Posted on by Tega Jessa

Where is Helium Found

Universe
Universe

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Helium is the second lightest element in the known universe. It is also the second most abundant. According to some estimates helium accounts for as much as 24 percent of the Universe’s mass. This element is also plentiful since it is a prime product of fusion nuclear reactions involving hydrogen. So if it is so plentiful where is Helium found?

The problem is that just because an element is common in the universe at large does not mean that it is common on Earth. Helium is an element that fits this scenario. Helium only accounts for 0.00052% of the Earth’s atmosphere and the majority of the helium harvested comes from beneath the ground being extracted from minerals or tapped gas deposits. This makes it one of the rarest elements of any form on the planet.

Like mentioned before Helium is rare on Earth but there are places where it is readily found. If you look at space the majority of helium is in stars and the interstellar medium. This is due to the fusion reaction that powers most stars fusing single hydrogen atoms to create helium atoms. This process balanced with a star’s gravity is what helps it to stay stable for billions of years. On Earth the majority of helium found comes from radioactive decay. This is the opposite nuclear reaction called fission that splits atoms. For this reason radioactive minerals in the lithosphere like uranium are prime sources for helium.

On Earth there are key locations where concentrated helium can be harvested. The United States produces the majority of the world’s helium supply at 78%. The rest of the world’s helium is harvested in North Africa, The Middle East, and Russia. The interesting thing is that thanks to these deposits the world’s demand for helium is being met regularly. Also unlike petroleum which can decades to form from organic material, 3000 metric tons of Hydrogen is produced yearly. Until helium demand reaches at least the same level of demand as petroleum there it little chance of that demand outpacing supply.

Helium is looking to be a major player in the near future. Governments are looking into using the gas as source of hydrogen for fuel cells and other transportation technologies. At the moment the promise is still tentative but at least with better surveying and knowledge of gas deposits there will be a supply waiting if becomes the next major element to power human civilization. In the meanwhile ours is still a planet beholden to carbon.

We have written many articles about Helium for Universe Today. Here’s an article about the discovery of Helium, and here’s an article about composition of the Sun.

If you’d like more info about helium on Earth, check out NASA’s Solar System Exploration Guide on Earth. And here’s a link to NASA’s Earth Observatory.

We’ve also recorded an episode of Astronomy Cast all about planet Earth. Listen here, Episode 51: Earth.

Source: Wikipedia

Posted on by Tega Jessa

Where Does Geothermal Energy Come From

Earth's core.
Earth's core.

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You may not have heard much about geothermal energy but it is one of the hottest alternative energy commodities around. It is a renewable and clean energy source that will be around for a long time. However where does geothermal energy come from? The answer is the earth itself. The world geothermal comes from the Greek words geo which means earth and therme which means heat. Basically geothermal energy is heat energy harvested from the Earth itself.

Geothermal heat is produced by the core of the Earth itself. You may not think that energy to be much when compared to the sun but you would be wrong in some aspects. The Earth’s core alone is 11,000 degrees. That is hotter than the surface of the sun. The Earth’s geothermal energy is created by the decay of radioactie materials in the core and in the surrounding layers of rock.

However this still doesnt tell us how this energy becomes accessible. The deepest mankind can even go with the best technology is around 11 km. The answer is plate tectonics. bounadaries and faults are cracks in the Earth’s crust where magma rises near or to the surface. Geothermal plants take advantage of this fact using water heated by this volcanic activity to produce electric power.

The main place where geothermal energy can be used have not only volcanic activity but also enough ground water to be used to power the turbines that generate power. Prime areas are near volcanoes, hot springs, and geysers. Large volcanic islands like Greenland have vast resources in terms of geothermal energy. In the end the most common location for geothermal reservoirs will be where ever there are major plate boundaries with a lot of seismic and volcanic activity.

The benefits of geothermal energy is already being discussed in nations like Iceland as way to reduce reliance on foreign oil. Geothermal is abundant where it can be accessed and can easily produce energy on par with the output of other types of energy production such as nuclear reactors. The best part is that it is clean energy. There is no way it can produce pollution that can harm the environment. The only risk is that drilling in active volcanic area can make them vulnerable to earthquakes.

In the end Geothermal still one of the best possible sources of clean energy on the planet. As the technology improves for accessing it more homes around the world will have the opportunity to be powered by this renewable energy resource.

We have written many articles about geothermal energy for Universe Today. Here’s an article about Geothermal Energy, and here’s an article about how geothermal energy works.

If you’d like more info on Earth, check out NASA’s Solar System Exploration Guide on Earth. And here’s a link to NASA’s Earth Observatory.

We’ve also recorded an episode of Astronomy Cast all about planet Earth. Listen here, Episode 51: Earth.

Sources:
http://www.eia.gov/kids/energy.cfm?page=geothermal_home-basics
http://en.wikipedia.org/wiki/Geothermal_energy
http://www.clean-energy-ideas.com/articles/what_is_geothermal_energy.html

Posted on by Jerry Coffey

Where do Hurricanes Occur?

View of Hurricane Ike From Space Station
View of Hurricane Ike From Space Station

What is a hurricane? Well, a hurricane is a tropical cyclone that occurs in the North Atlantic Ocean or the Northeast Pacific Ocean and remains east of the International Dateline. Tropical cyclones are characterized by a large low pressure center and numerous thunderstorms. These produce strong winds and heavy rain. These cyclones feed on heat released when moist air rises causing condensation of the water vapor that is contained in the moist air. These storms are fueled by a different heat mechanism than other cyclonic windstorms(nor’easters, polar lows, and European windstorms). They are classified as a warm core storm system.

All tropical cyclones are areas of low atmospheric pressure. As a matter of fact, the pressures recorded at the center of tropical cyclones are among the lowest that occur at sea level. A hurricane is characterized and driven by the release of large amounts of latent heat of condensation(water vapor condenses as it moves upward). This heat is distributed vertically around the center of the storm, so, except at the surface of water, it is warmer inside the cyclone than it is outside. At the center of the hurricane is an area of sinking air. If this area is strong enough, it can develop into a large eye. Weather in the eye is normally calm and free of clouds, but the surface of the sea may be tossing violently. The eye is normally circular in shape, and may range in size from 3 km to 370 km in diameter.

While a tropical cyclone’s primary energy source is the release of the heat of condensation, solar heating is the initial source of that evaporation. An initial warm core system(an organized thunderstorm complex) is necessary for the formation of a tropical cyclone, but a large flux of energy is needed to lower atmospheric pressure. The influx of warmth and moisture from the underlying ocean surface is critical for tropical cyclone strengthening and most of it comes from the lower 1 km of the atmosphere. Condensation leads to higher wind speeds. These faster winds and the lower pressure associated with them cause an increase in surface evaporation and more condensation. This positive feedback system continues and feeds the hurricane until the conditions for hurricane formation are gone. The rotation of Earth causes the system to spin,(the Coriolis effect) which gives it a cyclonic appearance and affects its trajectory.
Tropical cyclones are distinguished by the deep convection that fuels them. Since convection is strongest in the tropics it defines the initial domain of the tropical cyclone. To continue to feed itself a tropical cyclone must remain over warm water. When a tropical cyclone passes over land, it is cut off from its heat source and its strength diminishes rapidly. The passage of a tropical cyclone over the ocean can cause the upper layers of the ocean to cool substantially, which can influence subsequent cyclone development. Scientists at the National Center for Atmospheric Research in the US estimate that a tropical cyclone releases heat energy equal to 70 times the world energy consumption, 200 times the worldwide electrical generating capacity, or the same as exploding a 10 megaton nuclear bomb every 20 minutes.
Well, there you have the answer to what is a hurricane. It is a tropical nightmare, but if humans could somehow harness that energy we would never need fossil fuels again.

We have written many articles about hurricanes for Universe Today. Here’s an article about human influences generating more hurricanes, and here’s a NASA video of Hurricane Bill.

If you’d like more info on hurricanes, check out Visible Earth Homepage. And here’s a link to NASA’s Earth Observatory.

We’ve also recorded an episode of Astronomy Cast all about planet Earth. Listen here, Episode 51: Earth.

Posted on by Jerry Coffey

How Do Tornadoes Form?

Tornado in Kansas
Tornado in Kansas

How do tornadoes form? That is pretty easy to answer since there has been a large amount of study into the subject. They are usually the extreme result of a supercell thunderstorm. During the storm cold air and warm air combine in a set pattern: the cold air drops as the warm air rises. The warm air eventually twists into a spiral and forms the funnel cloud that we all associate with a tornado.

The formation of a tornado follows a clear set of steps. First there a change in wind direction and an increase in wind speed. This change occurs at an increasing altitude and creates an invisible horizontal spinning effect in the lower atmosphere. Next, rising air within the thunderstorm’s updraft tilts the rotating air from horizontal to vertical. Third, an area of rotation, 3-10 km wide is contained within a vast majority of the storm. This is where the strongest tornadoes form. Then a lower cloud base in the center of the storm becomes a rotating wall cloud. This area can be nearly rain-free. Lastly, a tornado develops and starts to wreak its destruction.

Once a tornado has formed, it follows a predictable life cycle. First, the mesocyclone(rotating air), along with the rear flank downdraft( RFD), starts moving towards the ground. A small funnel appears to build up at the bottom of a wall cloud. As the RFD reaches the ground, the surrounding dirt rises up, causing damage even to heavy objects. The funnel touches the ground immediately after the RFD, forming a tornado.

During the next stage the tornado’s main source of energy, the RFD, begins to cool. The distance the tornado covers, depends on the rate at which the RFD cools. If the RFD cannot further provide any more warm air to the tornado, it begins to die.

Lastly, with the tornado’s warm air supply cut, the vortex begins to weaken and shrivel away. As the tornado weakens, the mesocyclone also starts to dissipate, but a new mesocyclone can start very close to the dying one. Those are the basics of tornado formation and life.

We have written many articles about tornado for Universe Today. Here’s an article about the biggest tornado, and here’s an article about the Tornado Alley.

If you’d like more info on tornado, check out the National Oceanic and Atmospheric Administration Homepage. And here’s a link to NASA’s Earth Observatory.

We’ve also recorded an episode of Astronomy Cast all about planet Earth. Listen here, Episode 51: Earth.

Posted on by Nancy Atkinson

Where In The Universe Challenge #122

Ready for another Where In The Universe Challenge? Here’s #122! Take a look and see if you can name where in the Universe this image is from. Give yourself extra points if you can name the spacecraft, telescope or instrument responsible for the image. We provide the image today, but won’t reveal the answer until tomorrow. This gives you a chance to mull over the image and provide your answer/guess in the comment section. And Please, no links or extensive explanations of what you think this is — give everyone the chance to guess. (Some folks have been messing that up lately — let’s get it right, people!!)

UPDATE: Answer now posted below.

As some of you guessed (knew!) this is phytoplankton bloom off the coast of Argentina in early February 2010, which colors the Atlantic Ocean’s waters blue-green. The Moderate Resolution Imaging Spectroradiometer (MODIS) on NASA’s Terra satellite is the instrument and spacecraft responsible for this image. See the full image and more information at the NASA Earth Observatory website.

Posted on by Jerry Coffey

How Big Is Neptune

Are There Oceans on Neptune
Neptune is more than just the 8th planet in our solar system; it is a celestial reminder of the power that mathematics grants us.

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There are many ways to determine ‘how big is Neptune’. It has an equatorial radius 24,764 km, a polar radius of 24,341 km, and a surface area of 7.6408×10,sup>9km2. It has a volume of 6.254×1013km3, a mass of 1.0243×1026kg, and a mean density of 1.638 g/cm3. Now that you know most of the planet’s critical digits, here is a little information about its make up.

Neptune is the eighth and farthest planet from the Sun. It is the fourth-largest planet by diameter and the third-largest by mass. Neptune’s mass is 17 times that of the Earth. On average, Neptune orbits the Sun at a distance of 30.1 astronomical units. It was discovered on September 23, 1846. Neptune was the first planet found by mathematical prediction rather than direct observation. Alexis Bouvard deduced its existence from gravitational perturbations in the orbit of Uranus. The planet was later observed by Johann Galle. Its largest moon, Triton, was observed a short time later.

Neptune’s atmosphere is composed primarily of hydrogen and helium along with traces of hydrocarbons and nitrogen. It also contains a high proportion of ices like: water, ammonia, and methane. Astronomers occasionally categorize Neptune as an ice giant. The interior of Neptune, like that of Uranus, is primarily composed of ices and rock. Traces of methane in the outermost regions in part account for the planet’s blue appearance. Neptune’s atmosphere is notable for its active and visible weather patterns. When Voyager 2 flew by the planet’s southern hemisphere possessed a Great Dark Spot. These weather patterns are driven by the strongest sustained winds of any planet in the Solar System, with recorded wind speeds as high as 2,100 km/h.Because of its great distance from the Sun, Neptune’s outer atmosphere is one of the coldest places in the Solar System, with temperatures at its cloud tops approaching ?218°C. Temperatures at the planet’s center are approximately 5,000°C.

Neptune has a planetary ring system. The rings may consist of ice particles coated with silicates or carbon-based material, which gives them a reddish hue. The three main rings are the narrow Adams Ring, 63,000 km from the center of Neptune, the Le Verrier Ring, at 53,000 km, and the broader, fainter Galle Ring, at 42,000 km. A faint outward extension to the Le Verrier Ring has been named Lassell; it is bounded at its outer edge by the Arago Ring at 57,000 km. Not only is the planet large, but it has many interesting features as well.

We have written many articles about Neptune for Universe Today. Here’s an article about the color of Neptune, and here are some pictures of Neptune.

If you’d like more information on Neptune, take a look at Hubblesite’s News Releases about Neptune, and here’s a link to NASA’s Solar System Exploration Guide to Neptune.

We’ve also recorded an entire episode of Astronomy Cast all about Neptune. Listen here, Episode 63: Neptune.

Source: NASA

Posted on by Nancy Atkinson

How NASA Helped Rescue the Chilean Miners

Oct. 13, 2010: Trapped miner Victor Segovia reaches the surface to become the 15th to be rescued from the San Jose mine in Copiapo. Source: Reuters

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The world has been transfixed by the rescue of 33 miners trapped nearly a kilometer (about a half a mile) underground in the San Jose mine near Copiapo, Chile. Seeing the men emerge from their 69-day-long ordeal has been emotional for everyone involved, as well as for those of us just watching from afar. But were it not for NASA, the rescue might not be going as smoothly and trouble-free as, thankfully, it has. NASA’s expertise in long duration space missions – which are similar in many respects to what the miners endured – as well as the space agency’s knowledge in specialized engineering and training for emergencies has been invaluable during the rescue operations. NASA provided suggestions regarding the rescue cages that were specially-designed to pull the trapped miners out of the narrow shaft that was drilled to rescue them, and also is providing on-site expert advice on medical, nutritional and behavioral health issues.

“What we brought to the table for the Chileans was our experience in behavior health support, not only in terms of the confinement and entrapment for that period of time but also what the miners and the families could experience once the miner had been rescued,” said Dr. Michael Duncan, who led the team of NASA experts who traveled to Chile, in answer to a question posed by Universe Today during a web chat. “In working with our astronauts and their families we prepare them beforehand and we support them during the mission and we support them after the astronaut returns. And I think our expertise in those areas was very helpful for the Chilean doctors and psychologists.”

Among NASA’s suggestions were an increased supplement of Vitamin D to normalize sleep patterns and developing an organized daily routine that includes exercise.

NASA also helped with diet suggestions which would help their well being during their entrapment, as well as making sure the miners would be well enough and trim enough to ride in the rescue capsule.

Indeed, the miners have emerged looking healthy and several have bounded out from the capsule, running to hug family and friends or greet the cheering crowd.

When the Chilean engineers decided a capsule was the best way to rescue 33 trapped miners, the NASA Engineering and Safety Center (NESC) provided about 75 recommendations, said Clinton Cragg, principal engineer at NESC, in an interview on WAVY.com. Most of those design elements found their way into the 4-meter (13 foot) 420 kg (926-pound) capsule dubbed “Phoenix.”

With the cramped, one-at-a-time ride taking 20 minutes or more, the miners are monitored by video on the way up for any sign of distress or panic. They have oxygen masks, dark glasses to protect their eyes from unfamiliar daylight and sweaters for the huge temperature differences from the heat of underground to the chilling cold in the high altitude Atacama Desert in Chile.

Satellite image of the San Jose Mine area where the miners were trapped. NASA Earth Observatory image created by Jesse Allen and Robert Simmon, using Earth Observer-1 satellite.

“The Chileans had a very limited set of requirements that they had given their own engineers with regards to how to design this cage, and that was primarily length, diameter, and weight,” said Duncan. “Looking at the video of the cage, some of these things they’ve certainly incorporated into their design.”

In an image from video, rescuer Manuel Gonzalez Pavez reaches the 33 miners in the collapsed mine. Source: AP

Now that the miners are safe, Duncan said each will be observed for any medical conditions that they may have developed. “Of course, we’re looking for things like skin infections or infections of the sinuses or the lungs,” he said during the web chat. “Something that they may have acquired due to exposure to the warm, humid and dusty conditions in the mine.”

In regards to the psychological health of the miners, Duncan said doctors and psychologists have been working with the miners and their families in an effort to educate them on these types of issues and the sudden celebrity that the miners now find themselves in, and they hope to try to prevent any future psychological issues from occurring.

The NASA team assisting the Chilean rescue included two medical doctors, Duncan and J.D Polk; psychologist Al Holland and Cragg.

“I am proud of the people of this agency who were able to bring the experience of spaceflight down to Earth when it was needed most,” said NASA Administrator Charlie Bolden in a statement. “As the drama of this rescue continues to unfold before us, we pray for the safe return of each and every miner.”

For a wonderful slideshow of images from the rescue, see this link to Reuters.

Sources: NASA, Washington Post Web chat, WAVY-TV NASA Earth Observatory,

Posted on by Mark Thompson

Galaxy Growth Not Always Result of Violent Collisions

Artist’s impression of a young galaxy accreting material. Credit: ESO/L. Calçada

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Until recently, it was thought the galactic equivalent of a motorway pile-up was the only way galaxies got bigger. But startling new evidence from a European team of astronomers suggests that violent galactic collisions are not the only way that galaxies evolve and grow, and instead there seems to be something else happening that has affected the majority of galaxies — a kinder, gentler action which is not quite so disruptive.

For some years, astronomers have struggled to understand why the mass of galaxies seems to have increased dramatically just a few billion years after the Big Bang. We know from observation that galaxies collide but this is an incredibly violent activity and one that is not particularly common.

A new study using the Very Large Telescope (VLT) at the European Southern Observatory (ESO), by a team led by Giovanni Cresci, looked for evidence that galaxies might be accreting material from the hydrogen and helium gas that filled the early Universe and permeates the space between the galaxies. We know that they are surrounded by halos of unseen material but Cresci’s team wanted to see if there was any evidence of material being sucked into the galaxy from the surrounding environment.

Their study focused on a group of distant galaxies which would represent those in the early Universe, about 2 billion years after the big bang, to see if they could detect any evidence of this gas accretion.

Using the SINFONI (Spectrograph for Integral Field Observation in the Near Infrared) attached to the VLT, Cresci and his team mapped the distribution of elements within the target galaxies. Their findings showed that instead of heavier elements being concentrated around the core as we find in today’s galaxies, the core was surprisingly abundant of the lighter elements hydrogen and helium. This can only be as a result of accretion of lighter elements from the surrounding area boosting the rate of star formation in the core. The accretion process itself relies on cool gas being transferred directly into the core of the galaxy.

“The primordial gas in the halo of galaxies, especially at great distances, is mostly shock heated and therefore very hot,” Cresci told Universe Today. “To be accreted it has to be cooled and this is not an efficient process. Recent theoretical models have shown that narrow streams of cold gas can form, and that they are able to penetrate the hot gas and to provide fresh gas to the centre of the galaxy. Unlike more destructive and violent mergers between galaxies, the streams are likely to keep the rotating disk configuration intact, although turbulent.”

This new discovery means astronomers have perhaps found an answer to a long standing question but with the major consequence of needing to rewrite our current theories of the evolution of the Universe.

Source: ESO, email exchange with Cresci

Mark Thompson is a writer and the astronomy presenter on the BBC One Show. See his website, The People’s Astronomer, and you can follow him on Twitter, @PeoplesAstro

Posted on by Nicholos Wethington

Hubble Sees Asteroid Collision in Slow-Motion

The collision between two asteroids in early 2009 produced a strange, X-shaped aftermath. Image Credit: NASA, ESA and D. Jewitt (UCLA)

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Alas, the image above is not marking alien pirate treasure in space – for the first time, the aftermath of a collision between two asteroids has been imaged. Last January, an international team of astronomers saw the strange X-shaped object with the Hubble Space Telescope after ground-based observatories spotted evidence of an asteroid collision in the asteroid belt. The team has now used Hubble to do follow-up observations and uncovered a few surprises about the collision.

The collision produced an X shape, followed by a long comet-like tail. The astronomers, led by David Jewitt of the University of California in Los Angeles, were surprised to find that the collision did not happen as recently as they’d thought, but had actually occurred almost a year previous to the detection. It’s likely that the two asteroids smashed together sometime in February or March of 2009.

“When I saw the Hubbble image I knew it was something special,” said ESA astronomer Jessica Agarwal in a press release.

Named P/2010 A2, the object is located in the asteroid belt between Mars and Jupiter. Asteroid collisions are thought to be a commonplace occurrence, and are responsible for kicking up dust in our Solar System and other planetary systems. Just how much dust is produced, and how frequent the collisions happen is still a hazy topic, and the recent observation of P/2010 A2 should help astronomers to better model this phenomenon.

By figuring out how much dust is produced by the process of ‘collisional grinding’, astronomers could better model the dusty debris disks of other planetary systems, as well as our own.

The team monitored the slow-motion expansion of the leftovers of the colliding asteroids with the Hubble Space Telescope between January and May of 2010. They’ve determined that P/2010 A2 is about 120 meters (393 feet) wide, and the particles of dust that make up the tail following it are between 1 millimeter (0.04 inches) to 2.5 centimeters (1 inch) in diameter.

The collision producing the object P/2010 A2, as observed over the course of a few months by Hubble. Image Credit: NASA, ESA and D. Jewitt (UCLA)

The remnants of the collision suggest that a smaller asteroid – 3 to 5 meters (10-16 feet) wide – collided into a larger one at about 18,000 km per hour (11,000 miles per hour). This vaporized the smaller asteroid, and ejected material from the larger one.

Why is the object X-shaped? That mystery has yet to be determined. It is likely, according to the team, that the filaments produced by the collision suggest asymmetries in the colliding objects. Further observations of P/2010 A2 with the Hubble in 2011 will show just how the collision continues to change, allowing for a more precise model of how it started out.

The observed tail is caused by the same mechanism that produces cometary tails – radiation pressure from the Sun pushes the dust away from the nucleus of the object.

As to why we don’t have thousands of Hubble images to produce a whole alphabet of asteroid collisions shapes – “Catching colliding asteroids on camera is difficult because large impacts are rare, while small ones, such as the one that produced P/2010 A2, are exceedingly faint,” Jewitt said. The results of their observations will be published in the October 14th issue of the journal Nature.

Source: ESA Press Release

Posted on by Nancy Atkinson

New Galaxy Zoo Project Crowd-sources Old Climate Data

The newest citizen science project from the Galaxy Zoo team lets the public travel back in time and join the crews of over 280 different World War I royal navy warships. While an engaging historical journey, the project will help scientists better understand the climate of the past. There are gaps in weather and climate data records, particularly before 1920, prior to when weather station observations were accurately recorded. But old naval ships routinely recorded the weather they encountered – marking down temperatures and conditions even while in battle. The information in many of these weather logbooks has not been utilized – until now, as the “Old Weather” project has made its debut as the newest way for the public to contribute in scientific research.

The project is designed to provide a detailed map of the world’s climate around 100 years ago, which will help tell us more about the climate today. Anyone can take part, read the logs, follow events aboard the vessels and contribute to this fun and historical project, which could tell us more about our climate’s future.

“These naval logbooks contain an amazing treasure trove of information but because the entries are handwritten they are incredibly difficult for a computer to read,’ said Dr. Chris Lintott of Oxford University, a Galaxy Zoo founder and developer of the OldWeather.org project. “By getting an army of online human volunteers to retrace these voyages and transcribe the information recorded by British sailors we can relive both the climate of the past and key moments in naval history.”

By transcribing information about weather, and any interesting events, from images of each ship’s logbook web volunteers will help scientists to build a more accurate picture of how our climate has changed over the last century, as well as adding to our knowledge of this important period of British history.

HMS Acacia, one of the ships in the Old Weather project.

“Historical weather data is vital because it allows us to test our models of the Earth’s climate,”said Dr. Peter Stott, Head of Climate Monitoring and Attribution at the British meteorology, or Met Office. “If we can correctly account for what the weather was doing in the past, then we can have more confidence in our predictions of the future. Unfortunately, the historical record is full of gaps, particularly from before 1920 and at sea, so this project is invaluable.”

Weather observations by Royal Navy sailors were made every four hours without fail, said Dr. Robert Simpson of Oxford University, who added that this project is almost like “launching a weather satellite into the skies at a time when manpowered flight was still in its infancy.”

What is Old Weather from National Maritime Museum on Vimeo.

If you are not yet familiar yet with the Zooniverse, which includes citizen science projects like Galaxy Zoo and Moon Zoo, you are really missing out on a fun and engaging way to do actual, meaningful science. In those projects, 320,000 people have made over 150 million classifications and published several scientific papers – which shown that ordinary web users can make observations that are as accurate as those made by experts.

Old Weather is unique among the eight scientific projects encompassed by the Zooniverse because of how old the data is, and participating really is a trip back in time. The ‘virtual sailors’ visiting OldWeather.org are rewarded for their efforts by a rise through the ratings from cadet to captain of a particular ship according to the number of pages they transcribe. Historians are also hoping that a look into these old records will provide a fresh insight into naval history and encourage people to find out more about the past.

Here’s a tutorial on how to participate in Old Weather:

Old Weather – Getting Started from The Zooniverse on Vimeo.

To find out more, and participate visit OldWeather.org. There’s also an Old Weather blog at http://blogs.zooniverse.org/oldweather

You can also follow the project on Twitter (@OldWeather) and Facebook.