Houston, U.S.A. – NASA completed another successful test of the Orion crew vehicle’s parachutes high above the Arizona desert in preparation for the spacecraft’s orbital flight test in 2014. Orion will carry astronauts deeper into space than ever before, provide emergency abort capability, sustain the crew during space travel and ensure a safe re-entry and landing.

A C-17 plane dropped a test version of Orion from an altitude of 25,000 feet above the U.S. Army Yuma Proving Ground in southwestern Arizona. This test was the second to use an Orion craft that mimics the full size and shape of the spacecraft.

Orion’s drogue chutes were deployed between 15,000 feet and 20,000 feet, followed by the pilot parachutes, which deployed the main landing parachutes. Orion descended about 25 feet per second, well below its maximum designed touchdown speed, when it landed on the desert floor.

“Across the country, NASA and industry are moving forward on the most advanced spacecraft ever designed, conducting drop and splashdown tests, preparing ground systems, designing software and computers and paving the way for the future of exploration,” said William Gerstenmaier, associate administrator for the Human Exploration and Operations Mission Directorate at NASA Headquarters inWashington. “Today’s parachute test in Yuma is an important reminder of the progress being made on Orion and its ultimate mission — enabling NASA to meet the goal of sending humans to an asteroid and Mars.”

Orion parachutes have so-called reefing lines, which when cut by a pyrotechnic device, allow the parachute to open gradually, managing the initial amount of drag and force on the parachute. The main objective of the latest drop test was to determine how the entire system would respond if one of the reefing lines was cut prematurely, causing the three main parachutes to inflate too quickly.

Since 2007, the Orion program has conducted a vigorous parachute air and ground test program and provided the chutes for NASA’s successful pad abort test in 2010. All of the tests build an understanding of the chutes’ technical performance for eventual human-rated certification.

In 2014, an uncrewed Orion spacecraft will launch from Cape Canaveral Air Force Station in Florida on Exploration Flight Test-1. The spacecraft will travel 3,600 miles above Earth’s surface. This is 15 times farther than the International Space Station’s orbit and farther than any spacecraft designed to carry humans has gone in more than 40 years. The main flight objective is to understand Orion’s heat shield performance at speeds generated during a return from deep space.

In 2017, Orion will be launched by NASA’s Space Launch System (SLS), a heavy-lift rocket that will provide an entirely new capability for human exploration beyond low Earth orbit. Designed to be flexible for launching spacecraft for crew and cargo missions, SLS will enable new missions of exploration and expand human presence across the solar system.

Image Courtesy of  nasa hq photo

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Interstellar Boundary Explorer (IBEX) has captured the best and most complete glimpse yet of what lies beyond the solar system. The new measurements give clues about how and where our solar system formed, the forces that physically shape our solar system, and the history of other stars in the Milky Way.

The Earth-orbiting spacecraft observed four separate types of atoms including hydrogen, oxygen, neon and helium. These interstellar atoms are the byproducts of older stars, which spread across the galaxy and fill the vast space between stars. IBEX determined the distribution of these elements outside the solar system, which are flowing charged and neutral particles that blow through the galaxy, or the so-called interstellar wind.

“IBEX is a small Explorer mission and was built with a modest investment,” said Barbara Giles, director of the Heliophysics Division at NASA Headquarters in Washington. “The science achievements though have been truly remarkable and are a testament to what can be accomplished when we give our nation’s scientists the freedom to innovate.”

In a series of science papers appearing in the Astrophysics Journal on Jan. 31, scientists report finding 74 oxygen atoms for every 20 neon atoms in the interstellar wind. In our own solar system, there are 111 oxygen atoms for every 20 neon atoms. This translates to more oxygen in any part of the solar system than in nearby interstellar space.

“Our solar system is different than the space right outside it, suggesting two possibilities,” says David McComas, IBEX principal investigator, at the Southwest Research Institute in San Antonio. “Either the solar system evolved in a separate, more oxygen-rich part of the galaxy than where we currently reside, or a great deal of critical, life-giving oxygen lies trapped in interstellar dust grains or ices, unable to move freely throughout space.”

The new results hold clues about the history of material in the universe. While the big bang initially created hydrogen and helium, only the supernovae explosions at the end of a star’s life can spread the heavier elements of oxygen and neon through the galaxy. Knowing the amounts of elements in space may help scientists map how our galaxy evolved and changed over time.

Scientists want to understand the composition of the boundary region that separates the nearest reaches of our galaxy, called the local interstellar medium, from our heliosphere. The heliosphere acts as a protective bubble that shields our solar system from most of the dangerous galactic cosmic radiation that otherwise would enter the solar system from interstellar space.

IBEX measured the interstellar wind traveling at a slower speed than previously measured by the Ulysses spacecraft, and from a different direction. The improved measurements from IBEX show a 20 percent difference in how much pressure the interstellar wind exerts on our heliosphere.

“Measuring the pressure on our heliosphere from the material in the galaxy and from the magnetic fields out there will help determine the size and shape of our solar system as it travels through the galaxy,” says Eric Christian, IBEX mission scientist, at NASA’s Goddard Space Flight Center in Greenbelt, Md.

The IBEX spacecraft was launched in October 2008. Its science objective is to discover the nature of the interactions between the solar wind and the interstellar medium at the edge of our solar system.

The Southwest Research Institute developed and leads the IBEX mission with a team of national and international partners. The spacecraft is one of NASA’s series of low-cost, rapidly developed missions in the Small Explorers Program. Goddard manages the program for the agency’s Science Mission Directorate at NASA Headquarters in Washington.

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Earlier this month, NASA (National Aeronautics and Space Administration) once again found groundbreaking evidence that water once existed on Mars. The rover, Opportunity, has discovered a long, thin vein of gypsum deposit, found on the edge of the crater, Endeavor.

In January 2004, NASA sent the twin rovers, Opportunity and Spirit, to Mars as a part of the Mars Exploration Rover Mission to find clues that water once existed. Opportunity and Spirit discovered gypsum to be as much of a common mineral on Mars as it is on Earth. Gypsum, which is used as drywall and as an ingredient for plaster, is found evaporated in sedimentary environments, particularly in saline water beds (or seawater) containing high amounts of dissolved calcium sulfate (CaSO₄).

Since their landing on Mars, the rovers found, in the northern sand dunes, numerous pieces of gypsum, which were blown by winds and, hence, mixed with other minerals and materials. These dunes are similar to the White Sands National Monument located in New Mexico, where the sands are comprised of gypsum crystals. This discovery is one of the few that proves that water existed on Mars, but from where the gypsum originates baffles scientists.

Sometime in early 2010, Spirit had discontinued its mission due to being stuck and its eventual inability to communicate. Opportunity, on the other hand, has remained alive and active, and eventually found the gypsum deposit, slightly jutting out from the bedrock. The vein is approximately 2 cm wide and 50 cm long.

Although this discovery may seem redundant with the ones made in the past, it turns out that this strand of gypsum is more significant than the pieces found in dunes. Not only does it appear to have formed in place, but the deposit tells us that water once flowed through a crevice long ago.

“That can’t be said for other gypsum seen on Mars or for other water-related minerals Opportunity has found,” remarks Steve Squyres, a planetary scientist at Cornell University. “It’s not uncommon on Earth, but on Mars, it’s the kind of thing that makes geologists jump out of their chairs.”

Opportunity and Spirit have analyzed most Martian areas to be acidic – and definitely not suitable for life. However, the spot in which the gypsum deposit was found does contain the substances that cause acidity. Thus, the water may have been more neutral. Not only is the vein a sure sign that Mars once did have water, it also proves that the red and dusty planet may have been more habitable than we thought.

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Earlier this week, the spacecraft, Kepler, discovered two exoplanets around the size of the earth – the first of their kind – orbiting a sun-like star. Named Kepler-20e and Kepler-20f, these exoplanets are a part of the star system, Kepler-20, which lies 950 light years away from Earth near the constellation, Lyra.

“This discovery demonstrates for the first time that Earth-size planets exist around other stars and that we are able to detect them,” says Dr. Francois Fressin, an astronomer at the Harvard-Smithsonian Center for Astrophysics in Cambridge, Massachusetts.

Launched in 2009, Kepler is a space telescope built and sent by NASA to detect Earth-like exoplanets (also known as extrasolar planets, which are planets that exist outside our solar system) orbiting stars in habitable zones. Its most recent, significant discovery occurred in early December, when it detected the Neptune-sized Kepler-22b, the first of its kind that has been seen orbiting in the “Goldilocks zone” and that might possibly have water and life.

Kepler took a step closer in accomplishing its mission when it detected Kepler-20, Kepler-20e, and Kepler-20f. Kepler-20 is similar to the sun, in that it is a G-type star. It is yellowish, though a bit smaller and cooler. The star contains five planets in total, all of which orbit it closer than Mercury orbits the sun. The three other planets are gas giants, which are about the size of Neptune, and each planet orbits alternating in size.

These newly discovered exoplanets are only Earth-like in their sizes and rocky composition. Kepler-20e orbits its star every 6.1 days, and its temperature is 1400° F. Its diameter, 6900 miles, is 0.87 times the diameter of the Earth’s. Kepler-20f has an orbit of 19.6 days. It has the temperature of 800° F, and it is 1.03 times Earth’s diameter, being 8,200 miles.

Because of their close orbits and high temperatures, these two exoplanets are not able to sustain water, let alone life. For them to have water and life, they have to lie in the “Goldilocks zone,” or the habitable zone, in which a planet cannot be too close or too far (hence, too hot or too cold) from the star it orbits.

Ever since its launch in 2009, Kepler has been detecting hundreds of exoplanets, many of which are not Earth-like, being hostile and sometimes lonely, not orbiting any stars. With its most recent detection of Kepler-22b and of Kepler-20′s two Earth-like planets, Kepler has reached a new landmark, not just in its journey, but in our knowledge of the various kinds of planets that exist in the observable universe.

“This could be an important milestone,” Dr. Fressin states. “I think 10 years, or maybe even 100 years, from now people will look back and ask when was the first Earth-sized planet found. It is very exciting.”

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The Drake equation is a probability law which estimates the abundance of intelligent life in our Galaxy, the Milky Way. It is quite simple in appearance, and anyone can play with the variables in order to make their own personal estimate.

The variables encountered in the equation include the proportion of intelligent to non-intelligent life; the proportion of stars which would be capable of sustaining life in their environment to those who cannot; the number of planets a star is probable to have existing in this habitable zone, if the star were to harbour planets.

Although the scientific results of this equation are in great debate, it was developed by Prof. Frank Drake in order to open discussion on the topic for the famous meeting at the Green Bank radio observatory in 1961.

Current estimates ranging from the opinions of pessimists to optimists, are of the order of it being next to impossible to communicate with other lifeforms in our Galaxy, to a possible ten different alien civilisations who are currently in the same positions as us with appropiate technology who could be trying to communicate with us and others like us.

Hence the popularity of the SETI project (the Search for Extraterrestrial Intelligence). The equation brings many interesting topics to light such as how long intelligent civilisations may continue on living, with most estimates being of short duration. One hypothesise is that once nuclear power is developed by a civilisation, they will quickly destroy themselves through their new technology.

To date there have been 684 confirmed planets discovered orbiting a total number of 474 stars other than our Sun. With thousands more proposed from the Kepler mission awaiting comfirmation. More recently the Kepler mission has discovered the first planet known to be orbiting two stars.

The techniques involved in detecting these extra-solar (i.e. orbiting other stars than our Sun) objects favor the discovery of larger, more massive planets which have a more visible influence on their parent star. The techniques follow principles as simple as; does the parent star wobble?

If so, by how much and then knowing the distance to the parent star we can calculate the mass of the orbiting planet and orbital period, which in turn would give us the distance between the parent star and planet, using Kepler’s third law. This technique follows the principles of astrometry (basically astronomical geometry).

Then from analyzing the richness of the chemical environment of such systems through spectroscopy it is possible to say if at least one component of this system would be capable of sustaining life. Unfortunately, due to the large number of complexities which arise in the observational and analysis stages no one can say for sure if these planets are currently harbours of life.

However, all is not lost as we know already that our solar system contains life on a small out of the way planet amicably called Earth. So would it be possible for other lumps of rock in our Galaxy to host complex biological species? It is of popular opinion that yes, it is possible but due to the harsh environments in which they may exist they may not of had the possibility to evolve beyond microbial stages of evolution.

For example, if we ignore Mars for a minute and concentrate on the more probable hosts, the Gaililean satelites orbiting our local failed star Jupiter or Saturn’s Titan are good bets. It was initially thought that light was a neccessary ingredient for life to come into being. That was until the discovery of strange looking creatures living in the depths of our deepest darkest oceans close to hydrothermal vents.

This would lead a reasonable mind to believe that Europa, Ganymede or Titan may be hosts to such creatures thanks to their water ice crusts encasing their volcanic prone H2O oceans. How could we detect such life? Well as we know from studies of biological creatures back home we create a chemical diversity in our atmosphere which wouldn’t exist if we did not.

So we could look for gases such as methane trapped in ice crystals such as Clathrate Hydrates on the surface of these near by objects, with techniques such as infra-red reflection spectroscopy.

An exo-planet nicknamed ‘Snow White’ has been found to have a partially water ice surface with a possible light methane atmosphere. So in conclusion, no life has been currently detected aside from on planet Earth and it will prove difficult to find, but, we are off to a good start.

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