Posted on by Nancy Atkinson

Extracting Water From the Moon With Basic Home Appliances

Two scientists have cooked up a way to get water and oxygen from the moon. And to test their idea, they used a basic kitchen microwave oven. “This is exploration,” said Dr. Bill Kaukler of the University of Alabama in Huntsville’s Center for Materials Research. Kaukler and Dr. Ed Etheridge of Marshall Space Flight Center have proposed using microwaves to draw water from below the lunar surface. To do this, microwaves would be “shot” at the moon, likely from an orbiting spacecraft. But to test their theory, Kaukler and Etheridge didn’t build an elaborate test site. They just put a plate of simulated lunar regolith in a microwave oven and “nuked” it for a few minutes.

Kaukler said they were inspired by the results of 1994’s Clementine mission which uncovered the possible existence of ice within some of the craters at the moon’s poles. This discovery was confirmed in early 1998 by NASA’s lunar prospector. Scientists believe the ice was brought to the moon the same way water was brought to Earth – by comets crashing into the surface.

“If you estimate, there would be billions of tons of water,” Ethridge said.

The surface is covered by regolith, or silicate rock that is the lunar version of top soil. It’s about two meters deep “and where you have silicates, you have oxygen,” said Kaukler. “That makes it worthwhile to extract, and, one of the beauties of this is we don’t have to dig.”

Digging could stir up the fine, gritty dust. The microscopic particles then could adversely affect the astronauts’ spacesuits and their equipment, he said.

To get to the water, microwaves would be shot into the regolith, “thawing” the ice to about minus-50 degrees Celsius. Water vapor would be drawn to the surface by the moon’s vacuum environment. The water vapor is then collected on a plate as ice and scraped off to be used as water for the astronauts. The hydrogen and oxygen can also be separated through electrolysis to use as fuel for a trip to Mars.

In their Marshall lab, the scientists used a microwave oven, a vacuum, water and a simulant to regolith to verify their findings.

“We put some water in the simulant and placed it inside the microwave,” Kaukler said. “Then, we used the vacuum to replicate the lunar atmosphere.

“We were able to get about 95 percent of the water back in about two minutes.”

Other uses of microwaves would be to “melt” the lunar surface. The process would help create dust-free landing and launch sites as well as smoother floors for structures and roads for traveling without kicking up dust.

“For surface site preparation, the microwaves would melt the top layer, glazing it, so it’s not all dust,” Ethridge said. “It would create a cobblestone effect.”

So if the moon had water, oxygen and useable real estate, it might be a financially viable place to colonize.

“Since we’re planning to go to the moon and Mars, the idea is to save weight (on the flight) and to extract the materials the astronauts would need – oxygen and water,” said Kaukler. “There have been studies that showed (getting the water) to be economically viable,” he said. “It could be the first commercial venture.”

Source: Huntsville Alabama Times

Posted on by Nancy Atkinson

Galaxy Ramming Through Space Creates Fireballs

Fireball Galaxy. Credit: Subaru Telescope, National Astronomical Observatory of Japan (NAOJ)

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During routine observations of the Coma Cluster of galaxies using the Subaru Telescope in Hawaii, astronomers discovered a thread-like structure stretching from one of the galaxies. The astronomers determined this filament was about 260 thousand light years long, and spectral analysis of the filament suggested a younger age toward the outer edge of the filament. The filament also has many young stars surrounded by ionized gas that look like projectiles flying out from the galaxy. So what happened in this chaotic area of space? Astronomers determined a speeding galaxy rammed into the Coma Cluster, stripping gas from the galaxy and creating fireball-like projectiles.

Galaxies evolve over time, and astronomers do not yet understanding how they change in shape, size, and color. Galaxy Clusters, which are dense populations of galaxies, rich with hot intergalactic gas, accompanied by strong gravitational forces are some of the best locations to observe galactic evolution.

A team of researchers from the National Astronomical Observatory of Japan and the University of Tokyo used Suprime-cam on the Subaru Telescope to observe the Coma Cluster of galaxies. The Coma Cluster contains over 1,000 galaxies and is fairly close to Earth at about 300 million light years away.
During observations in 2006 and 2007, the astronomers saw the filament extending from Galaxy RB199 and several of the “fireballs.” Detailed study identified several bright knots connected by blue filamentary structures, and the knots are actually the clusters of young stars weighing 10 million times our Sun, contained in an area about 3000 to 6000 light years across. Because the knots are accompanied by ionized gas, active star formation is going on in the fireballs where usually far less star formation would be expected. The team noted that the size and the mass of the fireballs indicate they could develop into dwarf galaxies.

Closeups of four fireballs. Subaru Telescope, National Astronomical Observatory of Japan (NAOJ)
Closeups of four fireballs. Subaru Telescope, National Astronomical Observatory of Japan (NAOJ)

Because the inside of the cluster is crowded with galaxies, they pass by each other and crash into each other. The team thought that the tidal forces during such encounters could strip gas or stars from the galaxies. They also postulated that as a galaxy falls into the center of the cluster the gravitational forces of the cluster could remove the gas and stars from that galaxy. Both scenarios are possible, however, the research team found that these mechanisms could hardly explain the characteristics of the fireballs. The team then realized that ram pressure stripping occurs when superheated gas (several tens of million Kelvin) in the cluster and the galaxies collide at high speeds. Previous X-ray observation shows the presence of large amounts of hot ionized gas in the middle of the Coma Cluster while RB199 crashes into the center at a speed of 1200 miles per second, causing strong friction with this hot gas. As such, the team concluded that the ram pressure has enough power to strip the gas from the galaxy AND create the fireballs.

While there are several reports indicating ram pressure stripping in nearby galaxy clusters, the identification of fireballs in this study is the first to demonstrate the stripped gas turns into stars while traveling through remote space far away from its source. Similar phenomena have been observed in galaxy clusters much further away at several billions light years, however, those distant cases were interpreted through witnessing the transitional phase of galaxies changing their morphology or colors as they fall into a cluster. The fireballs discovered by this team of Japanese astronomers provide the first sample of such structures in a nearby cluster. Principal investigator, Dr. Michitoshi Yoshida, said “the team is confident that our study of these phenomena leads to a better understanding of the gas stripping processes in galaxy clusters, and the effect of clusters on the evolution of individual galaxies”.

Source: Subaru Press release

Posted on by Fraser Cain

Core of Uranus

Uranus Compared to Earth. Image credit: NASA

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Uranus has a mass of roughly 14.5 times that of Earth, which makes it the least massive of the giant planets. Astronomers know that it’s mostly made of various ices, like water, ammonia and methane. And they theorize that Uranus probably has a solid core.

The core of Uranus probably only accounts for 20% of the radius of Uranus, and only about 0.55 Earth masses. With gravity of all the outer mantle and atmosphere, regions in the core experience a pressure of about 8 million bars, and have a temperature of 5,000 Kelvin. That sounds hot, like as hot as the surface of the Sun, but keep in mind that the core of Jupiter is more like 24,000 K – much hotter. The core of Uranus has a density of about 9 g/cm3, which makes it about twice as dense as the average density of the Earth.

For astronomers, Uranus has an unusually low temperature; and that’s a mystery. One ideas is that the same impact that knocked Uranus off its rotational axis might have also caused it to expel much of its primordial heat. With the heat gone, Uranus was able to cool down significantly further than the other planets. Another idea is that there’s some kind of barrier in Uranus’ upper atmosphere that prevents heat from the core to reach the surface.

We have written many stories about Uranus on Universe Today. Here’s an article about a dark spot in the clouds on Uranus, and here’s an article about the composition of Uranus.

If you’d like more info on Uranus, check out Hubblesite’s News Releases about Uranus. And here’s a link to the NASA’s Solar System Exploration Guide to Uranus.

We have recorded an episode of Astronomy Cast just about Uranus. You can access it here: Episode 62: Uranus.

Posted on by Nancy Atkinson

Asteroid To Enter Earth’s Atmosphere Tonight (Oct. 6)

Looking for a little excitement tonight? An asteroid between 1-5 meters (3-15 feet) was discovered just hours ago at an Arizona observatory, and might provide a spectacular light show as it comes through Earth’s atmosphere. But don’t be alarmed – scientists predict it will be harmless and burn up before it reaches the ground. It is expected to be visible over eastern Africa, at approximately 2:46 a.m. Greenwich Mean Time (10:46 p.m. Eastern time ). There is no danger to people or property since the asteroid will not reach the ground. It will burn up in the upper atmosphere, well above aircraft heights. A brilliant fireball will be visible as a result. “We want to stress that this object is not a threat,” said Dr. Timothy Spahr, director of the International Astronomical Union’s Minor Planet Center. “We’re excited since this is the first time we have issued a prediction that an object will enter Earth’s atmosphere,” Spahr added. Odds are between 99.8 and 100 percent that the object will encounter Earth, according to calculations provided by Andrea Milani of the University of Pisa.

When a meteoroid (small asteroid) enters the atmosphere, it compresses the air in front of it. That compression heats the air, which in turn heats the object, causing it to glow and vaporize. Once it starts to glow, the object is called a meteor.

“A typical meteor comes from an object the size of a grain of sand,” explained Gareth Williams of the Minor Planet Center. “This meteor will be a real humdinger in comparison!”

The meteor is expected to be visible from eastern Africa as an extremely bright fireball traveling rapidly across the sky from northeast to southwest. The object is expected to enter the atmosphere over northern Sudan at a shallow angle.

“We’re eager for observations from astronomers near the asteroid’s approach path. We really hope that someone will manage to photograph it,” said Williams

Source: Center for Astrophysics Minor Planet Center

Image source

Posted on by Tammy Plotner

How To Use A Telescope

Choose Your Observing Site To Use A Telescope

One of the most important things to begin with is to carefully choose the site you will use set up and use your telescope at. While it would be tempting to take your new telescope out of the box and use it that night, it’s best to wait just a day or two! Begin the first clear night by going outside a taking a good look around. You want to choose an observing site where the view is as unobstructed and as dark as possible. While you are doing this, keep in mind that it must be comfortable to you as well. While the vista might be far improved a kilometer away – do you really want to have to take your equipment that distance each time you want to use it? Look at many different alternatives. If you live in a city, perhaps a rooftop will serve well. Urban settings often have very suitable yards that will work for most observing projects and rural settings are ideal.

Light pollution is another factor when choosing your site. Again, keep in mind that you must have a site that is accessible to enjoy. It isn’t always possible if you live in a well-lit area to take your equipment remote each time you want to use your telescope – but a sheltered area, such as in the shadow of a house, often blocks stray light well enough to enjoy using your telescope right at home. Of course, finding a dark sky site is also important, too. But not half as much as just finding a spot that you will enjoy and use.

While out during the day, look for level, solid ground. No one wants to see their telescope take a tumble. While it is tempting to set up on a deck, remember that any footsteps will cause vibration in the image. Setting up on places like a blacktop driveway or concrete can also cause thermal issues, too. Avoid them when you can, but do not discard these types of sites if they are comfortable and accessible.

How To Set Up Your Telescope

While every telescope set-up is slightly different, they are all basically the same in some respects. There must be an optical tube of some type, a mount and eyepieces. Take the time to become familiar with all the components of your telescope! If you must assemble and dis-assemble your telescope each time you use it, it’s a very wise idea to practice a few times before you go out in the dark. There is simply nothing more frustrating that trying to learn to set up your equipment when you cannot see what you are doing – or to loose a small part in the dark. If it is at all possible, leave your telescope and tripod fully assembled and in a place where it is easy to set outside at a moment’s notice. You’ll find that you’ll use it far more often if it takes less work.

Your telescope’s view is also dependent on ambient temperature. If you wear eyeglasses, you understand why! If you go from a very cool environment, such as a air-conditioned house, into a humid outdoors setting, your glasses fog up, don’t they? And so will your telescope’s optics. The same is true when observing outdoors in the winter. When taking your telescope from a heated climate to a cold one, you must give the telescope time to “cool down”. Even just a few degrees can mean waiver in the image.

Align your finderscope in advance! While this sounds rather strange, another frustrating thing to do in the dark is to align a finderscope – especially on a moving target. Once you have learned to assembly your telescope, learn to align your finder. Set up your scope and aim at a distant object. Now align your finder to that object as well. This will make things much easier, later!

Once your telescope is set up, the last thing to remember is to stow your things neatly so you won’t have any problems finding them when it comes time to put things away. Dust covers and eyepieces cases are so easy to lose. Keep things neat and you won’t have any problems. Choose the eyepiece you think you will need in advance and have them in a place where you won’t need to fumble in the dark. Have your red flashlight and maps handy. These are just little things that make using your telescope much more enjoyable!

Choose Your Observing Times

Experience will become your best teacher. It won’t take long before you realize that very humid nights or exceptionally cold ones are not particularly good times to observe. Unless you plan on looking at the Moon itself, nights that are well moon-lit are also not good times to search for a faint galaxy, either. Little things, like waiting for a planet to clear the atmospheric “murk” at the lower horizon mean a much better viewing experience.

How To Use A Telescope

Now that you have your observing site, learned to set up, and established a time to practice astronomy… Let’s learn how to use your telescope!

If you have an equatorial mount, align the axis to the pole star. Altazimuth mounts do not need this step. Take off your dustcaps and stow them away. Double check to make sure your tripod legs are secure. Choose your low power eyepiece and put it in the focuser. Are you ready? Now, loosen the axis and take aim at a star using your finderscope. When the star is aligned in the center of the finder, tighten the axis and it’s time to go to the eyepiece. Gently adjust the focus in or out until you have a crisp, clean image. Now watch the star move. This direction is always west – regardless of the orientation in the eyepiece. For equatorial mounts, use your slow motion cables to learn to “track” the star. For altazimuth mounts, use the pan control or shift the tube manually (dobsonian models). Once you have learned to “follow” and object, it’s time to star hop!

Each time you go to a new object with an equatorial mount, you must unlock the axis. The same is true with some styles of altazimuth mounts. Once you have the general location in the finder, lock the axis back up and use the slow motion cable controls or panhandle control to make small moves. Using a low power eyepiece first will help you locate things much easier, and you can then switch to more magnification once the object is located.

When you are finished for the evening, make sure to replace all your dustcaps. If your optics should become dewed, don’t wipe them off. Allow them to air dry to avoid micro-scratches on delicate coatings. Always make sure to give your observing area one last check before leaving just in case you’ve forgotten something!

Posted on by Tammy Plotner

A Herschel Anniversary – NGC 891 by Ken Crawford

NGC891 by Ken Crawford

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On this night – October 6 – in 1784, Sir William Herschel was busy at the eyepiece of his telescope with a new galaxy he’d just discovered. It was a beauty, too. A pencil-slim, edge-on galaxy with a dark dust lane. Herschel marked it down in his fifth catalog as discovery 19, but when he got excited talking about his sister Caroline’s discoveries, he made a mistake. Let’s learn…

Even though William Herschel later confused NGC 891 with Caroline’s independent discovery of NGC 205 (M110), you can understand how the brother/sister astronomy team could honestly make a mistake. In the words of Caroline Herschel; “I knew too little of the real heavens to be able to point out every object so as to find it again without losing too much time by consulting the Atlas. But all these troubles were removed when I knew my brother to be at no great distance making observations with his various instruments on double stars, planets, etc., and I could have his assistance immediately when I found a nebula, or cluster of stars, of which I intended to give a catalogue; but at the end of 1783 I had only marked fourteen, when my sweeping was interrupted by being employed to write down my brother’s observations with the twenty-foot.”

Oddly enough, Herschel’s mistake was perpetuated by Admiral William Henry Smyth – who when he retired from the Royal Navy spent his time in his private observatory equipped with a 6-inch refractor. There he observed a variety of deep sky objects, including double stars, clusters and nebulae, and kept careful records of his observations, publishing his work as the “Cycle of Celestial Objects” – including Herschel’s mistake. But in the end, does it really matter which Herschel discovered it? It’s what’s out there that counts…

Located some thirty million light years away in the Local Super Cluster, NGC 891 is wrapped by a cold, gaseous halo. According to Tom Oosterloo (et al); “HI observations are among the deepest ever performed on an external galaxy. They reveal a huge gaseous halo, much more extended than seen previously and containing almost 30 % of the HI. This HI halo shows structures on various scales. On one side, there is a filament extending (in projection) up to 22 kpc vertically from the disk. Small halo clouds, some with forbidden (apparently counter-rotating) velocities, are also detected. The overall kinematics of the halo gas is characterized by differential rotation lagging with respect to that of the disk. The lag, more pronounced at small radii, increases with height from the plane. There is evidence that a significant fraction of the halo is due to a galactic fountain. Accretion from intergalactic space may also play a role in building up the halo and providing low angular momentum material needed to account for the observed rotation lag. The long HI filament and the counter-rotating clouds may be direct evidence of such accretion.”

Accretion? Accretion from where? Is NGC 891 gathering material from somewhere else? Apparently so. According to work of Mapelli (et al): “It has been known for a long time that a large fraction of disc galaxies are lopsided. We simulate three different mechanisms that can induce lopsidedness: flyby interactions, gas accretion from cosmological filaments and ram pressure from the intergalactic medium. Comparing the morphologies, HI spectrum, kinematics and m = 1 Fourier components, we find that all of these mechanisms can induce lopsidedness in galaxies, although in different degrees and with observable consequences. The time-scale over which lopsidedness persists suggests that flybys can contribute to ~20 per cent of lopsided galaxies. We focus our detailed comparison on the case of NGC 891, a lopsided, edge-on galaxy with a nearby companion (UGC 1807). We find that the main properties of NGC 891 (morphology, HI spectrum, rotation curve, existence of a gaseous filament pointing towards UGC 1807) favour a flyby event for the origin of lopsidedness in this galaxy.”

Ah, ha! So, we have a nearby companion galaxy. We’ve learned recently that combining galaxies produces starburst activity and the case is true of NGC 891 as well. Studies done as recently as June 2008 indicate starbust activity based on the strength of the polycyclic aromatic hydrocarbon (PAH) features. And where are those PAHs? Why, in the halo, of course. According to the work of Rand (et al): “We present infrared spectroscopy from the Spitzer Space Telescope at one disk position and two positions at a height of 1 kpc from the disk in the edge-on spiral NGC 891, with the primary goal of studying halo ionization. Our main result is that the [Ne III]/[Ne II] ratio, which provides a measure of the hardness of the ionizing spectrum free from the major problems plaguing optical line ratios, is enhanced in the extraplanar pointings relative to the disk pointing. Using a 2D Monte Carlo-based photoionization code that accounts for the effects of radiation field hardening, we find that this trend cannot be reproduced by any plausible photoionization model and that a secondary source of ionization must therefore operate in gaseous halos. We also present the first spectroscopic detections of extraplanar PAH features in an external normal galaxy. If they are in an exponential layer, very rough emission scale heights of 330-530 pc are implied for the various features. Extinction may be non-negligible in the midplane and reduce these scale heights significantly. There is little significant variation in the relative emission from the various features between disk and extraplanar environment. Only the 17.4 ?m feature is significantly enhanced in the extraplanar gas compared to the other features, possibly indicating a preference for larger PAHs in the halo.”

So where is all this going? Current research shows a correlation between PAH abundance with galactic age. When asymptotic giant branch cough their carbon dust back into the interstellar medium at the end of their evolution, they become the primary source of PAHS and carbon dust in galaxies. As we know, a galaxy is one big recycling plant, and the ejecta is returned back to the interstellar medium after a few hundred million years along the line of main sequence evolution. But, the filamentary pattern extending away from the galactic disc of NGC 891 may very well point to stellar supernova explosions. By contrast, those, huge, massive stars that end up as Type II supernovae are the ones that blast dust and metals everywhere the moment they form.

So is this the result of old – or new – activity? According to Popescu (et al): “We describe a new tool for the analysis of the UV to the sub-millimeter (sub-mm) spectral energy distribution (SED) of spiral galaxies. We use a consistent treatment of grain heating and emission, solve the radiation transfer problem for a finite disk and bulge, and self-consistently calculate the stochastic heating of grains placed in the resulting radiation field. We use this tool to analyse the well-studied nearby edge-on spiral galaxy NGC 891. First we investigate whether the old stellar population in NGC 891, along with a reasonable assumption about the young stellar population, can account for the heating of the dust and the observed far-infrared and sub-mm emission. The dust distribution is taken from the model of Xilouris et al. (1999), who used only optical and near-infrared observations to determine it. We have found that such a simple model cannot reproduce the SED of NGC 891, especially in the sub-mm range. It underestimates by a factor of 2-4 the observed sub-mm flux. A number of possible explanations exist for the missing sub-mm flux. We investigate a few of them and demonstrate that one can reproduce the observed SED in the far-infrared and the sub-mm quite well, as well as the observed radial profile at 850 mu m. For the models calculated we give the relative proportion of the dust radiation powered by the old and young stellar populations as a function of FIR/sub-mm wavelength. In all models we find that the dust is predominantly heated by the young stellar population.”

Although it may have been busy at one time, NGC 891 is quiet now. According to Rowan Temple, “Using a sample of other local galaxies, we compare the X-ray and infrared properties of NGC 891 with those of `normal’ and starburst spiral galaxies, and conclude that NGC 891 is most likely a starburst galaxy in a quiescent state.” So take a look when you have time. This magnitude 10 beauty is located at (RA 2 : 22.6 Dec +42 : 21) at is often considered to be one of the finest deep sky objects Messier never cataloged.

No matter which Herchel discovered it.

Many thanks to AORAIA member Ken Crawford for the use of his superb image!

Posted on by Nancy Atkinson

MESSENGER’s Second Flyby of Mercury: Awaiting Data

Mercury, prior to MESSENGER's closest approach. Credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington

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This morning at 4:40 am EDT, the MESSENGER spacecraft passed only 200 kilometers (124 miles) above Mercury’s surface as it made its second flyby of the mission. Now, the spacecraft is speeding away from Mercury, continuing its science observations for about 20 hours following closest approach. This flyby should provide the first global perspective of Mercury, as, if all went well, we should have images in total covering about 95 percent of the planet. “This second flyby will show us a completely new area of Mercury’s surface, opposite from the side of the planet we saw during the first,” said Louise M. Prockter, scientist for the mission.

If you’re looking for images and data from the flyby here, sorry to disappoint, but data will be transmitted to Earth only after the completion of all science observations. So, for now, even the MESSENGER science team has to wait. But scientists are already eagerly exploring the optical navigation images acquired just prior to the flyby. Shown here is a Narrow Angle Camera (NAC) image from the eighth and final optical navigation image set, taken about 14.5 hours before the flyby’s closest approach.

As in the earlier seven sets, Mercury appears as a thin sunlit crescent. Though much of Mercury is in darkness in this image, the visible portion had never been seen by spacecraft before. This portion of Mercury’s surface was not viewed during any of Mariner 10’s three flybys or during MESSENGER’s first flyby earlier this year. The newly imaged terrain shows a wide range of geologic features, and scientists have marked them on the image. Near the northern limb of the planet, extensive smooth plains, possibly volcanic in origin, are identified. A nearby crater is the brightest feature visible in the image, suggesting a relatively young age. In the southern region, a large basin is seen with a smooth floor, likely also a product of volcanism. A large scarp that appears to cut through this basin may have formed as Mercury cooled and contracted.

For this flyby, MESSENGER was a “green” spacecraft – meaning it didn’t require the firing of its thrusters to fly precisely where the scientists wanted to make observations. Instead, engineers used a type of “solar sailing,” to guide the spacecraft. “There are no refueling station in interplanetary space, so we’re stuck with the amount of fuel we had at launch,” said principal investigator Sean Solomon during a press conference last week. “Some of that fuel is required to get us into orbit (of Mercury in 2011). By not using fuel on some smaller maneuvers makes the mission more reliable and saves propellant, and allows us to have it in our back pocket when we need it for contingencies.” This is the first spacecraft to use this technique with such precision. Planetary flyby has been described as a complex ‘threading of a needle,’ and the MESSENGER team is getting better and better. The spacecraft’s first flyby was in January 2008, and a third will take place on Sept. 29, 2009. Orbit insertion will be on March 18, 2011.

We’ll post the MESSENGER images from this second flyby as soon as they’re available.

Source: MESSENGER website

Posted on by Nancy Atkinson

Astronaut Diary Survives Columbia Accident

Page from Ilan Ramon's diary. Credit: Israel Museum

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Pages from an astronaut’s diary survived the explosion of the space shuttle Columbia in 2003, and on Sunday, selected pages went on display at a museum in Jerusalem. Israeli astronaut Ilan Ramon kept a personal diary during his time in orbit, and portions of it were found about two months after Columbia broke apart on February 1, 2003 while returning to Earth following the STS-107 mission. “Today was the first day that I felt that I am truly living in space. I have become a man who lives and works in space,” Ramon wrote in an entry on his sixth day in orbit.

Astronaut Ilan Ramon departs for his flight aboard Columbia. Credit: Chris O’Meara/Associated Press
Astronaut Ilan Ramon departs for his flight aboard Columbia. Credit: Chris O’Meara/Associated Press

37 pages survived the extreme heat of the explosion, as well as the 60 km (37-mile) fall to earth and several days of wet weather before they were found. “It’s almost a miracle that it survived — it’s incredible,” Israel Museum curator Yigal Zalmona said. “There is no rational explanation for how it was recovered when most of the shuttle was not.”

Diary pages as they were found. Credit: Israel Ministry of Public Security
Diary pages as they were found. Credit: Israel Ministry of Public Security

The pages were found in a field just outside of Palestine, Texas. On some pages, the writing was washed out, other pages were tattered and torn, pocked with irregular holes as if debris had ripped through them. Pieces were twisted into tightly crumpled wads smaller than a fingernail. Some pages were stuck tightly together and had to be delicately pried apart.

Once it had been verified that the pages were relevant to the Columbia debris, the papers were collected and given to Colonel Ramon’s family. Ramon’s wife, Rona, decided to bring the papers to Israel for deciphering the damaged writing and, ultimately, conservation of the torn and tattered pages.

Most of the pages contain personal information which Mrs. Ramon did not wish to make public. “We agreed to do the restoration completely respecting the family’s privacy and the sensitivity about how intimate the document is,” museum director James Snyder said.

The diary took about a year to restore, Zalmona said, and it took police scientists about four more years to decipher the pages. About 80 percent of the text has been deciphered, and the rest remains unreadable, he said.

Page of Ramon's diary that was restored using Photoshop™ and Image-Pro Plus™
Page of Ramon's diary that was restored using Photoshop™ and Image-Pro Plus™

Two pages will be displayed at the museum. One contains notes written by Ramon, and the other is a copy of the Kiddush prayer, a blessing over wine that Jews recite on the Sabbath. Zalmona said Ramon copied the prayer into his diary so he could recite it on the space shuttle and have the blessing broadcast to Earth.

There is no information available as to where the pages of the diary were situated during reentry, for example if they were in a pocket of Ramon’s spacesuit or in a padded, heat resistant container or simply held under his leg, as one astronaut suggested.

The diary provides no indication Ramon knew anything about potential problems on the shuttle. Columbia’s wing was gashed by a chunk of fuel tank foam insulation at liftoff and broke up just 16 minutes before it was scheduled to land at the Kennedy Space Center in Florida. All seven astronauts on board were killed.

The diary is being displayed as part of a larger exhibit of famous documents from Israel’s history, held to mark the country’s 60th anniversary this year.

Sources: Israel Ministry of Public Security, AP article

Posted on by Astronomy Cast

Podcast: Running Out of Gravitons and Hitting the Brakes at Light Speed

Lightspeed!

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Another week, another roundup of your questions. This week listeners asked: if forces are communicated through particles, can we run out? If you were traveling at light speed, when would you know to stop? And there’s even more. If you’ve got a question for the Astronomy Cast team, please email it in to [email protected] and we’ll try to tackle it for a future show.

Click here to download the episode.

Or subscribe to: astronomycast.com/podcast.xml with your podcatching software.

Running Out of Gravitons and Hitting the Brakes at Light Speed – Transcript and show notes.

Posted on by Astronomy Cast

Podcast: The Life of the Sun

The surface of the Sun. Image credit: NASA

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We’ve talked about the Sun before, but this time we’re going to look at the entire life cycle of the Sun, and all the stages it’s going to go through: solar nebula, protostar, main sequence, red giant, white dwarf, and more. Want to know what the future holds for the Sun, get ready for the grim details.

Click here to download the episode.

Or subscribe to: astronomycast.com/podcast.xml with your podcatching software.

The Life of the Sun – Transcript and show notes.