can Nearby Binary Star Systems Mimic Planets?

The vast majority of the known exoplanets have been discovered by the radial velocity method. This method employs the effects of a planet’s gentle tug on its parent star which is perceived as a “wobble” in the star’s motion. A new study, conducted by Morais and Correia, looks at whether this effect can be mimicked by another, distinctly non-planetary, source: Binary stars.

Conceptually, the idea is rather straightforward. A star of interest lies in a triple star system. It is the third member and in a larger orbit around a tight binary system. As the tight binary system orbits, there will be periods in which they line up with the star of interest giving a minutely greater pull before relaxing the pull later in their orbit. This remote tug would show a distinctly periodic effect very similar to the effects expected from an inferred planet.

The obvious question was how astronomers could miss the presence of binary stars, close enough to have a notable effect. The authors of the paper suggest that if the binary pair orbited sufficiently close, it would be unlikely that they could be resolved as a binary. Additionally, if one member were sufficiently faint (an M dwarf), it may not appear readily either. Both of these instances are plausible given that some three fourths of nearby main sequence stars are M class, and about half of all stars are in binary system.

Next, the team asked how important these effects may be. They considered the case of HD 18875, a binary system in which a distant star (A) has a 25.7 year period around a tight binary (Ba + Bb) that orbit each other with a period of 155 days. This system was noteworthy because a hot Jupiter planet was announced around the A star in 2005, but challenged in 2007 when another team could not repeat the observations.

The new study attempted to use their understanding and modeling of three body systems to see if the binary interaction could have produced the spurious signal. Using their model, they determined that the effects of the system itself would have produced effects similar to those of a planet of 4 Earth masses located at 0.38 AU. A planet of such mass is well below the limit of a hot Jupiter and the distance is somewhat larger than usual as well. Thus, the nearby B-binary could not have been responsible. Furthermore, such minute effects of this type are generally interpreted as “super-Earths” and have only become prevalent in observations in the past few years.

Thus, while the unconfirmed planet around HD 18875 A might not have been caused by the nearby binary, the work in this new paper has shown that effects of nearby binaries will become increasingly important as we start detecting radial velocities indicative of less and less massive planets.

Herschel Looks Back in Time to See Stars Bursting to Life

An artist's rendition of one of the newly discovered SPIRE 'hot starburst' galaxies (credit: NASA/CXC/M.Weiss)

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From a Royal Astronomical Society Press release:

Astronomers have found the first conclusive evidence for a dramatic surge in star birth in a newly discovered population of massive galaxies in the early Universe. Their measurements confirm the idea that stars formed most rapidly about 11 billion years ago, or about three billion years after the Big Bang, and that the rate of star formation is much faster than was thought.

The scientists used the European Space Agency’s Herschel Space Observatory, an infrared telescope with a mirror 3.5 m in diameter, launched in 2009. They studied the distant objects in detail with the Spectral and Photometric Imaging Receiver (SPIRE) camera, obtaining solid evidence that the galaxies are forming stars at a tremendous rate and have large reservoirs of gas that will power the star formation for hundreds of millions of years.

Dr. Scott Chapman, from the Institute of Astronomy in Cambridge, has presented the new results in a paper in a special edition of the journal Monthly Notices of the Royal Astronomical Society focusing on results from Herschel.

Scott comments “These Herschel-SPIRE measurements have revealed the new population of galaxies to be hotter than expected, due to stars forming far much more rapidly than we previously believed.”

The galaxies are so distant that the light we detect from them has been traveling for more than 11 billion years. This means that we see them as they were about three billion years after the Big Bang. The key to the new results is the recent discovery of a new type of extremely luminous galaxy in the early Universe. These galaxies are very faint in visible light, as the newly-formed stars are still cocooned in the clouds of gas and dust within which they were born. This cosmic dust, which has a temperature of around -240oC, is much brighter at the longer, far infrared wavelengths observed by the Herschel satellite.

The Herschel-SPIRE image, where 3 examples of the new 'hot starbursts' glowing blue are circled. They appear faint because they are very distant, seen only 3 billion years after the Big Bang (credit: ESA/SPIRE/HerMES).

A related type of galaxy was first found in 1997 (but not well understood until 2003) using the “SCUBA” camera attached to the James Clerk Maxwell Telescope on Hawaii, which detects radiation emitted at even longer sub-millimeter wavelengths. But these distant “sub-millimeter galaxies” were thought to only represent half the picture of star formation in the early Universe. Since SCUBA preferentially detects colder objects, it was suggested that similar galaxies with slightly warmer temperatures could exist but have gone largely unnoticed.

Dr. Chapman and others measured their distances using the Keck optical telescope on Hawaii and the Plateau de Bure sub-millimeter observatory in France, but were unable to show that they were in the throes of rapid star formation.

Herschel is the first telescope with the capability to detect these galaxies at the peak of their output, so Dr. Chapman joined forces with the “HerMES” team, led by Professor Seb Oliver of the University of Sussex and Dr Jamie Bock in Caltech who were undertaking the largest survey of galaxies with Herschel.

With the Herschel observations, focused on around 70 galaxies in the constellation of Ursa Major, the scientists acquired the missing piece of evidence to confirm that these galaxies represent a crucial episode in the build up of large galaxies around us today, such as our own Milky Way.

The orignal Herschel-SPIRE image. Credit: ESA/SPIRE/HerMES.

Team member Professor Rob Ivison from the University of Edinburgh explains the significance of the new results. “With the data we had before, we couldn’t tell exactly where the infrared light from these galaxies comes from. But using SPIRE we can see that this is the signature of star formation”.

The new galaxies have prodigious rates of star formation, far higher than anything seen in the present day Universe. They probably developed through violent encounters between hitherto undisturbed galaxies, after the first stars and galaxy fragments had already formed. None the less, studying these new objects gives astronomers an insight into the earliest epochs of star formation after the Big Bang.

Team colleague Dr Isaac Roseboom from the University of Sussex sums up the work. “It was amazing and surprising to see the Herschel-SPIRE observations uncover such a dramatic population of previously unseen galaxies”. Professor Seb Oliver, also from Sussex, adds: “We are really blown away by the tremendous capability of Herschel to probe the distant universe. This work by Scott Chapman gives us a real handle on how the cosmos looked early in its life.”

With the new discovery, the UK-led astronomers have provided a much more accurate census of some of the most extreme galaxies in the Universe at the peak of their activity. Future observations will investigate the details of the galaxies’ power source and try to establish how they will develop once their intense bursts of activity come to an end.

Read the team’s paper.

LOFAR Swedish Station Begins Construction

An aerial photograph shows the Onsala LOFAR station site. Credit: Onsala Space Observatory/Västkustflyg

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Robert Cumming from the Onsala Space Observatory in Sweden sent us this image, letting us know that construction has officially begun for the Swedish station of the new LOFAR radio telescope. The LOw Frequency ARray is a multi-purpose sensor array, with its main purpose to search the sky at low frequencies (10-250 MHz) which will enable astronomers to see the fog of hydrogen gas that filled the universe during its first two hundred million years. It will also be able to image the regions around supermassive black holes in the centres of nearby galaxies. The headquarters are in the Netherlands, but eight stations will be spread over Europe.

This aerial photograph shows the Onsala LOFAR station site at the lower right. Behind, the white radome of the observatory’s 20-metre telescope and the dish of the 25-meter telescope by the Kattegat shore.

The two circular areas where the LOFAR station’s high-band (snow-covered) and low-band antennas will be placed are already flattened. The cold weather has delayed the next stage in the work, deploying the fibre cables, but the Onsala station should still be fully operational by mid-2011.

Onsala is LOFAR’s northernmost station and will help give the array a close to circular beam. It will also contribute some of the array’s longest baselines.

“Each LOFAR station collects and handles up to 32 terabytes of data every day,” said John Conway, professor of observational radio astronomy at Chalmers University of Technology and Vice-Director of Onsala Space Observatory. “ At Chalmers we’re working together with our European colleagues to develop new kinds of software so that we can analyse radio signals from distant sources.”

Onsala’s LOFAR station will consist of 192 small antennas which together collect radio waves from space. The signals which are registered are then transferred by fiber link to the Netherlands to be combined with data from the other stations.

You can see more images from the Onsala Observatory at the Flickr page.

More information about LOFAR.

Darwin vs. the Sun

The Age of the Sun and Darwinism

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Today, we take it for granted that the Sun produces energy via nuclear fusion. However, this realization only came about in the early 1900’s and wasn’t confirmed until several decades later (see the Solar Neutrino Problem). Prior to that, several other methods of energy production had been proposed. These ranged from burning coal to a constant bombardment of comets and meteors to slow contraction. Each of these methods seemed initially plausible, but when astronomers of the time worked out how long each one could sustain such a brightness, they came up against an unlikely opponent: Charles Darwin.

In a “Catholic Magazine and Review” from 1889, known as The Month, there is a good record of the development of the problem faced in an article titled “The Age of the Sun and Darwinism”. It begins with a review of the recently discovered Law of Conservation of Energy in which they establish that a method of generation must be established and that this question is necessarily entangled with the age of the Sun and also, life on Earth. Without a constant generation of energy, the Sun would quickly cool and this was known to be unlikely due to archaeological evidences which hinted that the Sun’s output had been constant for at least 4,000 years.

While burning coal seemed a good candidate since coal power was just coming into fashion at the time, scientists had calculated that even burning in pure oxygen, the Sun could only last ~6,000 years. The article feared that this may signal “the end of supplies of heat and light to our globe would be very near indeed” since religious scholars held the age of the Earth to be some “4000 years of chronological time before the Christian era, and 1800 since”.

The bombardment hypothesis was also examined explaining that the transference of kinetic energy can increase temperatures citing examples of bullets striking metal surfaces or hammers heating anvils. But again, calculations hinted that this too was wrong. The rate with which the Sun would have to accumulate mass was extremely high. So much so that it would lead to the “derangement of the whole mechanism of the heavens.” The result would be that the period of the year over the past ~6,000 years would have shortened by six weeks and that the Earth too would be constantly bombarded by meteors (although some especially strong meteor showers at that time lent some credence to this).

The only strong candidate left was that of gravitational contraction proposed by Sir William Thomson (later Lord Kelvin) and Hermann von Helmholtz in a series of papers they began publishing in 1854. But in 1859, Darwin published the Origin of Species in which he required an age of at least two billion years. Thomson’s and Helmholtz’s hypothesis could only support an age of some tens of millions of years. Thus astronomy and biology were brought head to head. Darwin was fully aware of this problem. In a letter to a friend, he wrote that, “Thomson’s views of the recent age of the world have been for some time one of my sorest troubles”.

To back the astronomers was the developing field of spectroscopy in which they determined that the sun and other stars bared a strong similarity to that of nebulae. These nebulae could contract under their own gravity and as such, provided a natural establishment for the formation of stars, leading gracefully into the contraction hypothesis. Although not mentioned in the article, Darwin did have some support from geologists like Charles Lyell who studied the formation of mountain ranges and also posited an older Earth.

Some astronomers attempted to add other methods in addition to gravitational contraction (such as tidal friction) to extend the age of the solar system, but none could reach the age required by Darwin. Similarly, some biologists worked to speed up evolutionary processes by positing separate events of abiogenesis to shave off some of the required time for diversification of various kingdoms. But these too could not rectify the problem.

Ultimately, the article throws its weight in the camp of the doomed astronomers. Interestingly, much of the same rhetoric in use by anti-evolutionists today can be found in the article. They state, “it is not surprising to find men of science, who not only have not the slightest doubt about the truth of their own pet theories, but are ready to lay down the law in the realms of philosophy and theology, in science which with, to judge from their immoderate assertions, their acquaintance is of the most remote? Such language is to be expected from the camp-followers in the army of science, who assurance is generally inversely proportional to their knowledge, for many of those in a word who affect to popularize the doctrine of Natural Selection.”

In time, Darwin would win the battle as astronomers would realize that gravitational contraction was just the match that lit the fuse of fusion. However, we must ask whether scientists would have been as quickly able to accept the proposition of stellar fusion had Darwin not pointed out the fundamental contradiction in ages?

Qatar Led Team Discovers Exoplanet

When listing the major scientific powers, the tiny nation of Qatar is not one that generally comes to mind. However, a Qatar astronomer, partnered with teams from the Harvard-Smithsonian Center for Astrophysics (CfA) as well as other institutions has just discovered a new exoplanet, dubbed Qatar-1b.

The planet itself, is another in the class of hot Jupiters which are massive, gassy planets that orbit their stars extremely closely. It has an orbital period of 1.4 days and is expected to be tidally locked with its parent star, a K type star.

It was discovered by a set of wide angle cameras located in New Mexico which are capable of surveying a large number of stars at a single time. The goal was to find planets that eclipsed the parent star and would thus show regular variations in their light curve. Images taken from this system were then sent to teams working at Universities in St. Andrews, Leicester, and Qatar. These teams processed the images and narrowed the stars down to a list of a few hundred candidates to be studied further.

From there Dr. Khalid Al Subai as well as the Harvard CfA team used the Smithsonian’s Whipple 48-inch telescope to more accurately measure the transits as well as as their 60-inch telescope to make spectroscopic observations to weed out binary star systems. These observations confirmed the existence of the planet.

“The discovery of Qatar-1b is a great achievement — one that further demonstrates Qatar’s commitment to becoming a leader in innovative science and research,” said Al Subai. Indeed, in the past 15 years, Qatar has undergone a large revolution towards science and education. Many universities have begun to open remote campuses, including Carnegie Mellon and Texas A&M. A more comprehensive list of science initiatives can be found here.

“The discovery of Qatar-1b is a wonderful example of how science and modern communications can erase international borders and time zones. No one owns the stars. We can all be inspired by the discovery of distant worlds,” said CfA team member David Latham.

Ancient Eclipse-Predicting Computer Rebuilt in Lego

I grew up playing with Legos, but never constructed anything like this! Andrew Carol built a replica of the The Antikythera Mechanism, the oldest known scientific computer, which was built in Greece probably around 100 BCE. No one in the current age knew about it until it was recovered from a shipwreck in 1901. Even then, it took a century until anyone could figure out what it was: an astronomical clock that determines the positions of celestial bodies with extraordinary precision. It is an analog computer with over 100 gears and 7 differential gearboxes, and is accurate to a day or two over its range.
Continue reading “Ancient Eclipse-Predicting Computer Rebuilt in Lego”

Asteroid Scheila Sprouts a Tail and Coma

(596) Scheila, the asteroid with a tail. Image credit: Peter Lake

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When is an asteroid not an asteroid? When it turns out to be a comet, of course. Has this ever happened before? Why, yes it has. In fact it was just announced December 12, 2010 that the asteroid (596) Scheila has sprouted a tail and coma! This is likely a comet that has been masquerading as an asteroid.

Taken from New Mexico Skies between 8h15m and 11h45m UT. The image is a stack of 10 x 600 sec exposures using a 20 inch RCOS and STL11K camera. Scale is 0.91 asec/px.. Image courtesy of Joseph Brimacombe

See an animation by Joseph Brimacombe at this link.

Steve Larson of the Lunar and Planetary Laboratory (LPL), University of Arizona first reported that images of the minor planet (596) Scheila taken on December 11th showed the object to be in outburst, with a comet-like appearance and an increase in brightness from magnitude 14.5 to 13.4. The cometary appearance of the object was confirmed by several other observers within hours.

A quick check of archived Catalina images of Scheila from October 18, November 2 and November 11 showed Scheila to look star-like, which is what asteroids look like from Earth. They just happen to be moving across the field of view in contrast to the fixed background stars. The image taken by Catalina on December 3rd shows some slight diffuseness and an increase in overall brightness. So, it appears this event began on or around December 3rd.

Upon hearing the news, there was some speculation that this might be evidence of an impact event. Had something crashed into asteroid Scheila? It seems unlikely, and this is a story we have heard before.

The asteroid discovered in 1979 and named 1979 OW7 was lost to astronomers for years and then recovered in 1996. It was subsequently renamed 1996 N2. That same year it was discovered to have a comet-like appearance, and many believed this was the signature of an impact between two asteroids. After years of inactivity 1996 N2 sprouted a tail again in 2002. One collision between two asteroids was unlikely enough. The odds of it happening again to the same object were essentially zero. What we had was a comet masquerading as an asteroid. This object is now known by its cometary name 133P/Elst-Pizarro, named after the two astronomers who discovered its initial cometary outburst.

The 2002 outburst and the discovery of more active asteroids showing mass-loss led to a paper (Hsieh and Jewitt 2006, Science, 312, 561-563) introducing an entirely new class of solar system objects, Main Belt Comets (MBC). MBCs look like comets because they show comae and have tails but they have orbits inside Jupiter’s orbit like main belt asteroids.

The most likely cause of the mass loss activity in MBCs is sublimation of water ice as the surface of the MBC is heated by the Sun. This is suggested most strongly by the behavior of the best-studied example, namely 133P/Elst-Pizarro. Its activity is recurrent, and it is strongest near and after perihelion, the point in its orbit nearest the Sun, like other comets.

MBCs are interesting to astronomers because they appear to be a third reservoir of comets in our solar system, distinct from the Oort cloud and Kuiper belt. Since we know of no way for these other reservoirs to have deposited comets in the inner solar system, the ice in MBCs probably has a different history than the ice in the outer comets. This allows researchers to study the differences in the Sun’s proto-planetary disk at three separate locations. This might lead to information on the Earth’s oceans, one of the continuing lines of investigation by solar system scientists.

Now it seems we have another MBC to add to the sample. And Scheila will probably be getting a new name soon. Asteroid (596) Scheila was discovered Feb. 21, 1906, by A. Kopff at Heidelberg. The 113Km in diameter ‘asteroid’ was named after an acquaintance, an English student at Heidelberg. In the future it will be called XXXP/Lawson or something similar, and Kopff’s Scheila will become just another footnote in the history of astronomical nomenclature.