Posted on by Fraser Cain

Hubble Identifies the Oldest Known Planet

Image credit: Hubble

The Hubble Space Telescope was recently used to identify the oldest extrasolar planet ever discovered. The 2.5 Jupiter mass planet was originally discovered around a pulsar in the globular cluster M4 way back in 1988; astronomers detected a regular dimming of the pulsar’s radio wave emissions. By using Hubble, astronomers were better able to explain how the planet ended up around a pulsar. This discovery could reshape the current models of planetary development, which predicted that stars needed to go through at least one complete cycle to create the heavier elements that planets require.

Long before our Sun and Earth ever existed, a Jupiter-sized planet formed around a sun-like star. Now, 13 billion years later, NASA’s Hubble Space Telescope has precisely measured the mass of this farthest and oldest known planet. The ancient planet has had a remarkable history because it has wound up in an unlikely, rough neighborhood. It orbits a peculiar pair of burned-out stars in the crowded core of a globular star cluster.

The new Hubble findings close a decade of speculation and debate as to the true nature of this ancient world, which takes a century to complete each orbit. The planet is 2.5 times the mass of Jupiter. Its very existence provides tantalizing evidence that the first planets were formed rapidly, within a billion years of the Big Bang, leading astronomers to conclude that planets may be very abundant in the universe.

The planet now lies in the core of the ancient globular star cluster M4, located 5,600 light-years away in the summer constellation Scorpius. Globular clusters are deficient in heavier elements because they formed so early in the universe that heavier elements had not been cooked up in abundance in the nuclear furnaces of stars. Some astronomers have therefore argued that globular clusters cannot contain planets. This conclusion was bolstered in 1999 when Hubble failed to find close-orbiting “hot Jupiter”-type planets around the stars of the globular cluster 47 Tucanae. Now, it seems that astronomers were just looking in the wrong place, and that gas-giant worlds orbiting at greater distances from their stars could be common in globular clusters.

“Our Hubble measurement offers tantalizing evidence that planet formation processes are quite robust and efficient at making use of a small amount of heavier elements. This implies that planet formation happened very early in the universe,” says Steinn Sigurdsson of Pennsylvania State University.

“This is tremendously encouraging that planets are probably abundant in globular star clusters,” says Harvey Richer of the University of British Columbia. He bases this conclusion on the fact that a planet was uncovered in such an unlikely place, orbiting two captured stars ? a helium white dwarf and a rapidly spinning neutron star ? near the crowded core of a globular cluster, where fragile planetary systems tend to be ripped apart due to gravitational interactions with neighboring stars.

The story of this planet’s discovery began in 1988, when the pulsar, called PSR B1620-26, was discovered in M4. It is a neutron star spinning just under 100 times per second and emitting regular radio pulses like a lighthouse beam. The white dwarf was quickly found through its effect on the clock-like pulsar, as the two stars orbited each other twice per year. Sometime later, astronomers noticed further irregularities in the pulsar that implied that a third object was orbiting the others. This new object was suspected to be a planet, but it could also be a brown dwarf or a low-mass star. Debate over its true identity continued through the 1990s.

Sigurdsson, Richer, and their co-investigators settled the debate by at last measuring the planet’s actual mass through some ingenious celestial detective work. They had exquisite Hubble data from the mid-1990s, taken to study white dwarfs in M4. Sifting through these observations, they were able to detect the white dwarf orbiting the pulsar and measure its color and temperature. Using evolutionary models computed by Brad Hansen of the University of California, Los Angeles, the astronomers estimated the white dwarf’s mass. This in turn was compared to the amount of wobble in the pulsar’s signal, allowing the astronomers to calculate the tilt of the white dwarf’s orbit as seen from Earth. When combined with the radio studies of the wobbling pulsar, this critical piece of evidence told them the tilt of the planet’s orbit, too, and so the precise mass could at last be known. With a mass of only 2.5 Jupiters, the object is too small to be a star or brown dwarf, and must instead be a planet.

The planet has had a rough road over the last 13 billion years. When it was born, it probably orbited its youthful yellow sun at approximately the same distance Jupiter is from our Sun. The planet survived blistering ultraviolet radiation, supernova radiation, and shockwaves, which must have ravaged the young globular cluster in a furious firestorm of star birth in its early days. Around the time multi-celled life appeared on Earth, the planet and star were plunging into the core of M4. In this densely crowded region, the planet and its sun passed close to an ancient pulsar, formed in a supernova when the cluster was young, that had its own stellar companion. In a slow-motion gravitational dance, the sun and planet were captured by the pulsar, whose original companion was ejected into space and lost. The pulsar, sun, and planet were themselves flung by gravitational recoil into the less-dense outer regions of the cluster. Eventually, as the star aged it ballooned to a red giant and spilled matter onto the pulsar. The momentum carried with this matter caused the neutron star to “spin-up” and re-awaken as a millisecond pulsar. Meanwhile, the planet continued on its leisurely orbit at a distance of about 2 billion miles from the pair (approximately the same distance Uranus is from our Sun).

It is likely that the planet is a gas giant, without a solid surface like the Earth. Because it was formed so early in the life of the universe, it probably doesn’t have abundant quantities of elements such as carbon and oxygen. For these reasons, it is very improbable the planet would host life. Even if life arose on, for example, a solid moon orbiting the planet, it is unlikely to have survived the intense X-ray blast that would have accompanied the spin-up of the pulsar. Regrettably, it is unlikely that any civilization witnessed and recorded the dramatic history of this planet, which began at nearly the beginning of time itself.

Original Source: Hubble News Release

Posted on by Fraser Cain

Rocket Telescope Gets a Look at the Sun

Image credit: NASA

Scientists got the best ever ultraviolet view of the Sun using a telescope and camera launched on board a sounding rocket. The pictures will help researchers understand how the Sun’s outer atmosphere heats up to over one million degrees Celsius. The telescope was able to resolve areas in the ultraviolet spectrum as small as 240 kilometres across; three times better than any space-based observatory. The rocket trajectory only let the telescope take 21 images during its 15 minute flight.

Scientists got their closest-ever ultraviolet look at the Sun from space, thanks to a telescope and camera launched aboard a sounding rocket. The images revealed an unexpectedly high level of activity in a lower layer of the Sun’s atmosphere (chromosphere). The pictures will help researchers answer one of their most burning questions about how the Sun works: how its outer atmosphere (corona) heats up to over one million degrees Celsius (1.8 million Fahrenheit), 100 times hotter than the chromosphere.

A team of Naval Research Laboratory (NRL) scientists used the Very high Angular resolution ULtraviolet Telescope (VAULT) to take pictures of ultraviolet (UV) light (1216 ?) emitted from the upper chromosphere. Resolving areas as small as 240 kilometers (150 miles or 0.3 arcseconds) on each side, the June 14, 2002, flight captured images about three times better than the previous-best pictures from space. A few ground-based telescopes can observe the Sun in 150-kilometer (93-mile) increments, but only at visible wavelengths of light. UV and X-ray wavelength observations most directly matter to solar weather.

Since most solar weather originates as explosions of the electrified gas (plasma) in the corona, understanding the heating and magnetic activity of the coronal plasmas will lead to better predictions of solar weather events. Severe solar weather, like solar flares and coronal mass ejections, can disrupt satellites and power grids, affecting life on Earth.

The VAULT observations reveal a highly structured, dynamic upper chromosphere, with structures visible for the first time thanks to the detailed resolution. A large number of structures in the pictures change rapidly from one image to the next, 17 seconds later. Scientists previously thought these changes occurred over five minutes or more. The transience of the physical processes in this layer has significant theoretical implications, such as the fact that proposed heating mechanisms must now also be effective over relatively short time scales.

Scientists found chromospheric features in the VAULT images that match features, based on shape and spatial correlation, which they see in Transition Region And Coronal Explorer (TRACE) satellite images of the corona taken simultaneously. This comparison shows that these two layers have much higher correlation than previously thought and implies that similar physical processes likely heat each. However, theory predicts the activity in the chromosphere should be lower than what scientists observed in the VAULT emissions. “[There are] more things happening below [in the upper chromosphere] than you see in the corona,” says VAULT project scientist Angelos Vourlidas of the NRL.

VAULT also revealed unexpected structures in quiet areas of the Sun. The plasma and magnetic field bubble up like boiling water on the Sun’s visible surface (photosphere), and, like bubbles gathering and forming a ring at the edge of a pot, the field builds up in rings (network cells) in the quiet areas. VAULT captured images of smaller features and significant activity within the network cells, surprising scientists.

The telescope took 21 images in the Lyman-alpha wavelength of the electromagnetic spectrum during a six-minute-nine-second picture-taking window on its 15-minute flight. Offering the brightest solar emissions, the Lyman-alpha wavelength assured the best likelihood for pictures from the rocket and allowed for shorter exposure times and more pictures. An increase in Lyman-alpha radiation may indicate an increase in solar radiation reaching Earth.

The VAULT payload consists of a 30-centimeter (11.8-inch) Cassegrain telescope with a dedicated Lyman-alpha spectroheliograph focusing images onto a charge-coupled device (CCD) camera. The CCD, also employed in consumer digital cameras, has a photosensitivity 320 times greater than photographic film previously used. The Normal Incidence X-ray Telescope (NIXT) from the Harvard-Smithsonian Center for Astrophysics took the previous best-resolution pictures of the Sun from space in September 1989, also aboard a sounding rocket.

The scientists verified the payload performance with an engineering flight from White Sands Missile Range, N.M., May 7, 1999. The June 14, 2002, flight from White Sands was the first scientific flight of the payload. The NRL team led a campaign combining observations from satellites and ground-based instruments. Scientists plan a third launch in Summer 2004. The mission was conducted through NASA’s Sounding Rocket Program.

Original Source: NASA News Release

Posted on by Fraser Cain

Book Review: Our Final Hour by Sir Martin Rees

It’s strange how many “the world is going to end” books cross my desk here at Universe Today. Our Final Hour: A Scientist’s Warning: How Terror, Error, and Environmental Disaster Threaten Humankind’s Future In This Century–On Earth and Beyond is the latest offering is by Sir Martin Rees, England’s Astronomer Royal, and delves into the possiblility that the fate of humanity, the Earth, and maybe even the entire universe is in the hands of well-intentioned (or malicious) scientists as they push the boundaries of nature.

Scientists will destroy the world! We’ve all heard that before, but found it kind of a strange statement coming from one of the more prominent scientists in the world. In “Our Final Hour”, however, Rees makes some well-reasoned arguments about the dangers of scientific exploration. Not that we shouldn’t explore nature, just that we should be mindful of the risks and take extra precautions.

The book is a quick read, only 228 pages, and takes us through the range of doomsday scenarios that scientists can unleash: environmental disasters that warm/cool the Earth and make it unlivable; bioterrorism that could unleash a plague of germs on the populace; and exotic physics experiments that could convert all matter in the universe into something… unpleasant.

Rees is calm and reasoned in his arguments; at no point does he stray into “science is bad” rants. Instead, he adopts the tone of a scientific professional, concerned about the ethical implications of scientific discovery. But he doesn’t argue that science should be slowed down, in fact, Rees believes that it’s pretty much impossible to stop scientific development. For every country that has a ban on genetic research, there will be one happy to support it. And technology will allow the tools to create viruses and other nastiness by a much larger group of people – some with nasty intentions.

I guess that’s where the book fell down a bit for me. It offers up lots challenges the world could face from science, but it’s short on solutions that could help guide policy. I got the impression that Rees feels largely pessimistic that anything can really be done to slow progress, and the inevitable disasters science could cause. It’s unrealistic to tell scientists what they can and can’t work on; even more difficult to enforce ethical guidelines; and probably impossible to stop technology from falling into the wrong hands. The only hope Rees sees is in human spaceflight – essentially escaping the problem and heading to the stars. That’s all well and good, but the Earth is where I keep all my stuff. There’s got to be more than that. I was hoping for a much longer book that offered up some deeper policy suggestions, but I suspect the implications are just too far reaching to make realistic suggestions.

Still, it’s an interesting read.

Here’s a link to Amazon.com, Amazon UK, and Amazon Canada.

Posted on by Fraser Cain

New Observatories Could Spot Waterworlds

Image credit: ESA

The European Space Agency is planning a series of space-based observatories designed to search space for evidence of Earth-like worlds. But an easier target to spot should be waterworlds; six times the mass of the Earth and covered with an ocean 100km deep. The CNES/ESA mission Corot will launch in 2005, and should just barely be able to spot dimming stars as these “waterworlds” pass in front. Even more powerful Eddington will launch in 2008 and should be able to see planets half the size of Earth. Finally, Darwin will launch in 2014 and search for signs of life on Earthlike planets.

Science fiction writers and movie-makers have imagined a world completely covered by an ocean, but what if one really existed? Would such a world support life, and what would this life be like?

ESA could make science fiction become science fact when it finds such a world, if the predictions of a group of European astronomers are correct. The ESA mission Eddington, which is now in development, could be the key.

At the recent ESA co-sponsored ‘Towards Other Earths’ conference, nearly 250 of the world’s leading experts in planet detection discussed the strategy for finding Earth-like worlds. Alain L?ger and colleagues of the Institut d’Astrophysique Spatiale, France, described a new class of planets that could be awaiting discovery: ‘waterworlds’.

According to L?ger and his colleagues, these waterworlds would contain about six times the mass of Earth, in a sphere twice as wide as our planet. They would possess atmospheres and orbit their parent star at roughly the same distance that the Earth is from the Sun. Most excitingly, an ocean of water entirely covers each world and extends over 25 times deeper than the average depth of the oceans on Earth.

A hundred kilometres deep
According to calculations, the internal structure of a waterworld would consist of a metallic core with a radius of about 4000 kilometres. Then there would be a rocky mantle region extending to a height of 3500 kilometres above the core?s surface, covered by a second mantle made of ice up to 5000 kilometres thick. Finally, an ocean blankets the entire world to a depth of 100 kilometres, with an atmosphere on top of this.

With twice the radius of the Earth, they will be easily spotted by the Eddington spacecraft, which is designed to detect planets down to half the size of the Earth. “A waterworld passing in front of a star, somewhat cooler than the Sun, will cause a dimming in the stellar light by almost one part in a thousand. That’s almost ten times larger than the smallest variation Eddington is designed to detect. So, waterworlds ? if they exist ? will be a very easy catch for Eddington,” says Fabio Favata, ESA?s Eddington Project Scientist.

The CNES/ESA mission Corot, which is a smaller, precursor mission to Eddington due for launch around 2005, may also be just able to glimpse them, if they are close enough to their parent stars.

Origins of life
Scientists are now asking if such worlds could support life, and what would it be like, especially since water is a prime ingredient for life on Earth. While waterworlds seem to have everything to sustain life, there is a big question mark over whether they could actually allow it to start in the first place.

One of the leading theories for life’s origin in deep oceans is that it requires hot springs on the ocean floor, heated by volcanic activity like the ‘black smokers’ found here on Earth. On a waterworld however, 5000 kilometres of ice separate the ocean floor from any possible smokers. On the other hand, a water-surface origin may still be possible.

Perhaps the only way to know if anything lives on a waterworld will be to study them with ESA’s habitable-planet-finding mission, Darwin. When it launches in around 2014, this flotilla of spacecraft will look for tell-tale signs of life in the atmospheres of any planets, including waterworlds.

Original Source: ESA News Release

Posted on by Fraser Cain

How the Owl Nebula Got its Shape

Image credit: Hubble/NOAO

A team of astronomers have created a model to explain how the Owl Nebula (NGC 3587) got its unique shape. They believe that the outer halo was formed when the star first lost mass and blew off its outer layer; the circular middle shell was caused by solar wind from the star blowing additional material; and then an even faster solar wind created the inner layer. Other planetary nebulae show a similar triple-shell appearance, so it’s likely they formed the same way.

Astronomers have assembled the first effective model for both the shape and evolutionary history of the Owl Nebula, the well-known planetary nebula in the constellation Ursa Major.

Named for its ghostly similarity to the face of the carnivorous bird of prey, the Owl Nebula (NGC 3587) has a complex structure consisting of three concentric shells. The aptly named nebula boasts a faint outer halo, a circular middle shell, and a roughly elliptical inner shell. The inner shell houses a bipolar cavity that forms the owl?s ?eyes,? and two areas of enhanced brightness are seen as the owl?s ?forehead? and ?beak.?

In an article published in the June 2003 Astronomical Journal, researchers from the University of Illinois at Urbana-Champaign, the Instituto de Astrofisica de Canarias in Spain, and Williams College in Williamstown, MA, present the first cohesive model for the appearance and evolution of the Owl Nebula.

Using observations made with the William Herschel Telescope in La Palma, Spain, and the 0.6-meter Burrell Schmidt telescope at Kitt Peak National Observatory, the researchers concluded that the halo of the Owl was formed when the parent star first underwent significant mass loss after the cessation of fusion in its core. The resulting instabilities then produced a stellar wind, driven by a combination of stellar pulsations and radiation pressure.

Evolution of the Owl?s parent star caused the stellar wind to intensify to a ?superwind,? driving even more gas and dust outward to form the middle shell. A subsequent faster stellar wind compressed the superwind to form the inner shell and bipolar cavity, but that wind has since ceased. The cavity is currently being back-filled with nebular material in the absence of the fast stellar wind, much as air flows back out of a balloon if you stop blowing into it.

?Different evolutionary models can produce the same structure for the nebula, but until now none has been able to also account for its motion,? says Martin A. Guerrero of the University of Illinois, the lead author of the recent study. ?There are many investigations of physical structures of planetary nebulae, but most studies only look at one piece of data and tend to ignore the bigger picture.?

Other planetary nebulae show triple-shell structure similar to the Owl Nebula and it is likely that they followed this same evolutionary path, according to co-author Karen Kwitter of Williams College. ?These nebulae form an illuminating sample to study, and the Owl Nebula is the nearest one, only about 2,000 light-years from Earth.?

Despite the name, planetary nebulae are not related to planets. Sir William Herschel gave these fascinating objects their misleading name in 1782 because, through his telescope, they resembled the appearance of Uranus and Neptune. In reality, planetary nebulae are shells of gas and dust ejected from aging stars. When the mass loss is finished, the hot core of the star is exposed, causing the ejected gas to glow.

A newly processed image of the Owl Nebula from this study is available above.

The Burrell Schmidt telescope is part of the Warner and Swasey Observatory of Case Western Reserve University, Cleveland, OH. The telescope is located at Kitt Peak National Observatory near Tucson, AZ, which is part of the National Optical Astronomy Observatory (NOAO). NOAO is operated by the Association of Universities for Research in Astronomy (AURA) Inc., under a cooperative agreement with the National Science Foundation.

Original Source: NRAO News Release

Posted on by Fraser Cain

Discuss Articles on Universe Today

I’ve added a new feature to Universe Today: the ability for people to discuss stories posted on the website. If you look at today’s stories, you’ll see I added a “Discuss this story” link to each one. Click it and it’ll take you to a feedback page specifically for that story.

My hope is that people can use this mini-forum as a way to better understand the story. Ask questions, post your theories, and generally use it as a way to connect with other space fans. Of course, I’m sure it’ll also get used to catch my various typos. 🙂 I’ll be as active in the threads as I can, but I urge knowledgeable space experts to lend a hand answering people’s questions.

Please give me any feedback you may have about this.

Thanks!

Fraser Cain
Publisher
Universe Today

Posted on by Fraser Cain

Pluto’s Atmosphere is Expanding

Image credit: NASA

A team of astronomers from MIT reported today that Pluto’s atmosphere is expanding, even as the planet is getting further away from the Sun on its elliptical orbit. The team made their findings by watching the dimming of a star as Pluto passed in front. Astronomers were expecting to find the opposite situation; that its atmosphere would shrink as it gets further from the Sun, but it’s similar to the Earth, where early afternoon is hotter than noon, when the Sun is at its brightest. If all goes well, NASA will launch its New Horizons mission by 2006 to reach Pluto in 2015.

Pluto?s atmosphere is expanding even as it continues on its long orbit away from the sun, a team of astronomers from MIT, Boston University, Williams College, Pomona College, Lowell Observatory and Cornell University report in the July 10 issue of Nature.

The team, led by James Elliot, professor of planetary astronomy at MIT and director of MIT?s Wallace Observatory, made this finding by watching the dimming of a star when Pluto passed in front of it on Aug. 20, 2002. The team carried out observations using eight telescopes at Mauna Kea Observatory, Haleakala, Lick Observatory, Lowell Observatory and Palomar Observatory.

Elliot said the new results seem counterintuitive, because observers assumed Pluto?s atmosphere would begin to collapse as it cooled. In fact, the temperature of Pluto?s mostly nitrogen atmosphere has increased around 1 degree Celsius since it was closest to the sun in 1989.

Elliot attributes the increase to the same lag effect that we experience on Earth?even though the sun is most intense at its highest point at noon, the hottest part of the day is around 3 p.m. Because Pluto’s year is equal to 248 Earth years, 14 years after Pluto’s closest approach to the Sun is like 1:15 p.m. on Earth. At the rate of Pluto?s orbit, it may take another 10 years to cool down and would just be beginning to cool when the NASA New Horizons mission to Pluto, scheduled to be launched in 2006, reaches it in 2015.

Pluto?s predominantly nitrogen atmosphere is in vapor pressure equilibrium with its surface ice, and can therefore undergo large changes in pressure in response to small changes in surface ice temperature. As its icy surface gets colder, it condenses into fresh white frost that reflects more of the sun?s heat and gets colder still. As space dirt and objects collect on its surface, it darkens and absorbs more heat, accelerating the warming effect. Pluto has been darkening since 1954.

?The August 2002 data have allowed us to probe much more deeply into Pluto’s atmosphere and have given us a more accurate picture of the changes that have occurred,” Elliot said.

Pluto?s orbit is much more elliptical than that of the other planets, and its rotational axis is tipped by a large angle relative to its orbit. Both factors could contribute to drastic seasonal changes.

Since 1989, for example, the sun?s position in Pluto?s sky has changed by more than the corresponding change on the Earth that causes the difference between winter and spring. Pluto’s atmospheric temperature varies between around -235 and -170 degrees Celsius, depending on the altitude above the surface.

Pluto has nitrogen ice on its surface that can evaporate into the atmosphere when it gets warmer, causing an increase in surface pressure. If the observed increase in the atmosphere also applies to the surface pressure?which is likely the case?this means that the average surface temperature of the nitrogen ice on Pluto has increased slightly more than 1 degree Celsius over the past 14 years.

STUDYING ATMOSPHERES WITH SHADOWS
Researchers study faraway objects through occultations?eclipse-like events in which a body (Pluto in this case) passes in front of a star, blocking the star?s light from view. By recording the dimming of the starlight over time, astronomers can calculate the density, pressure and temperature of Pluto?s atmosphere.

Observing two or more occultations at different times provides researchers with information about changes in the planet?s atmosphere. The structure and temperature of Pluto?s atmosphere was first determined during an occultation in 1988. Pluto?s brief pass in front of a different star on July 19 led researchers to believe that a drastic atmospheric change was under way, but it was unclear whether the atmosphere was warming or cooling.

The data resulting from this occultation, when Pluto passed in front of a star known as P131.1, led to the current results. ?This is the first time that an occultation has allowed us to probe so deeply into Pluto’s atmosphere with a large telescope, which gives a high spatial resolution of a few kilometers,? Elliot said. He hopes to use this method to study Pluto and the Kuiper Belt objects more frequently in the future.

MISSION TO PLUTO
NASA recently authorized the New Horizons Pluto-Kuiper Belt mission to start building spacecraft and ground systems. The mission will be the first to Pluto and the Kuiper Belt. Richard P. Binzel, professor of earth, atmospheric and planetary sciences (EAPS) at MIT, is co-investigator.

The New Horizons spacecraft is scheduled to launch in January 2006, swing past Jupiter for a gravity boost and scientific studies in 2007, and reach Pluto and Charon moon of Pluto as early as summer 2015. Pluto is the only planet not yet observed at close range. This mission will seek to answer questions about the surfaces, atmospheres, interiors and space environments of the solar system?s outermost planet and its moon.

In the meantime, researchers hope to use SOFIA, a 2.5-meter telescope mounted in an aircraft being built by NASA in collaboration with the German space agency, starting in 2005. SOFIA would be able to be sent to the right location around the globe to best observe occultations, providing high-quality data on a much more frequent basis than is possible using ground-based telescopes alone.

In addition to Elliot, MIT co-authors are recent physics graduate Kelly B. Clancy; graduate students Susan D. Kern and Michael J. Person; recent MIT graduate Colette V. Salyk; and aeronautics and astronautics senior Jing Jing Qu.

The Williams College collaborators included Jay M. Pasachoff, professor of astronomy; Bryce A. Babcock, staff physicist; Steven V. Souza, observatory supervisor; and undergraduate David R. Ticehurst. They used the University of Hawaii’s telescope at the 13,800-foot altitude of the Hawaiian volcano Mauna Kea and a Williams College electronic detector normally part of eclipse expeditions.

Pomona College collaborators are Alper Ates and Ben Penprase. The Boston University collaborator is Amanda Bosh. Lowell Observatory collaborators are Marc Buie, Ted Dunham, Stephen Eikenberry, Cathy Olkin, Brian W. Taylor, and Lawrence Wasserman. Boeing collaborators are Doyle Hall and Lewis Roberts.

The United Kingdom Infrared Telescope collaborator is Sandy K. Leggett. U.S. Naval Observatory collaborators are Stephen E. Levine and Ronald C. Stone. The Cornell collaborator is Dae-Sik Moon. David Osip and Joanna E. Thomas-Osip were at MIT and are now at the Carnegie Observatories. John T. Rayner is at NASA’s Infrared Telescope Facility. David Tholen is at the University of Hawaii.

This work is funded by Research Corp., the Southwest Research Institute, the National Science Foundation and NASA.

Original Source: MIT News Release

Posted on by Fraser Cain

Beagle 2 Tests Complete

Image credit: ESA

The European Space Agency has been testing all aspects of the Mars Express spacecraft to ensure that it’s ready for its encounter with Mars. This week they put the UK-built Beagle 2 lander through its paces. The tests included uploading software and turning various instruments on and off, and everything seems to be working properly. A final series of tests will be done in mid-July. Mars Express is expected to reach the Red Planet on December 19 – Beagle 2 will land on the surface on December 25.

On Friday 4 July, and Saturday 5 July 2003, engineers successfully carried out overnight tests on the Mars Express lander, Beagle 2.

Ground controllers at the European Space Agency’s Operations Centre in Darmstadt, Germany, contacted Mars Express at the weekend to carry out the tests on the lander, which were rescheduled from two weeks ago. These functional tests included uploading software and switching units on and off.

With these tests, the near-Earth phase of the Mars Express payload check-outs is almost complete. All instruments, including the lander, have performed as expected. Star calibration of some instruments is scheduled for mid-July, which marks the first attempt to make scientific measurements. This will also be done in the same way when nearer to Mars.

Rudi Schmidt, ESA Mars Express Project Manager, said: “This check-out was a marvellous example of complete cooperation between ESA?s Mars Express and the Beagle lander teams Another major milestone has been achieved successfully. What a fantastic feeling!”

Original Source: ESA News Release

Posted on by Fraser Cain

Hot Gases Breached a Shuttle Back in 2000

NASA has released photographs that show how the space shuttle Atlantis suffered damage from hot gases back in May 2000 when it returned through the atmosphere on a mission. The damage wasn’t permanent and repaired in time for its next mission four months later. NASA blamed the damage on improper installation of a seal between protective panels on the shuttle’s left wing. Atlantis is expected to be the first shuttle to return to space when NASA begins launches again in early 2004.

Posted on by Fraser Cain

X-Prize Entrant Completes Drop Test

Image credit: Armadillo Aerospace

Texas-based Armadillo Aerospace successfully performed a helicopter drop test on a component of their spacecraft on Sunday. Armadillo is just one of the teams competing for the X-Prize, which will pay $10 million to the first private space ship capable of lifting three people to an altitude of 100km. The company is led by John Carmack, who’s better known as the founder of id software – creators of the popular video games Doom and Quake.

We finished up all of the prep work for the vehicle on Tuesday. We welded in strapping points to hold 600 pounds of ?passenger? sandbags in the cabin area, and we mounted five 45 pound Olympic barbell plates on a peg at the end to simulate the weight of the final engines, plumbing, and backup recovery system that will be on the full size vehicle. We mounted four 2? throat engine shells as placeholders. Total weight is just under 2400 pounds. We use a combination of multiple chain hoists, a palette jack, and a forklift to move the full vehicle around and get it up on the trailer, but we did wind up breaking one of the castor wheels that we had mounted on our tank cradle. If we wind up having to use the 1600 gallon propellant tank (the current one is 850 gallons), we aren?t going to be able to stand the vehicle up under the main girder inside our shop, which will be inconvenient.

On Saturday, we headed out to our test site for the drop test. There were quite a few stares on the road in transit? We had a few spatters of rain, and the wind occasionally gusted to 12 knots, but we were able to perform the drop in relatively calm 6 knot winds.

Anna rented a big RV for the day, which was very worthwhile. It was nice to be able to take a break in an air-conditioned space.

5 State Helicopters arrived with a big Sikorsky for the lifting. It was very convenient that they were based close by, and didn?t have a problem with our unusual application (although they did have us contact the local mayor and sheriff for explicit permission). We were very impressed with the precision that they were able to do the lifting ? we were afraid that the vehicle might get dragged or bounced on the crush cone, which could buckle it before the test even started, but they were able to perfectly pivot it up on the nose, and gently lift it off the ground. If we had known they were that precise, we probably could have skipped renting the forklift truck for recovery and just had them lower the rocket back onto the trailer after the test.

We made several 18? diameter test parachutes that were weighted to drift at about the same rate that the full size parachute was expected to fall. We did the test drop from 1500? AGL, under the assumption that the big vehicle would fall several hundred feet before the main chute was fully deployed. The landing point for the test parachute was satisfactory, so we planned the full vehicle drop for 2000? AGL. Neil rode in the helicopter to do the parachute releasing, and Anna hung out the side of the helicopter (with a safety strap) to get aerial footage.

We had to abort our first attempt to drop the vehicle, because the line that we ran from the helicopter to the Sea-Catch toggle release above the rocket had wrapped itself around the chain so many times that Neil couldn?t pull it hard enough to trigger the release. This was fixed by tying loose loops of plastic every few feet along the chain, which kept the pull-line in place.

On the second try, the release worked perfectly. You can clearly see the naturally unstable aerodynamics of the vehicle, as it starts to tip over almost immediately after release. We all held our breath as it started to fall, but the drogue immediately inflated and started pulling the main canopy out. It was nine seconds from release to full canopy inflation. The opening shock was negligible, barely hitting 2G?s. For high altitude flights, we are aiming for a 200 mph terminal velocity under the stabilizer drogue at the time of main canopy deployment, so opening shock will be much greater then.

The wake of the main canopy is so great that the deployment drogue just rests on the canopy during descent, without any inflation at all. The real deployment system will have a much longer line on the drogue (because it is used for vehicle stabilization before deploying the main), which will probably cause it to trail behind the main chute, still inflated.

The drift was going about where we expected, but we were a little concerned when we saw that the vehicle was oscillating +/- 13 degrees under the canopy, which is a pretty big swing at that length. The actual landing point was unfortunately just behind some low foliage, so we didn?t get a perfect shot of it, but we did see it hit at enough of an angle that it rolled almost back upright as it landed.

We ran over to collapse the chute and examine the state of the vehicle. The crush cone had buckled right at the mounting point from the angled impact, but the vehicle looked basically sound. None of the sandbags in the cabin had broken open. Two of the engine support studs were bent from when it tipped back up.

We had the helicopter pick it back up and drop it off by the trailer, which was a lot more convenient than driving the lift truck over to the vehicle.

When we got it back to the shop, we pulled some things apart to take a closer look. The bent mounting studs unscrewed right out of their mounts, so replacing those is trivial. We are considering adding some more bracing below the engine plates, which would probably keep them from bending at all. When we got the crush cone off, we did find that the cabin had been bent right at the end of the cone, and the buckle in the crush cone had pushed in far enough to crease the honeycomb bulkhead.

We are probably going to continue using this cabin for the first couple flights of the big vehicle, but start on a second-generation cabin structure that will incorporate some improvements for off-angle landings, as well as several other lessons we have learned in working with the current cabin. Because we bonded a mounting flange to the tank, we should be able to simply swap the cabin when we want to.

The accelerometer data showed 10G acceleration peaks during the landing and bounce, which is over twice what we saw with the straight down drop tests that collapsed perfectly. This is still acceptable, although bouncing up and back down in the cabin would have been a pretty harsh ride. Making some changes to the vehicle structure will improve the behavior of the crush cone and over tipping effects, and we are going to see if Strong Enterprises can do anything with the canopy design to reduce the oscillations during descent.

Overall, the operation was a good success, and demonstrates that recovering the complete vehicle after flight should work fine.

Original Source: Armadillo Aerospace News Release