Posted on by Mark Mortimer

Book Review: Practical Astronomy

The first half of the book is a reference source for how to observe. With good sense, it gives credit to the unaided eye and it extols the benefits of quickly and easily orienting yourself amongst the limitless dots and streaks in the black canopy of night. Visual aids are described. Telescope types; refractor, reflector and catadioptric, are compared. Ancillary equipment from red lights, to telescope drives to planispheres are also discussed. There are star charts (white dot on blue background) for the complete sky, that is both northern and southern hemispheres. These charts show stars up to magnitude 5 as well as the constellations and their boundaries. This half of the book also includes a section on how to locate the constellations and many of the most significant stars using the altazimuthal system, celestial coordinates, and/or from starting from other, easy to find sights such as Orion.

The second half of the book categorizes the sources of light from near Earth outwards. It starts with meteors, satellites and auroras, then to the Moon, the Sun, and through each of the planets. The final section looks at star clusters, binary stars and nebulae. There is even a brief discussion of galaxies and some exciting amateur prints of them. Rather than solely stating where to find each object, this half discusses characteristics of interest (e.g. the cusps of Venus), noteworthy events (e.g. occultations) and effects in time (e.g. variable stars). Throughout this half the author emphasizes the benefits of recording observations, such as by sketching. This is both for self-satisfaction and as a means of proving observations of an original event.

I like this book as it explains all the necessary fundamentals for sky watching. Without costing more than the price of this text, a person can occupy themselves for a long time in getting acquainted with the sights and events that occur while most everyone else is safely tucked into bed. Sometimes I did find the text a little difficult to follow especially with some of the explanations. Yet there are many prints and drawings that provide a lot of clarity. Also, there are enough inline references throughout the text to aid in following any particular topic.

In all, Practical Astronomy is a great reference for getting a person started onto the road of understanding the night sky and enjoying a pastime that keeps many night owls happily occupied.

Buy this book and others from Amazon.com

Review by Mark Mortimer

Posted on by Fraser Cain

Aura Satellite Delivered to Launch Facility

Image credit: NASA/JPL
NASA’s Aura spacecraft, the latest in the Earth Observing System series, has arrived at Vandenberg Air Force Base, Calif., to begin launch preparations.

Aura was transported from Northrop Grumman’s Space Park manufacturing facility in Redondo Beach, Calif. The spacecraft will undergo final tests and integration with a Boeing Delta II rocket for a scheduled launch in June.

Aura’s four state-of-the-art instruments, including two built and managed by NASA’s Jet Propulsion Laboratory, Pasadena, Calif., will study the atmosphere’s chemistry and dynamics. The spacecraft will provide data to help scientists better understand Earth’s ozone, air quality and climate change. JPL’s Tropospheric Emission Spectrometer is an infrared sensor designed to study Earth’s troposphere-the lowest region of the atmosphere-and to look at ozone. JPL’s Microwave Limb Sounder is an instrument intended to improve our understanding of ozone in Earth’s stratosphere, vital in protecting us from solar ultraviolet radiation.

“The entire Aura team is very excited to see all our efforts come to fruition and is looking forward to a successful launch,” said Rick Pickering, Aura project manager at NASA’s Goddard Space Flight Center in Greenbelt, Md.

Aura fulfills part of NASA’s commitment to study Earth as a global system and represents a key agency contribution to the U.S. Global Change Research Program. This mission will continue the global data collection underway by NASA’s other Earth Observing System satellites: Terra, which monitors land; and Aqua, which observes Earth’s water cycle.

The Aura spacecraft is part of NASA’s Earth Science Enterprise, a long-term research effort to determine how human-induced and natural changes affect the global environment.

For more information about Aura on the Internet, visit http://aura.gsfc.nasa.gov . For more information about the Tropospheric Emission Spectrometer on the Internet, visit http://tes.jpl.nasa.gov/ . For more information about the Microwave Limb Sounder on the Internet, visit http://mls.jpl.nasa.gov/ .

Original Source: NASA/JPL News Release

Posted on by Fraser Cain

Outer Planets Could Warm Up as Sun Dies

Image credit: NASA
We are doomed. One day the Earth will be a burnt cinder orbiting a swollen red star.

This is the ultimate fate of any planet living close to a main sequence star like our sun. Main sequence stars run on hydrogen, and when this fuel runs out, they switch over to helium and become a red giant. While the sun’s transition into a red giant is sad news for Earth, the icy planets in the most distant regions of our solar system will bask in the sun’s warmth for the first time.

The sun has been slowly but steadily growing brighter and hotter over the course of its lifetime. When the sun becomes a red giant in about 4 billion years, our familiar yellow sun will turn a vivid red, as it mainly emits the lower frequency energy of infrared and visible red light. It will grow thousands of times brighter and yet have a cooler surface temperature, and its atmosphere will expand, slowly engulfing Mercury, Venus and possibly even the Earth.

While the sun’s atmosphere is predicted to reach Earth’s orbit of 1 AU, red giants tend to lose a lot of mass, and this wave of expelled gases could push Earth just out of range. But whether the Earth is consumed or merely singed, all life on Earth will have passed into oblivion.

Yet the conditions that make life possible could appear elsewhere in the solar system, according to a paper published in the journal Astrobiology by S. Alan Stern, Director of the Southwest Research Institute’s Department of Space Studies in Boulder, Colorado. He says that planets located 10 to 50 AU will be in the red giant sun’s habitable zone. The habitable zone of a solar system is the region where water can remain in a liquid state.

The habitable zone will shift gradually through the 10 to 50 AU region as the sun grows brighter and brighter, evolving through its red giant phase. Saturn, Uranus, Neptune and Pluto all lie within 10 to 50 AU, as do their icy moons and the Kuiper Belt Objects. But not all these worlds will have an equal chance at life.

The prospects for habitability on the gaseous planets Saturn, Neptune and Uranus may not be affected all that much by the red giant transition. Astronomers have discovered gaseous planets orbiting very close to their parent star in other solar systems, and these “hot Jupiters” seem to hold onto their gaseous atmospheres despite their proximity to the intense radiation. Life as we know it is not likely to appear on gaseous planets.

Stern thinks Neptune’s moon Triton, Pluto and its moon Charon, and the Kuiper Belt Objects will have the best chances for life. These bodies are rich in organic chemicals, and the heat of the red giant sun will melt their icy surfaces into oceans.

“When the sun is a red giant, the ice worlds of our solar system will melt and become ocean oases for tens to several hundreds of millions of years,” says Stern. “Our solar system will then harbor not one world with surface oceans, as it does now, but hundreds, for all of the icy moons of the giant planets, and the icy dwarf planets of the Kuiper Belt will also bear oceans then. Because temperature on Pluto will not be very different then, than Miami Beach’s temperature now, I like to call these worlds ‘warm Plutos,’ in analogy to the plethora of hot Jupiters found orbiting sun-like stars in recent years.”

The influence of the sun is not the whole story, however – the characteristics of a planetary body go a long way toward determining habitability. Such characteristics include a planet’s internal activity, the reflectivity, or “albedo” of a planet, and the thickness and composition of the atmosphere. Even if a planet has all the elements that favor habitability, life will not necessarily appear.

“We don’t know what is needed to start life,” says Don Brownlee, an astronomer with the University of Washington in Seattle and co-author of the book, “The Life and Death of Planet Earth.” Brownlee says that if warm wet interiors and organic materials are all that’s needed, then Pluto, Triton, and the Kuiper Belt Objects could harbor life.

“As a word of caution, however, the interiors of asteroids that produced the carbonaceous chondrite meteorites were warm and wet for perhaps millions of years in the early history of the solar system,” says Brownlee. “These bodies are extremely rich in both water and organic materials, and yet there is no compelling evidence that any asteroidal meteorite ever had living things in it.”

A planetary body’s orbit also will affect its chances for life. Pluto, for instance, doesn’t have a nice, regular orbit like the Earth. The orbit of Pluto is comparatively eccentric, varying in distance from the sun. From January 1979 through February 1999, Pluto was closer to the sun than Neptune, and in a hundred years, it’ll be almost twice as far out as Neptune. This type of orbit will cause Pluto to undergo extreme heating alternating with extreme cooling.

Triton’s orbit, too, is peculiar. Triton is the only large moon to orbit backwards, or “retrograde.” Triton may have this unusual orbit because it formed as a Kuiper Belt Object and then was captured by Neptune’s gravity. It’s an unstable alliance, since the retrograde orbit creates tidal interactions with Neptune. Scientists predict that someday Triton will either crash into Neptune, or break up into tiny pieces and form a ring around the planet.

“The timescale for the tidal decay of Triton’s orbit is uncertain, so it could be around, or it might have already crashed by the time the sun goes red giant,” says Stern. “If Triton is around, it’ll probably end up looking like the same kind of organic-rich ocean world as Pluto.”

The sun will burn as a red giant for about 250 million years, but is that enough time for life to get a foothold? During most of the red giant lifetime, the sun will be only 30 times brighter than its current state. Toward the end of the red giant phase the sun will grow more than 1,000 times brighter, and occasionally release pulses of energy reaching 6,000 times current brightness. But this period of intense brightness will last for a few million years, or tens of millions of years at most.

The brevity of the red giant’s brightest phases suggests to Brownlee that Pluto doesn’t hold much promise for life. Because of Pluto’s average orbit of 40 AU, the sun would have to be 1,600 times brighter for Pluto to get the same solar radiation we currently get on Earth.

“The sun will reach this brightness, but only for a very brief period of time – only a million years or so,” says Brownlee. “The surface and atmosphere of Pluto will be ‘improved’ from our point of view, but it won’t be a nice place for any significant period of time”.

After the red giant phase, the sun will become fainter, and will shrink to the size of the Earth, becoming a white dwarf. The distant planets that basked in the light of the red giant will become frozen ice worlds once again.

So if life is to appear in a red giant system, it will need a quick start. Life on Earth is thought to have originated 3.8 billion years ago, some 800 million years after our planet was born. But that is probably because the planets in the inner solar system experienced 800 million years of heavy asteroid bombardment. Even if life had gotten started immediately, the early rain of asteroids would’ve wiped the Earth clean of that life.

Brownlee says a new era of bombardment could begin for the outer planets, because the red giant sun could disturb the vast number of comets in the Kuiper Belt.

“When the red giant sun is 1,000 times brighter, it loses almost half of its mass to space,” says Brownlee. “This causes orbiting bodies to move outward. Gas loss and other effects might destabilize the Kuiper Belt and create another period of interesting bombardment.”

But Stern says that planets made habitable by a red giant sun won’t be bombarded as often as the early Earth was, because the ancient asteroid belt had much more material than the Kuiper Belt has today.

In addition, the outer planets won’t experience the same ultraviolet (UV) levels that Earth has had to endure, since red giants have very low UV radiation. The higher intensity UV of a main sequence star can be damaging to the delicate proteins and RNA strands needed for life’s origin. Life on Earth could only originate underwater, in depths protected from this light intensity. Life on Earth is therefore inextricably linked to liquid water. But who knows what sort of life might originate on planets that have no need for UV shielding?

Stern thinks we should look for evidence of life on Pluto-like worlds orbiting around red giants today. We currently know of 100 million solar-type stars in the Milky Way galaxy that burn as red giants, and Stern says that all of these systems could have habitable planets within 10 to 50 AU. “It would be a good test of the time required to create life on warm, water-rich worlds,” he says.

“The idea of organic-rich distant bodies getting baked by a red giant star is an intriguing one, and could provide very interesting if short-lived habitats for life,” adds Brownlee. “But I am glad that our sun has a good margin of time left.”

What’s Next
While much of what we know about the outer solar system is based on distant measurements made from Earth-based telescopes, on January 2, 2004, scientists caught a close-up glimpse of a Kuiper Belt Object. The Stardust spacecraft passed within 136 kilometers of comet Wild2, an enormous snowball that spent most of its 4.6 billion-year lifetime orbiting in the Kuiper Belt. Wild2 now orbits mostly inside the orbit of Jupiter. Brownlee, who is the Principle Investigator for the Stardust mission, says that the Stardust images show fantastic surface details of a body shaped both by its ancient and recent history. Stardust images show gas and dust jets shooting off the comet, as Wild2 rapidly disintegrates in the strong solar heat of the inner solar system.

To learn more about the outer solar system, we’ll need to send a spacecraft out there to investigate. In 2001, NASA selected the New Horizons mission for just such a purpose.

Stern, who is the Principal Investigator for the New Horizons mission, reports that the spacecraft assembly is scheduled to begin this summer. The spacecraft is due to launch in January 2006, and arrive at Pluto the summer of 2015.

The New Horizons mission will allow scientists to study the geology of Pluto and Charon, map their surfaces, and take their temperatures. Pluto’s atmosphere also will be studied in detail. In addition, the spacecraft will visit the icy bodies in the Kuiper Belt in order to make similar measurements.

Original Source: Astrobiology Magazine

Posted on by Fraser Cain

Genesis Prepares to Return to Earth

Image credit: NASA/JPL
Since October 2001 NASA’s Genesis spacecraft has exposed specially designed collector arrays of sapphire, silicon, gold and diamond to the Sun’s solar wind.

That collection of pristine particles of the Sun came to an end last week, when NASA’s Genesis team at the Jet Propulsion Laboratory in Pasadena, Calif., ordered the spacecraft’s collectors deactivated and stowed. The closeout process was completed when Genesis closed and sealed the spacecraft’s sample-return capsule.

“This is a momentous step,” said Genesis project manager Don Sweetnam. “We have concluded the solar-wind collection phase of the mission. Now we are focusing on returning to Earth, this September, NASA’s first samples from space since Apollo 17 back in December 1972.”

NASA’s Genesis mission was launched in August 2001 from the Cape Canaveral Air Force Station, Fla. Three months and about one million miles later, the spacecraft began to amass solar wind particles on hexagonal wafer-shaped collectors made of pure silicon, gold, sapphire and diamond.

“The material our collector arrays are made of may sound exotic, but what is really unique about Genesis is what we collected on them,” said mission principal investigator Don Burnett. “With Genesis we’ve had almost 27 months far beyond the Moon’s orbit collecting atoms from the Sun. With data from this mission, we should be able to say what the sun is composed of at a level of precision for planetary science purposes that has never been seen before.”

To get Genesis’ precious cargo into the sterilized-gloved hands of Burnett and solar scientists around the world is an exotic endeavor in itself.

Later this month, Genesis will execute the first in a series of trajectory maneuvers that will place the spacecraft on a route toward Earth. On Sept. 8, 2004, the spacecraft will dispatch a sample-return capsule containing its solar booty. The capsule will re-enter Earth’s atmosphere for a planned landing at the U.S. Air Force Utah Test and Training Range at about 9:15 a.m. EDT.

To preserve the delicate particles of the Sun in their prisons of gold, sapphire and diamond, specially trained helicopter pilots will snag the return capsule from mid-air using giant hooks. The flight crews for the two helicopters assigned for the capture and return of Genesis are former military aviators, Hollywood stunt pilots and an active-duty Air Force test pilot.

For information about NASA and agency missions on the Internet, visit http://www.nasa.gov . For information about Genesis on the Internet, visit http://genesismission.jpl.nasa.gov/ . For information about the capture-and-return process on the Internet, visit http://www.genesismission.org/mission/recgallery.html.

Original Source: NASA/JPL News Release

Posted on by Fraser Cain

Milky Way is a Dangerous, Turbulent Place

Image credit: ESO
Home is the place we know best. But not so in the Milky Way – the galaxy in which we live. Our knowledge of our nearest stellar neighbours has long been seriously incomplete and – worse – skewed by prejudice concerning their behaviour. Stars were generally selected for observation because they were thought to be “interesting” in some sense, not because they were typical. This has resulted in a biased view of the evolution of our Galaxy.

The Milky Way started out just after the Big Bang as one or more diffuse blobs of gas of almost pure hydrogen and helium. With time, it assembled into the flattened spiral galaxy which we inhabit today. Meanwhile, generation after generation of stars were formed, including our Sun some 4,700 million years ago.

But how did all this really happen? Was it a rapid process? Was it violent or calm? When were all the heavier elements formed? How did the Milky Way change its composition and shape with time? Answers to these and many other questions are ‘hot’ topics for the astronomers who study the birth and evolution of the Milky Way and other galaxies.

Now the rich results of a 15 year-long marathon survey by a Danish-Swiss-Swedish research team [2] are providing some of the answers.

1,001 nights at the telescopes
The team spent more than 1,000 observing nights over 15 years at the Danish 1.5-m telescope of the European Southern Observatory at La Silla (Chile) and at the Swiss 1-m telescope of the Observatoire de Haute-Provence (France). Additional observations were made at the Harvard-Smithsonian Center for Astrophysics in the USA. A total of more than 14,000 solar-like stars (so-called F- and G-type stars) were observed at an average of four times each – a total of no less than 63,000 individual spectroscopic observations!

This now complete census of neighbourhood stars provides distances, ages, chemical analysis, space velocities and orbits in the general rotation of the Milky Way. It also identifies those stars (about 1/3 of them all) which the astronomers found to be double or multiple.

This very complete data set for the stars in the solar neighbourhood will provide food for thought by astronomers for years to come.

A dream come true
These observations provide the long-sought missing pieces of the puzzle to get a clear overview of the solar neighbourhood. They effectively mark the conclusion of a project started more than twenty years ago..

In fact, this work marks the fulfilment of an old dream by Danish astronomer Bengt Str?mgren (1908-1987), who pioneered the study of the history of the Milky Way through systematic studies of its stars. Already in the 1950’s he designed a special system of colour measurements to determine the chemical composition and ages of many stars very efficiently. And the Danish 50-cm and 1.5-m telescopes at the ESO La Silla Observatory (Chile) were constructed to make such projects possible.

Another Danish astronomer, Erik Heyn Olsen made the first step in the 1980’s by measuring the flux (light intensity) in several wavebands (in the “Str?mgren photometric system”) of 30,000 A, F and G stars over the whole sky to a fixed brightness limit. Next, ESA’s Hipparcos satellite determined precise distances and velocities in the plane of the sky for these and many other stars.

The missing link was the motions along the line of sight (the so-called radial velocities). They were then measured by the present team from the Doppler shift of spectral lines of the stars (the same technique that is used to detect planets around other stars), using the specialized CORAVEL instrument.

Stellar orbits in the Milky Way
With the velocity information completed, the astronomers can now compute how the stars have wandered around in the Galaxy in the past, and where they will go in the future, cf. PR Video Clip 04/04.

Birgitta Nordstr?m, leader of the team, explains: “For the first time we have a complete set of observed stars that is a fair representation of the stellar population in the Milky Way disc in general. It is large enough for a proper statistical analysis and also has complete velocity and binary star information. We have just started the analysis of this dataset ourselves, but we know that our colleagues worldwide will rush to join in the interpretation of this treasure trove of information.”

The team’s initial analysis indicates that objects like molecular clouds, spiral arms, black holes, or maybe a central bar in the Galaxy, have stirred up the motion of the stars throughout the entire history of the Milky Way disc.

This in turn reveals that the evolution of the Milky Way was far more complex and chaotic than traditional, simplified models have long so far assumed. Supernova explosions, galaxy collisions, and infall of huge gas clouds have made the Milky Way a very lively place indeed!

Original Source: ESO News Release

Posted on by Fraser Cain

Asteroid Search Looks South

Image credit: UA
The hunt for space rocks on a collision course with Earth has so far been pretty much limited to the Northern Hemisphere.

But last week astronomers took the search for Earth-threatening asteroids to southern skies.

Astronomers using a refurbished telescope at the Australian National University’s Siding Spring Observatory discovered their first two near-Earth asteroids (NEAs) on March 29. NEAs are asteroids that pass near the Earth and may pose a threat of collision.

Siding Spring Survey (SSS) astronomer Gordon Garradd detected a roughly 100-meter (about 300-foot) diameter asteroid and 300-meter (about 1,000-foot) diameter asteroid in images he obtained with the 0.5-meter (20-inch) Uppsala Schmidt telescope.

SSS partner Robert H. McNaught confirmed both discoveries in images he took with the Siding Spring 1-meter (40-inch) that same night.

The 100-meter asteroid, designated 2004 FH29, makes a complete orbit around the sun every 2.13 years. It missed Earth by 3 million kilometers (1.9 million miles), or 8 times the Earth-to-moon distance, yesterday, traveling at 10 km per second (22,000 mph) relative to Earth.

The 300-meter asteroid, designated 2004 FJ29, orbits the sun about every 46 weeks. It came within 20 million kilometers (12 million miles), or within 52 lunar distances of Earth, last Tuesday, March 30, traveling at 18 km per second (40,000 mph) relative to Earth.

Neither object poses a direct threat of colliding with Earth.

Had the asteroids not missed, damage from their impacts would have depended on what kind of rock they’re made of. The 100-meter object likely would mostly burn up in Earth’s atmosphere in an airblast equivalent to 10 megatons of TNT, comparable to the 1908 explosion above the Tunguska River valley in Siberia, McNaught said. The 300-meter rocky asteroid likely would reach Earth’s surface, dumping the equivalent of 1,400 megatons of TNT energy into Earth’s atmosphere, he added. That’s comparable to 200 Tunguskas, or 24 times the largest thermonuclear bomb explosion, a 58 megaton Soviet bomb exploded in 1961.

The new survey is a joint collaboration between the University of Arizona Lunar and Planetary Laboratory and ANU’s Research School of Astronomy and Astrophysics. It is funded by NASA’s Near-Earth Object Observation Program, a 10-year effort to discover and track at least 90 percent of the one kilometer (six-tenths of a mile) or larger NEOs with the potential to become impact hazards.

When astronomers detect what they suspect is an NEA, they immediately must take additional images to confirm their discovery, McNaught said. Surveys often have to suspend their NEA searches and spend observing time confirming NEAs, or they risk losing them altogether because follow-up observations were made too late, he added.

The SSS plan is to use the 1-meter (40-inch) telescope for part of the month to quickly confirm suspect asteroids detected with the Uppsala, freeing the smaller telescope to continue it searches.

“Our confirmation strategy worked beautifully on our first try,” McNaught said.

The Uppsala Schmidt telescope was built in the 1950s for Uppsala Observatory in Sweden. It was sited at Stromlo as the Uppsala Southern Station to make wide field photographs of the southern sky. Increasing light pollution from Canberra led to its relocation to Siding Spring, near Coonabarabran in New South Wales, in 1982. Despite its high quality optics, the telescope drifted into disuse because it used photographic film rather than modern electronic detectors and had to be operated manually.

In 1999, McNaught and Stephen M. Larson of UA?s Lunar and Planetary Laboratory joined in an effort to refurbish and upgrade the Uppsala telescope. Larson had similarly just overhauled a manually operated, photographic wide-field Schmidt telescope in the Santa Catalina Mountains north of Tucson for his Catalina Sky Survey (CSS), part of the NASA-funded program to spot and track asteroids headed toward Earth.

The SSS builds on telescope control, detector technology and software developed for the CSS in Tucson. During the upgrade, the Uppsala was completely reconditioned, and fitted with computer control, a large format (16 megapixel) solid state detector array, and extensive support computers and software that detects objects moving against background stars.

Larson said his reaction to the SSS milestone was “one of relief, since it took several years to make the telescope and facility modifications. Now the real work begins.”

Larson and Catalina Sky Survey team member Ed Beshore worked on commissioning the Uppsala telescope during the past few months. Commissioning a telescope is like commissioning a ship: You have to get all the parts working and working together, and adjust things so they perform as expected.

“We actually achieved ‘first light’ last summer, with good images from the start,” Larson said.

McNaught and Garradd will operate SSS about 20 nights each month. They suspend operations when the week around full moon brightens the sky, making faint object detection difficult.

The Catalina telescope, which Larson and his team upgraded again in May 2000, features new optics that give it a 69 centimeter (27-inch) aperture and a new, more sensitive camera. In addition to Larson and Beshore, Eric Christensen, Rik Hill, David McLean, and Serena Howard operate CSS.

Both CSS and SSS telescopes can detect objects as faint as 20th magnitude, close to sky background level generated by scattered city light and auroral glow that brightens Earth?s upper atmosphere.

Original Source: UA News Release

Posted on by Fraser Cain

SOHO Has Seen 750 Comets

Image credit: ESA
On 22 March 2004, the ESA/NASA SOHO solar observatory spacecraft discovered its 750th comet since its launch in December 1995.

SOHO comet 750 was discovered by the German amateur astronomer Sebastian H?nig, one of the most successful SOHO comet-hunters. It was a part of the Kreutz family of ‘sungrazing’ comets, which usually evaporate in the hot solar atmosphere.

The LASCO coronagraph on SOHO, designed for seeing outbursts from the Sun, uses a mask to block the bright rays from the visible surface. It monitors a large volume of surrounding space and, as a result, has become the most prolific ‘discoverer’ of comets in the history of astronomy. Its images are displayed on the internet.

More than 75% of the discoveries have come from amateur comet hunters around the world, watching these freely available SOHO images on the internet. So, anyone with internet access can take part in the hunt for new comets and be a ‘comet discoverer’! Click here for information about how to search for your own comet.

SOHO is a mission of international co-operation between ESA and NASA, launched in December 1995. Every day SOHO sends thrilling images from which research scientists learn about the Sun’s nature and behaviour. Experts around the world use SOHO images and data to help them predict ‘space weather’ events affecting our planet.

Original Source: ESA News Release

Posted on by Fraser Cain

Chandra Sees Titan’s X-Ray Shadow

Image credit: Chandra
A rare celestial event was captured by NASA’s Chandra X-ray Observatory as Titan ? Saturn’s largest moon and the only moon in the Solar System with a thick atmosphere ? crossed in front of the X-ray bright Crab Nebula. The X-ray shadow cast by Titan allowed astronomers to make the first X-ray measurement of the extent of its atmosphere.

On January 5, 2003, Titan transited the Crab Nebula, the remnant of a supernova explosion that was observed to occur in the year 1054. Although Saturn and Titan pass within a few degrees of the Crab Nebula every 30 years, they rarely pass directly in front of it.

“This may have been the first transit of the Crab Nebula by Titan since the birth of the Crab Nebula,” said Koji Mori of Pennsylvania State University in University Park, and lead author on an Astrophysical Journal paper describing these results. “The next similar conjunction will take place in the year 2267, so this was truly a once in a lifetime event.”

Chandra’s observation revealed that the diameter of the X-ray shadow cast by Titan was larger than the diameter of its solid surface. The difference in diameters gives a measurement of about 550 miles (880 kilometers) for the height of the X-ray absorbing region of Titan’s atmosphere. The extent of the upper atmosphere is consistent with, or slightly (10-15%) larger, than that implied by Voyager I observations made at radio, infrared, and ultraviolet wavelengths in 1980.

“Saturn was about 5% closer to the Sun in 2003, so increased solar heating of Titan may account for some of this atmospheric expansion,” said Hiroshi Tsunemi of Osaka University in Japan, one of the coauthors on the paper.

The X-ray brightness and extent of the Crab Nebula made it possible to study the tiny X-ray shadow cast by Titan during its transit. By using Chandra to precisely track Titan’s position, astronomers were able to measure a shadow one arcsecond in diameter, which corresponds to the size of a dime as viewed from about two and a half miles.

Unlike almost all of Chandra’s images which are made by focusing X-ray emission from cosmic sources, Titan’s X-ray shadow image was produced in a manner similar to a medical X-ray. That is, an X-ray source (the Crab Nebula) is used to make a shadow image (Titan and its atmosphere) that is recorded on film (Chandra’s ACIS detector).

Titan’s atmosphere, which is about 95% nitrogen and 5% methane, has a pressure near the surface that is one and a half times the Earth’s sea level pressure. Voyager I spacecraft measured the structure of Titan’s atmosphere at heights below about 300 miles (500 kilometers), and above 600 miles (1000 kilometers). Until the Chandra observations, however, no measurements existed at heights in the range between 300 and 600 miles.

Understanding the extent of Titan’s atmosphere is important for the planners of the Cassini-Huygens mission. The Cassini-Huygens spacecraft will reach Saturn in July of this year to begin a four-year tour of Saturn, its rings and its moons. The tour will include close flybys of Titan that will take Cassini as close as 600 miles, and the launching of the Huygens probe that will land on Titan’s surface.

“If Titan’s atmosphere has really expanded, the trajectory may have to be changed,” said Tsunemi.

The paper on these results has been accepted and is expected to appear in a June 2004 issue of The Astrophysical Journal. Other members of the research team were Haroyoski Katayama (Osaka University), David Burrows and Gordon Garmine (Penn State University), and Albert Metzger (JPL). Chandra observed Titan from 9:04 to 18:46 UT on January 5, 2003, using its Advanced CCD Imaging Spectrometer instrument.

NASA’s Marshall Space Flight Center, Huntsville, Ala., manages the Chandra program for the Office of Space Science, NASA Headquarters, Washington. Northrop Grumman of Redondo Beach, Calif., formerly TRW, Inc., was the prime development contractor for the observatory. The Smithsonian Astrophysical Observatory controls science and flight operations from the Chandra X-ray Center in Cambridge, Mass.

Additional information and images are available at:

http://chandra.harvard.edu/ and http://chandra.nasa.gov/

Original Source: Chandra News Release

Posted on by Fraser Cain

Is There Life on Europa?

Image credit: NASA
Christopher Chyba is the principal investigator for the SETI Institute lead team of the NASA Astrobiology Institute (NAI). Chyba formerly headed the SETI Institute’s Center for the Study of Life in the Universe. His NAI team is pursuing a wide range of research activities, looking at both life’s beginnings on Earth and the possibility of life on other worlds. Several of his team’s research projects will examine the potential for life – and how one might go about detecting it – on Jupiter’s moon Europa. Astrobiology Magazine’s managing editor Henry Bortman recently spoke with Chyba about this work.

Astrobiology Magazine: One of the areas of focus of your personal research has been the possibility of life on Jupiter’s moon Europa. Several of the projects funded by your NAI grant deal with this ice-covered world.

Christopher Chyba: Right. We’re interested in interactions of life and planetary evolution. There are three worlds that are most interesting from that point of view: Earth, Mars and Europa. And we have a handful of projects going that are relevant to Europa. Cynthia Phillips is the leader of one of those projects; my grad student here at Stanford, Kevin Hand, heads up another one; and Max Bernstein, who’s a SETI Institute P.I., is a leader on the third.

There are two components to Cynthia’s projects. One that I think is really exciting is what she calls “change comparison.” That goes back to her days of being a graduate associate on the Galileo imaging team, where she did comparisons to look for surface changes on another of Jupiter’s moons, Io, and was able to extend her comparisons to include older Voyager images of Io.

We have Galileo images of Io, taken in the late 1990s, and we have Voyager images of Io, taken in 1979. So there are two decades between the two. If you can do a faithful comparison of the images, then you can learn about what’s changed in the interim, get some sense of how geologically active the world is. Cynthia did this comparison for Io, then did it for the much more subtle features of Europa.

That may sound like a trivial task. And for really gross features I suppose it is. You just look at the images and see if something’s changed. But since the Voyager camera was so different, since its images were taken at different lighting angles than Galileo images, since the spectral filters were different, there are all sorts of things that, once you get beyond the biggest scale of examination, make that much more difficult than it sounds. Cynthia takes the old Voyager images and, if you will, transforms them as closely as one can into Galileo-type images. Then she overlays the images, so to speak, and does a computer check for geological changes.

When she did this with Europa as part of her Ph.D. thesis, she found that there were no observable changes in 20 years on those parts of Europa that we have images for from both spacecraft. At least not at the resolution of the Voyager spacecraft – you’re stuck with the lowest resolution, say about two kilometers per pixel.

Over the duration of the Galileo mission, you’ve got at best five and a half years. Cynthia’s idea is that you’re more likely to detect change in smaller features, in a Galileo-to-Galileo comparison, at the much higher resolution that Galileo gives you, than you were working with images that were taken 20 years apart but that require you to work at two kilometers per pixel. So she’s going to do the Galileo-to-Galileo comparison.

The reason this is interesting from an astrobiological perspective is that any sign of geological activity on Europa might give us some clues about how the ocean and the surface interact. The other component of Cynthia’s project is to better understand the suite of processes involved in those interactions and what their astrobiological implications might be.

AM: You and Kevin Hand are working together to study some of the chemical interactions believed to be taking place on Europa. What specifically will you be looking at?

There are a number of components of the work I’m doing with Kevin. One component stems from a paper that Kevin and I had in Science in 2001, which has to do with the simultaneous production of electron donors and electron acceptors. Life as we know it, if it doesn’t use sunlight, makes its living by combining electron donors and acceptors and harvesting the liberated energy.

For example, we humans, like other animals, combine our electron donor, which is reduced carbon, with oxygen, which is our electron acceptor. Microbes, depending on the microbe, may use one, or several, of many possible different pairings of electron donors and electron acceptors. Kevin and I were finding abiotic ways that these pairings could be produced on Europa, using what we understand about Europa now. Many of these are produced through the action of radiation. We’re going to continue that work in much more detailed simulations.

We’re also going to look at the survival potential of biomarkers at Europa’s surface. That is to say, if you’re trying to look for biomarkers from an orbiter, without getting down to the surface and digging, what sort of molecules would you look for and what are your prospects for actually seeing them, given that there’s an intense radiation environment at the surface that should slowly degrade them? Maybe it won’t even be that slow. That’s part of what we want to understand. How long can you expect certain biomarkers that would be revelatory about biology to survive on the surface? Is it so short that looking from orbit doesn’t make any sense at all, or is it long enough that it might be useful?

That has to be folded into an understanding of turnover, or so-called “impact gardening” on the surface, which is another component of my work with Cynthia Phillips’, by the way. Kevin will be getting at that by looking at terrestrial analogs.

AM: How do you determine which biomarkers to study?

CC: There are certain chemical compounds that are commonly used as biomarkers in rocks that go back billions of years in the terrestrial past. Hopanes, for example, are viewed as biomarkers in the case of cyanobacteria. These biomarkers withstood whatever background radiation was present in those rocks from the decay of incorporated uranium, potassium, and so on, for over two billion years. That gives us a kind of empirical baseline for survivability of certain kinds of biomarkers. We want to understand how that compares to the radiation and oxidation environment on the surface of Europa, which is going to be much harsher.

Both Kevin and Max Bernstein are going to get after that question by doing laboratory simulations. Max is going to be irradiating nitrogen-containing biomarkers at very low temperatures in his laboratory apparatus, trying to understand the survivability of the biomarkers and how radiation changes them.

AM: Because even if the biomarkers don’t survive in their original form they might get transformed into another form that a spacecraft could detect?

CC: That’s potentially the case. Or they might get converted into something that is indistinguishable from meteoritic background. The point is to do the experiment and find out. And to get a good sense of the time scale.

That’s going to be important for another reason as well. The kind of terrestrial comparison I just mentioned, while I think it’s something we should know, potentially has limits because any organic molecule on the surface of Europa is in a highly oxidizing environment, where the oxygen’s getting produced by the radiation reacting with the ice. Europa’s surface is probably more oxidizing than the environment organic molecules would experience trapped in a rock on the Earth. Since Max will be doing these radiation experiments in ice, he will be able to give us a good simulation of the surface environment on Europa.

Original Source: Astrobiology Magazine

Posted on by Fraser Cain

Two Directions for Sample Return Mission

Image credit: EADS
Following award of the ?600k study contract by ESA, EADS Space has made significant progress in completing the first definition of a European Mars Sample Return (MSR) mission. While EADS Astrium is defining the overall mission and the spacecraft, EADS Space Transportation is responsible for the re-entry systems and a ‘Mars Ascent Vehicle’ – a small rocket to carry the precious sample up through the Martian atmosphere.

The team at EADS Astrium, Stevenage is currently preparing for the Mid Term Review where two very different designs will have to be reduced to one.

In the first concept the launch vehicle lifts the sample from the surface of Mars and docks with the Earth Return Vehicle. In the second concept the launch vehicle releases the sample container into a low Mars orbit and the Earth Return Vehicle uses a capture mechanism to perform the rendezvous. The selection of the rendezvous concept has a significant impact on the overall mass, cost and complexity of the mission.

Marie-Claire Perkinson, Senior Systems Engineer at EADS Astrium, Stevenage, leading the study said. “Our industrial team, which includes EADS Space in France; Galileo Avionica in Italy, Sener in Spain and Utopia Consultancies in Germany has done a great job so far in proposing the two exciting concepts. We now have to select the best solution and then, once ESA has raised the appropriate support and funds for the implementation of the mission, launch could be as early as 2011.”

European astronauts may land on Mars one day, but getting them there and safely returning them to Earth will involve many steps and numerous technical challenges in propulsion, structures, computers and software. It will require sophisticated spacecraft to escape from Earth’s orbit; fly to Mars, survive atmospheric entry and landing; operate on the surface; take-off; return to Earth and then finally get the crew back on terra firma. Long before this can be accomplished some key technologies must be demonstrated. The best way to do this is to fly a robotic mission with a scaled-down version of the eventual manned mission.

This is exactly the goal of Mars Sample Return, the second flagship mission of the European Space Agency’s Aurora planetary exploration initiative and one of the most eagerly awaited future space missions for the planetary scientists.

Because Martian winds have transported dust across the planet’s surface over millions of years, the MSR sample could include particles from many different sources, representing a wide variety of rock types and ages, like grains of sand on a beach. Each granule could offer completely different insights into the rich geologic past of the Red Planet. Scientists could now “look at the sample as if each grain were a rock,” said Professor Colin Pillinger of the Open University. This would build on the decades of research already carried out on lunar rock samples.

EADS Space has used its unique heritage in building launch vehicles, planetary spacecraft and re-entry systems, combined with a deep understanding of the science goals to win the ESA mission study. ESA’s Aurora Project Manager Bruno Gardini said “The Mars Sample Return mission is one of the most challenging missions ever considered by ESA. Not only does it include many new technologies and four or five different spacecraft, but it is also a mission of tremendous scientific importance and the first robotic mission with a similar profile to a possible human expedition to Mars.”

Original Source: RAS News Release