Posted on by Fraser Cain

Antarctica Is Getting Ready to Really Heat Up

While Antarctica has mostly cooled over the last 30 years, the trend is likely to rapidly reverse, according to a computer model study by NASA researchers. The study indicates the South Polar Region is expected to warm during the next 50 years.

Findings from the study, conducted by researchers Drew Shindell and Gavin Schmidt of NASA’s Goddard Institute of Space Studies (GISS), New York, appeared in the Geophysical Research Letters. Shindell and Schmidt found depleted ozone levels and greenhouse gases are contributing to cooler South Pole temperatures.

Low ozone levels in the stratosphere and increasing greenhouse gases promote a positive phase of a shifting atmospheric climate pattern in the Southern Hemisphere, called the Southern Annular Mode (SAM). A positive SAM isolates colder air in the Antarctic interior.

In the coming decades, ozone levels are expected to recover due to international treaties that banned ozone-depleting chemicals. Higher ozone in the stratosphere protects Earth’s surface from harmful ultraviolet radiation. The study found higher ozone levels might have a reverse impact on the SAM, promoting a warming, negative phase. In this way, the effects of ozone and greenhouse gases on the SAM may cancel each other out in the future. This could nullify the SAM’s affects and cause Antarctica to warm.

“Antarctica has been cooling, and one could argue some regions could escape warming, but this study finds this is not very likely,” Shindell said. “Global warming is expected to dominate in future trends.”

The SAM, similar to the Arctic Oscillation or Northern Annular Mode in the Northern Hemisphere, is a seesaw in atmospheric pressure between the pole and the lower latitudes over the Southern Ocean and the tip of South America.

These pressure shifts between positive and negative phases speed-up and slow down the westerly winds that encircle Antarctica. Since the late 1960s, the SAM has more and more favored its positive phase, leading to stronger westerly winds. These stronger westerly winds act as a kind of wall that isolates cold Antarctic air from warmer air in the lower latitudes, which leads to cooler temperatures.

Greenhouse gases and ozone depletion both lower temperatures in the high latitude stratosphere. The cooling strengthens the stratospheric whirling of westerly winds, which in turn influences the westerly winds in the lower atmosphere. According to the study, greenhouse gases and ozone have contributed roughly equally in promoting a strong-wind, positive SAM phase in the troposphere, the lowest part of the atmosphere.

Shindell and Schmidt used the NASA GISS Climate Model to run three sets of tests, each three times. For each scenario, the three runs were averaged together. Scenarios included the individual effects of greenhouse gases and ozone on the SAM, and then a third run that examined the effects of the two together.

The model included interactions between the oceans and atmosphere. Each model run began in 1945 and extended through 2055. For the most part, the simulations matched well compared with past observations.

Model inputs of increasing greenhouse gases were based upon observations through 1999, and upon the Intergovernmental Panel on Climate Change mid-range estimates of future emissions. Stratospheric ozone changes were based on earlier NASA GISS model runs that were found to be in good agreement with past observations and similar to those found in other chemistry-climate models for the future.

Shindell said the biggest long-term danger of global warming in this region would be ice sheets melting and sliding into the ocean. “If Antarctica really does warm up like this, then we have to think seriously about what level of warming might cause the ice sheets to break free and greatly increase global sea levels,” he said.

In the Antarctic Peninsula, ice sheets as big as Rhode Island have already collapsed into the ocean due to warming. The warming in this area is at least partially a result of the strengthened westerly winds that pass at latitudes of about 60 to 65 degrees south. As the peninsula sticks out from the continent, these winds carry warm maritime air that heats the peninsula.

Original Source: NASA News Release

Posted on by Fraser Cain

Epsom Salts Could Be a Source of Martian Water

Epsom-like salts believed to be common on Mars may be a major source of water there, say geologists at Indiana University Bloomington and Los Alamos National Laboratory. In their report in this week’s Nature, the scientists also speculate that the salts will provide a chemical record of water on the Red Planet.

“The Mars Odyssey orbiter recently showed that there may be as much as 10 percent water hidden in the Martian near-surface,” said David Bish, Haydn Murray Chair of Applied Clay Mineralogy at IU and a co-author of the report. “We were able to show that under Mars-like conditions, magnesium sulfate salts can contain a great deal of water. Our findings also suggest that the kinds of sulfates we find on Mars could give us a lot of insight into the history of water and mineral formation there.”

The scientists learned that magnesium sulfate salts are extremely sensitive to changes in temperature, pressure and humidity. For that reason, the scientists argue that information contained in the salts could be easily lost if samples were brought back to Earth for study. Instead, they say, future missions to Mars should measure the properties of the salts on site.

The existence of magnesium sulfate salts on Mars was first suggested by the 1976 Viking missions and has since been confirmed by the Mars Exploration Rover as well as the Odyssey and Pathfinder missions. One way to quash remaining doubts that the salts are really there, however, would be to equip a Martian rover with an X-ray diffractometer — an instrument that analyzes the properties of crystals. Coincidentally, such a device could also be used to examine magnesium sulfate salts on Mars. Bish and collaborators from NASA Ames and Los Alamos are currently developing a miniaturized X-ray diffractometer with NASA funding.

Some magnesium sulfate salts trap more water than others. Epsomite, for example, has the most water in it — 51 percent by weight — while hexahydrite and kieserite have less (47 percent and 13 percent by weight, respectively). The proportion of water to magnesium sulfate affects the chemical properties of the different salts.

While varying temperature, pressure and humidity inside an experimental chamber, the scientists studied how the different magnesium salts transform over time.

When temperature and pressure inside an experimental chamber were lowered to Mars-like conditions (minus 64 degrees Fahrenheit, and less than 1 percent of Earth’s normal surface pressure), crystals of epsomite initially transformed into slightly less watery hexahydrite crystals and then became disorganized, but they still contained water. In contrast, “kieserite doesn’t let go of its water very easily, even at very low pressure and humidity or at elevated temperatures,” Bish said.

But when the scientists increased humidity inside the experimental chamber, they found that kieserite transformed into hexahydrite and then epsomite, which have more water.

Bish and his Los Alamos colleagues believe that the proportion and distribution of hexahydrite, kieserite and other magnesium sulfate salts on Mars may hold a record of past changes in climate and whether or not water once flowed there. However, kieserite might not be preserved through cycles of wetting and drying because of its ability to rehydrate to hexahydrite and epsomite, which can then become amorphous through drying.

Los Alamos National Laboratory geologists David Vaniman, Steve Chipera, Claire Fialips, William Carey and William Feldman also contributed to the study. It was funded by LANL Directed Research and Development Funding and NASA Mars Fundamental Research Program grants.

Original Source: Indiana University News Release

Posted on by Fraser Cain

New Mission Will Survey the Entire Sky in Infrared

A new NASA mission will scan the entire sky in infrared light in search of nearby cool stars, planetary construction zones and the brightest galaxies in the universe.

Called the Wide-field Infrared Survey Explorer, the mission has been approved to proceed into the preliminary design phase as the next in NASA’s Medium-class Explorer program of lower cost, highly focused, rapid-development scientific spacecraft. It is scheduled to launch in 2008.

Like a powerful set of night vision goggles, the new space-based telescope will survey the cosmos with infrared detectors up to 500,000 times more sensitive than previous survey missions. It will reveal hundreds of cool, or failed, stars, called brown dwarfs, some of which may lie closer to us than any known stars.

“Approximately two-thirds of nearby stars are too cool to be detected with visible light,” said Principal Investigator Dr. Edward Wright of the University of California, Los Angeles, who proposed the new mission to NASA. “The Wide-field Infrared Survey Explorer will see most of them.”

The telescope will also provide a complete inventory of dusty planet-forming discs around nearby stars, and find colliding galaxies that emit more light – specifically infrared light – than any other galaxies in the universe. In the end, the survey will consist of more than one million images, from which hundreds of millions of space objects will be catalogued.

“The mission will complete the basic reconnaissance of the universe in mid-infrared wavelengths, providing a vast storehouse of knowledge that will endure for decades,” said Dr. Peter Eisenhardt, project scientist for the mission at NASA’s Jet Propulsion Laboratory, Pasadena, Calif. “This catalogue of data will also provide NASA’s future James Webb Space Telescope with a comprehensive list of targets.”

JPL will manage the Wide-field Infrared Survey Explorer at a total cost to NASA of approximately $208 million. William Irace of JPL is the project manager. The cryogenic instrument will be built by the Space Dynamics Laboratory, Logan, Utah, and the spacecraft will be built by Ball Aerospace and Technologies Corporation, Boulder, Colorado. Science operations and data processing will take place at the JPL/Caltech Infrared Processing and Analysis Center, Pasadena. Calif. JPL is a division of Caltech.

More than 70 U.S. and cooperative international scientific space missions have been part of NASA’s Explorer program. The missions are characterized by relatively moderate cost, and by small- to medium-sized missions that are capable of being built, tested and launched in a short time interval compared to the large observatories. NASA Goddard Space Flight Center, Greenbelt, Md., manages the Explorer program for the Science Mission Directorate, NASA Headquarters, Washington.

For more information, visit http://ds9.ssl.berkeley.edu/wise/ or http://explorers.gsfc.nasa.gov.

Original Source: NASA/JPL News Release

Posted on by Fraser Cain

It Gave Until it Couldn’t Give Any More

Astronomers using the Gemini North and Keck II telescopes have peered inside a violent binary star system to find that one of the interacting stars has lost so much mass to its partner that it has regressed to a strange, inert body resembling no known star type.

Unable to sustain nuclear fusion at its core and doomed to orbit with its much more energetic white dwarf partner for millions of years, the dead star is essentially a new, indeterminate type of stellar object.

“Like the classic line about the aggrieved partner in a romantic relationship, the smaller donor star gave, and gave, and gave some more until it had nothing left to give,” says Steve B. Howell, an astronomer with Wisconsin-Indiana-Yale-NOAO (WIYN) telescope and the National Optical Astronomy Observatory, Tucson, AZ. “Now the donor star has reached a dead end – it is far too massive to be considered a super-planet, its composition does not match known brown dwarfs, and it is far too low in mass to be a star. There’s no true category for an object in such limbo.”

The binary system, known as EF Eridanus (abbreviated EF Eri), is located 300 light-years from Earth in the constellation Eridanus. EF Eri consists of a faint white dwarf star with about 60 percent of the mass of the Sun and the donor object of unknown type, which has an estimated bulk of only 1/20th of a solar mass.

Howell and Thomas E. Harrison of New Mexico State University made high-precision infrared measurements of the binary star system using the spectrographic capabilities of the Near Infrared Imager (NIRI) on the Gemini North telescope and NIRSPEC on Keck II both on Mauna Kea in December 2002 and September 2003, respectively. Supporting observations were made with the 2.1-meter telescope at Kitt Peak National Observatory near Tucson in September 2002.

EF Eri is a type of binary star system known as magnetic cataclysmic variables. This class of systems may produce many more of these ‘dead’ objects than scientists have realized, says Harrison, co-author of a paper on the discovery to be published in the October 20 issue of the Astrophysical Journal. “These types of systems are not generally accounted for within the usual census figures of star systems in a typical galaxy,” Harrison says. “They certainly should be considered more carefully.”

The white dwarf in EF Eri is a compressed, burnt-out remnant of a solar-type star that is now about the same diameter as the Earth, though it still emits copious amounts of visible light. Howell and Harrison observed EF Eri in the infrared because infrared light from the pair is naturally dominated by heat and longer wavelength emissions from the secondary object.

The scientific detective work to deduce the components of this binary system was complicated greatly by the cyclotron radiation emitted as free electrons spiral down the powerful magnetic field lines of the white dwarf. The white dwarf’s magnetic field is about 14 million times as powerful as the Sun’s. The resulting cyclotron radiation is emitted primarily in the infrared part of the spectrum.

“In our initial spectroscopy of EF Eri, we noted that some parts of the infrared continuum light became about 2-3 times brighter for a time period, then went away. This brightening repeated every orbit, and thus had to have an origin within the binary,” Howell explains. “We first thought the brightness change resulted from the difference between a heated side and a cooler side of the donor object, but further observations with Gemini and Keck instead pointed to cyclotron radiation. We ‘see’ this additional infrared component at the phases which occur when the radiation is beamed in our direction, and we do not see it when the beaming points in other directions.”

The 81-minute orbital period of the two objects was probably four or five hours when the mass transfer process began about five billion years ago. Originally, the secondary object may also have been similar in size to the Sun, with perhaps 50-100 percent of a solar mass.

“When this interactive process of mass transfer from the secondary star to the white dwarf begin, and why it stopped, both remain unknown to us,” Howell says. During this process, repeated outbursts and novae explosions were very likely. The physics of the process also caused the two objects to spiral closer to each other. Today, the two objects orbit each other at about the same separation as the distance from the Earth to the Moon. The donor object has regressed to a body with a diameter roughly equal to the planet Jupiter.

The combined observing power of the Gemini 8-meter and Keck 10-meter telescopes and their large primary mirrors, which were essential to this research, Howell says, makes it clear that neither spectral features of the donor nor its composition match any known type of brown dwarf or planet.

Derek Homeier University of Georgia created a series of computer models that attempt to replicate the conditions at EF Eri, but even the best of these do not match perfectly.

The shape of the spectra indicate a very cool object (about 1,700 degrees Kelvin, equivalent to a cool brown dwarf), yet they do not have the same detailed shape or key features of brown dwarf spectra. The coolest normal stars (very low mass M-type stars) are about 2,500 degrees K, and Jupiter is 124 degrees K. The close-in “hot Jupiter” exoplanets detected indirectly by other astronomers using their gravitational effect on their parent stars are estimated to be 1,000-1,600 degrees K.

There is a small chance that the EF Eri system could have originally consisted of the progenitor of the present-day white dwarf star and some sort of “super-planet” that survived the evolution of the white dwarf to result in the system observed now, but this is considered unlikely.

“There are about 15 other known binary systems out there that may be similar to EF Eri, but none has been studied enough to tell,” Howell says. “We are working on some of them right now, and trying to improve our models to better match the infrared spectra.”

Co-authors of this paper on EF Eri are Paula Szkody of the University of Washington in Seattle, and Joni Johnson and Heather Osborne of New Mexico State.

The WIYN 3.5-meter telescope is located at Kitt Peak National Observatory, 55 miles southwest of Tucson, AZ. Kitt Peak National Observatory is part of the National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA), Inc., under a cooperative agreement with the National Science Foundation (NSF).

The national research agencies that form the Gemini Observatory partnership include: the US National Science Foundation (NSF), the UK Particle Physics and Astronomy Research Council (PPARC), the Canadian National Research Council (NRC), the Chilean Comisi?n Nacional de Investigaci?n Cientifica y Tecnol?gica (CONICYT), the Australian Research Council (ARC), the Argentinean Consejo Nacional de Investigaciones Cient?ficas y T?cnicas (CONICET) and the Brazilian Conselho Nacional de Desenvolvimento Cient?fico e Tecnol?gico (CNPq). The Observatory is managed by AURA under a cooperative agreement with the NSF.

The W.M. Keck Observatory is operated by the California Association for Research in Astronomy (CARA), a scientific partnership of the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration.

Original Source: Gemini News Release

Posted on by Fraser Cain

Rover’s Wheels Acting Up

Engineers on NASA’s Mars Exploration Rover team are investigating possible causes and remedies for a problem affecting the steering on Spirit.

The relay for steering actuators on Spirit’s right-front and left-rear wheels did not operate as commanded on Oct. 1. Each of the front and rear wheels on the rover has a steering actuator, or motor, that adjusts the direction in which the wheels are headed independently from the motor that makes the wheels roll. When the actuators are not in use, electric relays are closed and the motor acts as a brake to prevent unintended changes in direction.

Engineers received results from Spirit today from a first set of diagnostic tests on the relay. “We are interpreting the data and planning additional tests,” said Rick Welch, rover mission manager at NASA’s Jet Propulsion Laboratory, Pasadena, Calif. “We hope to determine the best work-around if the problem does persist.”

Spirit and its twin, Opportunity, successfully completed their three-month primary missions in April and five-month mission extensions in September. They began second extensions of their missions on Oct. 1. Spirit has driven more than 3.6 kilometers (2.2 miles), six times the distance set as a goal for mission success. It is climbing into uplands called the “Columbia Hills.”

JPL’s Jim Erickson, rover project manager, said, “If we do not identify other remedies, the brakes could be released by a command to blow the fuse controlling the relay, though that would make those two brakes unavailable for the rest of the mission.” Without the steering-actuator brakes, small bumps or dips that a wheel hits during a drive might twist the wheel away from the intended drive direction.

“If we do need to disable the brakes, errors in drive direction could increase. However, the errors might be minimized by continuing to use the brakes on the left-front and right-rear wheels, by driving in smaller segments, and by adding a software patch to reset the direction periodically during a drive,” Erickson said. Engineers believe the steering-brake issue is not related to excessive friction detected during the summer in the drive motor for Spirit’s right-front wheel, because the steering actuator is a different motor.

Meanwhile, the team continues to use Spirit’s robotic arm and camera mast to study rocks and soils around the rover, without moving the vehicle until the cause of the anomaly is understood and corrective measures can be implemented.

JPL, a division of the California Institute of Technology in Pasadena, manages the Mars Exploration Rover project for NASA’s Science Mission Directorate, Washington. Additional information about the project is available from JPL at http://marsrovers.jpl.nasa.gov/ and from Cornell University, Ithaca, N.Y., at http://athena.cornell.edu.

Original Source: NASA/JPL News Release

Posted on by Fraser Cain

The Great Observatories Examine Kepler’s Supernova

Four hundred years ago, sky watchers, including the famous astronomer Johannes Kepler, best known as the discoverer of the laws of planetary motion, were startled by the sudden appearance of a “new star” in the western sky, rivaling the brilliance of the nearby planets.

Modern astronomers, using NASA’s three orbiting Great Observatories, are unraveling the mysteries of the expanding remains of Kepler’s supernova, the last such object seen to explode in our Milky Way galaxy.

When a new star appeared Oct. 9, 1604, observers could use only their eyes to study it. The telescope would not be invented for another four years. A team of modern astronomers has the combined abilities of NASA’s Great Observatories, the Spitzer Space Telescope, Hubble Space Telescope and Chandra X-ray Observatory, to analyze the remains in infrared radiation, visible light, and X-rays. Ravi Sankrit and William Blair of the Johns Hopkins University in Baltimore lead the team.

The combined image unveils a bubble-shaped shroud of gas and dust, 14 light-years wide and expanding at 6 million kilometers per hour (4 million mph). Observations from each telescope highlight distinct features of the supernova, a fast-moving shell of iron-rich material, surrounded by an expanding shock wave sweeping up interstellar gas and dust.

“Multi-wavelength studies are absolutely essential for putting together a complete picture of how supernova remnants evolve,” Sankrit said. Sankrit is an associate research scientist, Center for Astrophysical Sciences at Hopkins and lead for Hubble astronomer observations.

“For instance, the infrared data are dominated by heated interstellar dust, while optical and X-ray observations sample different temperatures of gas,” Blair added. Blair is a research professor, Physics and Astronomy Department at Hopkins and lead astronomer for Spitzer observations. “A range of observations is needed to help us understand the complex relationship that exists among the various components,” Blair said.

The explosion of a star is a catastrophic event. The blast rips the star apart and unleashes a roughly spherical shock wave that expands outward at more than 35 million kilometers per hour (22 million mph) like an interstellar tsunami. The shock wave spreads out into surrounding space, sweeping up any tenuous interstellar gas and dust into an expanding shell. The stellar ejecta from the explosion initially trail behind the shock wave. It eventually catches up with the inner edge of the shell and is heated to X-ray temperatures.

Visible-light images from Hubble’s Advanced Camera for Surveys reveal where the supernova shock wave is slamming into the densest regions of surrounding gas. The bright glowing knots are dense clumps that form behind the shock wave. Sankrit and Blair compared their Hubble observations with those taken with ground-based telescopes to obtain a more accurate distance to the supernova remnant of about 13,000 light-years.

The astronomers used Spitzer to probe for material that radiates in infrared light, which shows heated microscopic dust particles that have been swept up by the supernova shock wave. Spitzer is sensitive enough to detect both the densest regions seen by Hubble and the entire expanding shock wave, a spherical cloud of material. Instruments on Spitzer also reveal information about the chemical composition and physical environment of the expanding clouds of gas and dust ejected into space. This dust is similar to dust which was part of the cloud of dust and gas that formed the Sun and planets in our solar system.

The Chandra X-ray data show regions of very hot gas. The hottest gas, higher-energy X-rays, is located primarily in the regions directly behind the shock front. These regions also show up in the Hubble observations and also align with the faint rim of material seen in the Spitzer data. Cooler X-ray gas, lower-energy X-rays, resides in a thick interior shell and marks the location of the material expelled from the exploded star.

There have been six known supernovas in our Milky Way over the past 1,000 years. Kepler’s is the only one for which astronomers do not know what type of star exploded. By combining information from all three Great Observatories, astronomers may find the clues they need. “It’s really a situation where the total is greater than the sum of the parts,” Blair said. “When the analysis is complete, we will be able to answer several questions about this enigmatic object.”

Images and additional information are available at http://www.nasa.gov, http://hubblesite.org/news/2004/29, http://chandra.harvard.edu , http://spitzer.caltech.edu ,http://www.jhu.edu/news_info/news/, http://heritage.stsci.edu/2004/29 and http://www.nasa.gov/vision/universe/starsgalaxies/kepler.html.

Original Source: NASA/JPL News Release

Posted on by Fraser Cain

Rocket Will Launch 50 Nanosatellites

Image credit: Arianespace
During this year’s International Astronautical Federation (IAF) Congress in Vancouver, Canada, Arianespace, the Russian Space Agency with the support of the Russian space industry and IAF, in partnership with the leading space agencies from around the world, are proposing to commemorate the first satellite launch in 1957, by orbiting a cluster of 50 nanosatellites, each representing a different country.

Each nanosat will weigh about one kilogram, and will be dedicated to a scientific experiment under the responsibility of researchers at universities or other organizations. Each nanosat will offer a design life of about two years. All 50 will be launched on a single Arianespace mission.

“Arianespace is very proud to be participating in this commemoration,” said Jean-Yves Le Gall, the company’s Chief Executive Officer. “Supporting science and research is an integral part of our assigned mission. We have already orbited some 40 auxiliary payloads of the same type we will launch in 2007. Just like 50 years ago, when the first man-made Earth satellite was launched, these nanosatellites will signal a new era for scientists worldwide.”

Original Source: Arianespace News Release

Posted on by Mark Mortimer

Book Review: New Moon Rising

In an easy to read style, the book, for the most part, follows a chronological list of relevant events from about the year 2000 to the present. The main ones are Goldin’s last days, finding his replacement, the appointment of Sean O’Keefe, the loss of Columbia and the fabrication of NASA’s new vision which President Bush provided in early 2004. Names predominate throughout. Large quantities of people, projects, programs, companies and foundations appear in what sometimes seems to be a never ending parade. As quickly as these come, they go again. So, it is difficult to find a common thread or reason for their inclusion. Perhaps these names and/or offices are essential contributors, but this is not apparent. Nevertheless, the discussed events all directly contribute to the making of NASA’s new vision.

During Goldin’s time as administrator, NASA had many mandates and insufficient resources. The Challenger accident left the space shuttle program with a blemish and an even greater launch cost than originally estimated. The orbiting space station went through innumerable configurations and designs in an effort to please as many potential users as possible. Even NASA’s various field offices seemed more focussed on their own agendas than on a ‘corporate’ vision. Sean O’Keefe, Goldin’s replacement, had recent experience in financial auditing including a recent review of NASA’s finances. As the new administrator, his main assignment was to reassert fiscal realism. But to do this he needed priorities. And to set priorities he needed an achievable and specific vision. Thus, as much as O’Keefe replaced Goldin, so did O’Keefe need a vision to replace and rebuild from the current situation.

The premise of this book is that the creation of NASA’s vision was by the spontaneous and surreptitious meetings of a cadre of very junior hill staffers during coffee break and lunch. This seems difficult to believe, but the authors weave a very reasonable and continuous thread from this ‘rump’ group as they were called, through to more senior groups, senators and agencies and then up to the president. Again, names are liberally included, so this thread may be authentic, but still it seems a bit far fetched. Perhaps the most intriguing element is that NASA was apparently not part of this process until very late in the formulation. So in one sense it does seem a bit too fanciful to have junior staffers making a vision for an agency with an annual budget of $16 billion (can you imagine this happening for foreign policy?!). But, as they had nothing to lose and probably no alternate agendas, there is a ring of truth to this premise.

Perhaps equally fanciful is the claim that this new vision will get humans operating in space. Having a vision and a supporting budget is critical. Equally critical is the support of the elected politicians, who regularly change, as well as the support of other nations and their respective space agencies. But all of these will be needed for the duration. The authors rightly point out that this will be challenging. They even provide an excellent perspective on what to expect should either of this year’s presidential candidates win. Sadly, neither candidate seems solidly behind NASA and perhaps with this, the authors unknowingly provide more evidence contrary to their expectations than for it.

In their writing, the authors show they are non-partisan but very supportive of NASA’s new space vision. They acknowledge that senior NASA leadership provided access to information and verified personal communications, but they are also quick to point out that the contents is their own. The included DVD has memorable video footage of President Bush’s introduction of this vision, as well as Sean O’Keefe’s comments. This all lends authenticity to the contents and claim.

This book is good but it has its weaknesses. One item lacking is an index. Retracing people and events is almost impossible. Further, though the names and events may be very applicable today (the fall of the year 2004), expect them to become quickly very dated. With retirements and re-appointments, the parade of people just changes too quickly to make this book a useful reference in the long term. Also, perhaps the weakest element of the book is the lack of justification for spending nearly $100 billion for a program to send people to the Moon, Mars and beyond. Though more effort could have remedied these, the book is still a good read.

As the authors say in New Moon Rising, NASA needed and obtained a new space vision to direct its efforts. The authors provide a detailed and broad overview of the very large supporting cast that contributed to the vision that was initiated with President Bush’s speech early in the year 2004. Now, in the authors viewpoint, NASA and its new administrator, Sean O’Keefe, have what they need to ensure this vision becomes reality.

To read more reviews, or order the book online, visit Amazon.com.

Review by Mark Mortimer

Posted on by Fraser Cain

Astronaut Gordon Cooper Dies

Gordon Cooper Jr., the astronaut who piloted the sixth and last flight of the Mercury program and later commanded Gemini 5, died earlier today at his home in Ventura, Calif. He was 77 years old.

“As one of the original seven Mercury astronauts, Gordon Cooper was one of the faces of America’s fledgling space program. He truly portrayed the right stuff, and he helped gain the backing and enthusiasm of the American public, so critical for the spirit of exploration. My thoughts and prayers are with Gordon’s family during this difficult time,” said NASA Administrator Sean O’Keefe.

“Cooper’s efforts and those of his fellow Mercury astronauts, Alan Shepard, Gus Grissom, John Glenn, Scott Carpenter, Wally Schirra and Deke Slayton, serve as reminders of what drives us to explore. They also remind us that to succeed any vision for exploration needs the support of the American people.”

“Gordo was one of the most straightforward people I have ever known. What you saw was what you got,” said fellow Mercury astronaut and former U.S. Senator John Glenn, in a statement released by the Astronaut Scholarship Foundation.

Another of the “Original Seven,” Wally Schirra added, “We seven were bonded like brothers, maybe even closer if that’s possible.”

“He never said ‘you can’t do it.’ He was gung ho on everything,” said Norris Gray, the NASA Fire Chief and Emergency Preparedness Officier during the Mercury days. Sam Beddingfield, then Mechanical Engineer for Project Mercury added, “He knew what he was doing and could always make things work.”

“Gordon Cooper’s legacy is permanently woven into the fabric of the Kennedy Space Center as a Mercury Seven astronaut,” said Kennedy Space Center director Jim Kennedy. “His achievements helped build the foundation of success for human space flight that NASA and KSC have benefited from for the past four decades.

“While the KSC family mourns the loss of this space pioneer, we honor his contributions and rest easy knowing his imprint on KSC will last forever. I consider it a privilege to have known Gordon Cooper. On behalf of the KSC family, I extend condolences to the Cooper family and our prayers are with them in their trying days ahead. ”

The youngest of the original seven astronauts, Cooper’s flight in his Faith 7 capsule stretched the capabilities of the Mercury spacecraft to the limits. The mission, May 15 and 16, 1963, lasted more than 34 hours and 22 orbits. That was more than three times the longest U.S. human space flight until that time, and far exceeded the initial design capability of the capsule. During his flight, Cooper also became the first astronaut to sleep in space.

“NASA’s astronauts extend their deepest sympathies to Gordon Cooper’s family,” said Kent Rominger, chief of the astronaut office at NASA’s Johnson Space Center in Houston. “He was among the first pioneers in space and his achievements inspired many of us to pursue our dreams of exploring our universe. We salute his many accomplishments as an astronaut and as a husband and father. He will be truly missed.”

Cooper and Charles “Pete” Conrad Jr. flew the troubled and suspenseful third flight of the Gemini program in August 1965. The goal of the mission was to prove astronauts could survive in space long enough to perform a lunar mission, which takes eight days.

During their eight-day mission, they experienced a number of problems with power systems, thruster fuel, venting gas that caused the spacecraft to roll, and more in a seemingly unending series. But they stayed in orbit for almost 191 hours, 122 orbits in nearly eight days, and got themselves and their spacecraft back intact. In orbit, they accomplished a “shadow rendezvous” with an imaginary spacecraft, an exercise demonstrating it could be done.

The Gemini 5 mission established a new space endurance record at the time, travelling 3,312,993 miles in 190 hours and 56 minutes. Cooper also became the first man to make a second orbital flight and thus won for the United States the lead in man-hours in space by accumulating a total of 225 hours and 15 minutes.

A Life of Service
Leroy Gordon Cooper Jr. was born on March 6, 1927, in Shawnee, Okla. He served in the Marine Corps in 1945 and 1946, then attended the University of Hawaii where he was commissioned a second lieutenant in the U.S. Army.

In 1949 he was called to active duty and completed pilot training in the U.S. Air Force. From 1950 to 1954 he was a fighter pilot in Germany.

Cooper earned a bachelor’s degree at the Air Force Institute of Technology in 1956, then completed test pilot school at Edwards Air Force Base, Calif. He served as a test pilot there until he was selected as a Mercury astronaut.

In addition to his two flights, Cooper was backup command pilot of Gemini 12, launched in November 1965. He also served as backup command pilot for Apollo 10, which flew in May 1969. He left NASA and retired from the Air Force as a colonel on July 31, 1970.

He founded Gordon Cooper and Associates that year and served as president of the consulting firm that specialized in activities ranging from aerospace to hotel and land development projects. Cooper was a director of a number of other organizations, most specializing in energy, advanced electronics systems, efficient homes, boats and marine systems and equipment.

In 1975, he became vice president for research and development for Walter E. Disney Enterprises Inc. of Glendale, Calif., the research and development subsidiary of Walt Disney Productions.

Throughout his life, Cooper pursued a wide range of activities, both professionally and as hobbies. A NASA biography lists his hobbies as treasure hunting, archaeology, racing, flying, skiing, boating, hunting and fishing. Among his numerous awards were the Air Force Legion of Merit, the Distinguished Flying Cross with cluster, NASA’s Exceptional Service Medal, the Collier Trophy and the Harmon Trophy.

He was the first active-duty military man to address joint sessions of Congress twice.

Cooper continued to design and test new aircraft in Southern California, never giving up his passion for pushing the envelope. Cooper told a reporter when he was 71, “I get cranky if I don’t fly at least three times a month.”

Original Source: NASA News Release

Posted on by Fraser Cain

Giant Infrared Space Observatory Considered by NASA

A NASA-led team is studying the construction of a railway in space for a pair of telescopes that will provide views of planet, star, and galaxy formation in unprecedented detail. The proposed Space Infrared Interferometric Telescope (SPIRIT) mission will also examine the atmospheric chemistry of giant planets around other stars.

SPIRIT will consist of two telescopes at opposite ends of a 120-foot (40-meter) beam. The telescopes will move along the beam like cars on a railway, combing their images using the techniques of interferometry to achieve the resolving power of a single giant telescope 120 feet across.

NASA’s Goddard Space Flight Center, Greenbelt, Md., will lead a NASA/university/industry team to develop a preliminary design for SPIRIT. The team will evaluate various mission concepts, create a roadmap of the technology development required for the mission, and generate independent cost assessments.

The study was commissioned in July 2004 by NASA Headquarters, Washington, D.C., as one of nine proposals that will help strategic planning for NASA’s Origins Space Science research theme. NASA’s Origins program seeks to answer the fundamental questions about the universe, such as where we came from and whether or not we are alone. The team will report to the Origins Roadmap Committee in early January, 2005, and a final report is due three months later.

“I’m delighted that SPIRIT was chosen for study,” said Dr. David Leisawitz of NASA Goddard, Principal Investigator for the proposed mission. “We’re going to give NASA a chance to build a telescope that will dazzle the world with crisp, clear infrared pictures of the universe.”

“These images will help us to answer some very profound questions. How did we living critters wind up on a rocky planet bathed in light from the Sun, one of a hundred billion stellar denizens of the magnificently spiral-shaped Milky Way galaxy? Perhaps even more tantalizing, we should expect the unexpected, as that’s what we find whenever a big step is taken to improve the scientific community’s tools. SPIRIT will use techniques pioneered a century ago by Nobel Laureate Albert A. Michelson, so we know it can be done, and I think it’s an excellent match to the Origins mission class envisioned in NASA’s call for proposals,” said Leisawitz.

SPIRIT will examine the universe in the far-infrared and sub-millimeter wavelengths of light. This light is invisible to the human eye, but some types of infrared light are perceived as heat.

The processes that build planets, stars, and galaxies are most readily visible in these kinds of light. For example, stars are born when massive interstellar clouds collapse under their own gravity. The collapse generates heat, causing the central star-forming region of the cloud to glow in infrared. Newborn stars are frequently surrounded by disks of dust and gas, which also collapse under their own gravity to form planets. While the planets are too small to be seen directly, their gravity disturbs the dust disk, forming ripples and lumps. Warmed by the central star, the dust glows in infrared light, revealing the dusty structures to SPIRIT and divulging the locations and sizes of previously unknown planets.

Looking farther into space is equivalent to seeing back in time, because the speed of light is finite, and it takes light a significant amount of time to traverse immense cosmic distances. We see the nearest large galaxy (Andromeda) as it appeared about two million years ago, because that’s how long it took for its light to reach us. We cast our gaze back billions of years by looking toward the limit of the observable universe, and thus can watch galaxies as they evolve. However, since the universe is expanding, light emitted by remote galaxies has been stretched by the expansion of space to infrared and sub-millimeter wavelengths, so we need telescopes highly sensitive to these types of light to observe distant galaxy formation.

Many of these objects appear too small, or shine too faintly at their remote distances for existing telescopes to observe in great detail. To accomplish such ambitious observations, SPIRIT will have 100 times the angular resolution (ability to see fine detail) than existing infrared telescopes, complemented with a matching improvement in sensitivity.

Technical challenges to overcome include keeping the telescope mirrors extremely cold (about 4 degrees Kelvin or minus 452 degrees Fahrenheit) so their own heat does not obscure the faint infrared light they are trying to collect. The detectors also need to have greater sensitivity and more pixels. The Goddard/industry team is up to the challenge: “Our engineers love working on this project; there’s a lot of room for creative thought, and everyone understands that this is an opportunity to take a giant leap forward scientifically while inspiring the next generation of explorers.” says Leisawitz.

If approved, SPIRIT could be ready for launch in 2014, on board a large expendable rocket. SPIRIT would travel to the L2 libration point one million miles from Earth where it will automatically unfold its beam and deploy the telescopes. The Goddard-led team includes collaborators from Caltech, Cornell, the Harvard-Smithsonian Center for Astrophysics, the University of Maryland, the Massachusetts Institute of Technology, the Naval Research Laboratory, Princeton, the University of California, Los Angeles, the University of Wisconsin, and NASA’s Jet Propulsion Laboratory and Marshall Space Flight Center. The industry team includes Ball Aerospace, Boeing, Lockheed-Martin, and Northrop-Grumman.

Original Source: NASA News Release