Universe Today

May 1, 2013December 23, 2015 by Nancy Atkinson

Watch Live Hangout: TESS and the Search for Exoplanets

Artist's rendition of TESS in space. (Credit: MIT Kavli Institute for Astrophysics Research).

Last month, NASA announced plans to launch the Transiting Exoplanet Survey Satellite (TESS) in 2017. This is a satellite that will perform an all-sky survey to discover transiting exoplanets in orbit around the brightest stars in the Sun’s neighborhood. “TESS will carry out the first space-borne all-sky transit survey, covering 400 times as much sky as any previous mission,” said George Ricker, the mission’s principal investigator. “It will identify thousands of new planets in the solar neighborhood, with a special focus on planets comparable in size to the Earth.”

Read more about the TESS mission here.

Today, Wednesday May 1, at 19:00 UTC (12:00 p.m. PDT, 3:00 pm EDT) you can take part in a live Google+ Hangout, and have your questions answered about TESS and the search for exoplanets with three leading members of NASA’s TESS mission:

George Ricker is principal investigator of the TESS mission and a senior research scientist at the MIT Kavli Institute for Astrophysics and Space Research (MKI) in Cambridge, Mass.

Sara Seager is a professor of planetary science and physics at MKI and a member of the TESS team. Seager’s research focuses on computer models of exoplanet atmospheres, interiors and biosignatures.

Joshua Winn is an associate professor of physics at MKI and deputy science director for the TESS mission. Winn is interested in the properties of planets around other stars, how planets form and evolve, and whether there are habitable planets beyond Earth.

Watch in the viewer above, or at the Kavli Foundation website.

Questions can be submitted ahead of and during this special event via Twitter using the hashtag #KavliAstro and by email to [email protected].

May 1, 2013December 23, 2015 by Elizabeth Howell

Will Antimatter Obey Gravity’s Pull?

What matter and antimatter might look like annihilating one another. Credit: NASA/CXC/M. Weiss

What goes up must always come down, right? Well, the European Laboratory for Particle Physics (CERN) wants to test if that principle applies to antimatter.

Antimatter, most simply speaking, is a mirror image of matter. The concept behind it is that the particles that make up matter have an opposite counterpart, antiparticles. For example, if you consider that electrons are negatively charged, an antielectron would be positively charged.

This sounds like science fiction, but as NASA says, it is “real stuff.” In past experiments, CERN’s particle accelerator has created antiprotons, positrons and even antihydrogen. Properly harnessed, antimatter could be used for applications ranging from rocketry to medicine, NASA added. But we’ll need to figure out its nature first.

Continue reading “Will Antimatter Obey Gravity’s Pull?”

May 1, 2013December 23, 2015 by Bob King

The Curious Channel 37 — Must-see TV For Radio Astronomy

The Very Large Array, one of the world's premier astronomical radio observatories, consists of 27 radio antennas in a Y-shaped configuration 50 miles west of Socorro, New Mexico. Each antenna is 82 feet (25 m) in diameter. The data from the antennas is combined electronically to give the resolution of an antenna 22 miles (36 km) across. Image courtesy of NRAO/AUI and NRAO

Thanks to Channel 37, radio astronomers keep tabs on everything from the Sun to pulsars to the lonely spaces between the stars. This particular frequency, squarely in the middle of the UHF TV broadcast band, has been reserved for radio astronomy since 1963, when astronomers successfully lobbied the FCC to keep it TV-free.

Back then UHF TV stations were few and far between. Now there are hundreds, and I’m sure a few would love to soak up that last sliver of spectrum. Sorry Charley, the moratorium is still in effect to this day. Not only that, but it’s observed in most countries across the world.

Channel 37, a slice of the radio spectrum from 608 and 614 Megahertz (MHz) reserved for radio astronomy, sits in the middle of the UHF TV band. Click to see the full spectrum. Credit: US Dept. of Commerce

So what’s so important about Channel 37? Well, it’s smack in the middle of two other important bands already allocated to radio astronomy – 410 Megahertz (MHz) and 1.4 Gigahertz (Gz). Without it, radio astronomers would lose a key window in an otherwise continuous radio view of the sky. Imagine a 3-panel bay window with the middle pane painted black. Who wants THAT?

The visible colors, infrared, radio, X-rays and gamma rays are all forms of light and comprise the electromagnetic spectrum. Here you can compare their wavelengths with familiar objects and see how their frequencies (bottom numbers) increase with decreasing wavelength. Credit: ESA

Channel 37 occupies a band spanning from 608-614 MHz. A word about Hertz. Radio waves are a form of light just like the colors we see in the rainbow or the X-rays doctors use to probe our bones. Only difference is, our eyes aren’t sensitive to them. But we can build instruments like X-ray machines and radio telescopes to “see” them for us.

Diagram showing what how Earth's atmosphere allows visible light, a portion of infrared and radio light to reach the ground from outer space but filters shorter-wavelength, more dangerous forms of light like X-rays and gamma rays. To study the cosmos in these varieties of light, orbiting telescopes are required. — Diagram showing what how Earth’s atmosphere allows visible light, a portion of infrared and radio light to reach the ground from outer space but filters shorter-wavelength, more dangerous forms of light like X-rays and gamma rays. To study the cosmos in these varieties of light, orbiting telescopes are required.

Every color of light has a characteristic wavelength and frequency. Wavelength is the distance between successive crests in a light wave which you can visualize as a wave moving across a pond. Waves of visible light range from one-millionth to one-billionth of a meter, comparable to the size of a virus or DNA molecule.

X-rays crests are jammed together even more tightly – one X-ray is only as big as an small atom. Radio waves fill out the opposite end of the spectrum with wavelengths ranging from baseball-sized to more than 600 miles (1000 km) long.

The frequency of a light wave is measured by how many crests pass a given point over a given time. If only one crest passes that point every second, the light beam has a frequency of 1 cycle per second or 1 Hertz. Blue light has a wavelength of 462 billionths of a meter and frequency of 645 trillion Hertz (645 Terahertz).

If our eyes could see radio light, this is what the sky would look like. What appear to be stars are distant galaxies. The wispy arcs and shells are the remnants of exploding supernovae. — If our eyes could see radio light, this is what the sky would look like. What appear to be stars are actually distant galaxies glowing brightly with energy radiated as matter gets sucked down black holes in the cores. The wispy arcs and shells are the remnants of exploding supernovae. Since air molecules don’t scatter radio waves like they do visible light to create a blue sky, the sky would be dark even on a sunny day. Credit: National Science Foundation

The higher the frequency, the greater the energy the light carries. X-rays have frequencies starting around 30 quadrillion Hertz (30 petahertz or 30 PHz), enough juice to damage body cells if you get too much exposure. Even ultraviolet light has power to burn skin as many of us who’ve spent time outdoors in summer without sunscreen are aware.

Radio waves are the gentle giants of the electromagnetic spectrum. Their enormous wavelengths mean low frequencies. Channel 37 radio waves have more modest frequencies of around 600 million Hertz (MHz), while the longest radio waves deliver crests almost twice the width of Lake Superior at a rate of 3 to 300 Hertz.

Sun as it would look in the radio portion of the spectrum at a frequency of 1.4 gigahertz (GHz). Credit: NRAO — The sun as it would look in the radio portion of the spectrum at a frequency of 1.4 gigahertz (GHz). Image courtesy of the National Radio Astronomy Observatory (NRAO/AUI)

If Channel 37 were ever lost to TV, the gap would mean a loss of information about the distribution of cosmic rays in the Milky Way galaxy and rapidly rotating stars called pulsars created in the wake of supernovae. Closer to home, observations in the 608-614 MHz band allow astronomers track bursts of radio energy produced by particles blasted out by solar flares traveling through the sun’s outer atmosphere. Some of these can have powerful effects on Earth. No wonder astronomers want to keep this slice of the electromagnetic spectrum quiet. For more details on how useful this sliver is to radio astronomy, click HERE.

Just as optical astronomers seek the darkest sites for their telescopes to probe the most remote corners of the universe, so too does radio astronomy need slices of silence to listen to the faintest whispers of the cosmos.

May 1, 2013December 23, 2015 by Nancy Atkinson

The Sun Burps Out a Gigantic Rolling Wave

Imagery from SDO, SOHO and LASCO of the May 1, 2013 coronal mass ejection. Credit: NASA/ESA.

Just in time for May Day, the Sun blasted out a coronal mass ejection (CME) from just around the limb earlier today, May 1, 2013. In a gigantic rolling wave, this CME shot out about a billion tons of particles into space, traveling at over a million miles per hour. This CME is not headed toward Earth. The video, taken in extreme ultraviolet light by NASA’s Solar Dynamics Observatory (SDO), covers about two and a half hours of elapsed time.

Camilla, the rubber chicken mascot for the SDO, said via YouTube that getting this side view shows the power and force behind these solar flares and coronal mass ejections.

This image shows three views of the CME from three different instruments. Left is the SDO image, taken at 02:40 UT. Center is from the SOHO spacecraft, looking through their coronograph instrument. The “mushroom” cloud of plasma leaving the Sun is visible. On the right is the LASCO C2 (red) and C3 (blue) instruments on SOHO, which use a disk to block out the Sun. Visible are the solid occulter disk, used to create a false eclipse; the “pylon”, which is an arm that holds the occulter disk in place; a representation of the Sun in the form of a white disk drawn on the occulter during our image processing and then you can see background stars and the cloud of plasma leaving the Sun.

A coronal mass ejection from the Sun on May 1, 2013. Credit: NASA/SDO

May 1, 2013December 23, 2015 by Nancy Atkinson

How the Fermi Spacecraft Almost Got Taken Out by a Relic of the Cold War

Artist concept of the Fermi Space Telescope. Credit: NASA.

As a space telescope scientist or satellite operator, the last thing you want to hear is that your expensive and possibly one-of-a kind — maybe irreplaceable — spacecraft is in danger of colliding with a piece of space junk. On March 29, 2012, scientists from the Fermi Gamma-ray Space Telescope were notified that their spacecraft was at risk from a collision. And the object heading towards the Fermi spacecraft at a relative speed of 44,000 km/h (27,000 mph) wasn’t just a fleck of paint or tiny bolt.

Fermi was facing a possible direct hit by a 1,400 kg (3,100-pound) defunct Russian spy satellite dating back to the Cold War, named Cosmos 1805. If the two satellites met in orbit, the collision would release as much energy as two and a half tons of high explosives, destroying both spacecraft and creating more pieces of space junk in the process.

But this story has a happy ending, with the Fermi telescope still operating and continuing its mission to map the highest-energy light in the universe, all thanks to a little orbital traffic control.

You can watch the video here for the complete story, or read more at the Fermi website about how the Fermi Space Telescope dodged a speeding bullet.

May 1, 2013December 23, 2015 by Tammy Plotner

NGC 6240: Gigantic Hot Gas Cloud Sheaths Colliding Galaxies

Credit: X-ray (NASA/CXC/SAO/E.Nardini et al); Optical (NASA/STScI)

Looking almost like a cosmic hyacinth, this image is anything but a cool, Spring flower… it’s a portrait of an enormous gas cloud radiating at more than seven million degrees Kelvin and enveloping two merging spiral galaxies. This combined image glows in purple from the Chandra X-ray information and is embellished with optical sets from the Hubble Space Telescope. It flows across 300,000 light years of space and contains the mass of ten billion Suns. Where did it come from? Researchers theorize it was caused by a rush of star formation which may have lasted as long as 200 million years.

What we’re looking at is known in astronomical terms as a “halo” – a glorious crown which is located in a galactic system cataloged as NGC 6240. This is the site of an interacting set of of spiral galaxies which have a close resemblance to our own Milky Way – each with a supermassive black hole for a heart. It is surmised the black holes are headed towards each other and may one day combine to create an even more incredible black hole.

However, that’s not all this image reveals. Not only is this pair of galaxies combining, but the very act of their mating has caused the collective gases to be “violently stirred up”. The action has caused an eruption of starbirth which may have stretched across a period of at least 200 million years. This wasn’t a quiet event… During that time, the most massive of the stars fled the stellar nursery, evolving at a rapid pace and blowing out as supernovae events. According to the news release, the astronomers who studied this system argue that the rapid pace of the supernovae may have expelled copious quantities of significant elements such as oxygen, neon, magnesium and silicon into the gaseous envelope created by the galactic interaction. Their findings show this enriched gas may have expanded into and combined with the already present cooler gas.

Now, enter a long time frame. While there was an extensive era of star formation, there may have been more dramatic, shorter bursts of stellar creation. “For example, the most recent burst of star formation lasted for about five million years and occurred about 20 million years ago in Earth’s time frame.” say the paper’s authors. However, they are also quick to point out that the quick thrusts of star formation may not have been the sole producer of the hot gases.

Perhaps one day these two interactive spiral galaxies will finish their performance… ending up as rich, young elliptical galaxy. It’s an act which will take millions of years to complete. Will the gas hang around – or will it be lost in space? No matter what the final answer is, the image gives us a first-hand opportunity to observe an event which dominated the early Universe. It was a time “when galaxies were much closer together and merged more often.”

Original Story Source: Chandra X-Ray Observatory News Release.

April 30, 2013December 23, 2015 by Nancy Atkinson

An Awesome Look at Enceladus, the Jet-Powered Moon

Plumes from Enceladus' geysers are illuminated by reflected light from Saturn. Credit: NASA/JPL-Caltech, Space Science Institute.

According to planetary scientist and Cassini imaging team leader Carolyn Porco, about 98 geyser jets of all sizes near Enceladus’s south pole are spraying water vapor, icy particles, and organic compounds out into space. The spray from those geysers are evident in this new image from Cassini, showing a big, beautiful plume, illuminated by light reflected off of Saturn. Look closely to see that the plume is as large as the moon itself.

Cassini first discovered the jets of water ice particles in 2005, and since then scientists have been trying to learn more about how they behave, what they are made of and – most importantly – where they are coming from. The working theory is that Enceladus has a liquid subsurface ocean, and pressure from the rock and ice layers above combined with heat from within force the water up through surface cracks near the moon’s south pole. When this water reaches the surface it instantly freezes, sending plumes of ice particles hundreds of miles into space.

A patchwork network of frozen ridges and troughs cover the face of Enceladus. Credit: NASA/ESA, image processed by amateur astronomer Gordan Ugarkovi?. — A patchwork network of frozen ridges and troughs cover the face of Enceladus. Credit: NASA/ESA, image processed by amateur astronomer Gordan Ugarkovic.

Cassini has flown through the spray several times now, and instruments have detected that aside from water and organic material, there is salt in the icy particles. The salinity is the same as that of Earth’s oceans.

Enceladus is just 504 kilometers (313 miles) across, but it potentially could be one of the best spots in the solar system for finding life.

The top image was taken on January 18, 2013. This view looks toward the Saturn-facing side of Enceladus, and was taken when Cassini was approximately 483,000 miles (777,000 kilometers) from Enceladus. Image scale is 3 miles (5 kilometers) per pixel.

The second, face-on, color view of Enceladus was taken by the Cassini spacecraft on January 31 2011, from a distance of 81,000 km, and processed by amateur astronomer Gordan Ugarkovic.

Sources: CICLOPS, ESA

April 30, 2013December 23, 2015 by Elizabeth Howell

Space Robotics Dominate New $5 Bill in Canada

Canadarm2, Dextre and an unidentified astronaut will all feature on Canada's new $5 bill. Credit: Bank of Canada

In a world first, Canada’s Chris Hadfield unveiled a new money note — while in space.

Hadfield spun a fiver before the camera Tuesday as part of a ceremony to announce new $5 and $10 bills that will be distributed in Canada this year. The $5 bill will feature two pieces of Canadian technology that helped build the station: Canadarm2, which is a mobile robotic arm, and the hand-like Dextre.

The bill also shows an unidentified astronaut. That said, the choice to use Hadfield in the press conference was likely not a coincidence: Hadfield assisted with Canadarm2’s installation in 2001 when he became the first Canadian to walk in space.

“These bills will remind Canadians, every time they buy a sandwich and a coffee and a donut, what we are capable of achieving,” said Hadfield, who is in command of Expedition 35 on the International Space Station. His comments were carried on a webcast from the Bank of Canada.

The money note travelled with Hadfield in his Soyuz when he rocketed to the station in December, the Canadian Space Agency told Universe Today.

The polymer notes are intended to be more secure than the last generation of bills issued in Canada. Polymer $20, $50 and $100 bills are already available, but the smaller currencies won’t hit consumer pocketbooks until November.

Canadian astronaut Chris Hadfield holds a version of the $5 bill on the International Space Station. Credit: Bank of Canada (webcast)

“Featuring a sophisticated combination of transparency and holography, this is the most secure bank note series ever issued by the Bank of Canada. The polymer series is more economical, lasting at least two and half times longer than cotton-based paper bank notes, and will be recycled in Canada,” the Bank of Canada stated in a press release.

As with the past $5 bill, the opposite face of the new bill shows a drawing of past prime minister Wilfrid Laurier. Also shown at the ceremony: the $10 bill, with a Via Canada train on one side and John A. Macdonald, the first Canadian prime minister, on the other.

Both Jim Flaherty, Canada’s minister of finance, and Bank of Canada governor Mark Carney wore Expedition 35 pins at the press conference.

“I hope that’s not London calling,” Flaherty quipped to laughing reporters when NASA’s Mission Control phoned in with Hadfield on the line.

Hadfield is no stranger to space-themed currency. In 2006, the Royal Mint of Canada released two coins featuring him and Canadarm2. Hadfield and several other Canadian astronauts were also put on to Canadian stamps in 2003.

You can check out the full set of polymer bills on this Flickr series uploaded by the Bank of Canada.

April 30, 2013December 23, 2015 by Katrina Cain

Giveaway: Pocket Universe App for Your iOS Device

The name says it all – Pocket Universe answers every question you have and never knew you had about the great beyond – astronomically speaking. Pocket Universe also has a feature that speaks to the trivial in me – the need to fill my brain with interesting factoids that I can regale my friends with at parties.

Universe Today and Craic Design are giving away 10 free copies of Pocket Universe to our readers.

If you don’t want to wait for the win; you can purchase this app through the iTunes Store.

This giveaway will run for a week starting today, so get your entries in! How?

In order to be entered into the giveaway drawing, just put your email address into the box at the bottom of this post (where it says “Enter the Giveaway”) before Tuesday, May 7, 2013. We’ll send you a confirmation email, so you’ll need to click that to be entered into the drawing.

Here are some words from John Kennedy, developer of Pocket Universe:

Pocket Universe is one of those apps that re-affirms your belief in modern technology. Take it outside on a dark, cloudless night, hold it up at the sky, and you’ll get a real-time 3D rendered view of the heavens – complete with star and planet names, constellation images, as well as bright satellites, comets and more. If you ever wanted to know what it was you were looking at, this is the app for you. To help with new stargazers, there is also information on what you should be looking out for every month, and a list of interesting things visible on that very night. The app will also pop-up reminders when something interesting is happen – a meteor shower perhaps, or a flypast of the International Space Station – so you don’t miss out.

April 30, 2013December 23, 2015 by David Dickinson

Watch for the Eta Aquarid Meteor Shower this Weekend

The radiant of the Eta Aquarids rising. Looking to the south east from latitude 30 degrees north about 3 hours before local sunrise on May 5th. (Created by the author in Stellarium).

An often ignored meteor shower may offer fine prospects for viewing this weekend.

The Eta Aquarid meteors provide a dependable display in early May. With a radiant very near a Y-shaped asterism in northern Aquarius, the Eta Aquarids are one of the very few major showers that provide a decent annual show for southern hemisphere residents.

This year, the peak of the Eta Aquarids as per the International Meteor Organization (IMO) comes on May 6^th at 1:00 UT, or 9:00 PM EDT on May 5th. This favors European longitudes eastward on the morning of Monday, May 6^th. The Eta Aquarid radiant rises just a few hours before dawn, providing optimal viewing in the same time frame.

Keep in mind, the shower is active from April 19^th to May 28^th. Predicting the arrival of the peak of a meteor shower can be an inexact science. North American observers may still see an early arrival of the Eta Aquarids on May 5^th or even the morning of the 4^th.

Could “the 4^th be with us” at least in terms of meteor shower activity?

The Eta Aquarids are one of two annual meteor showers associated with that most famous of comets: 1P/Halley. The other shower associated with Halley’s Comet is the October Orionids. This makes it one of the very few periodic comets associated with two established annual meteor showers.

Like the Orionids, the Eta Aquarid meteors have one of the highest atmospheric velocities of any shower, at 66 kilometres per second. Expect short, swift meteors radiating from low in the southeast (or northeast if you’re based south of the equator) a few hours before local dawn.

This year’s ZHR is expected to reach 55. This year also offers outstanding prospects, because the Moon is only a 17% illuminated waning crescent just 4 days from New at the shower’s peak. There’s some thought in the meteor observing community that this shower experiences a cyclical peak every 12 years.

If this is indeed the case, we could be headed towards a mild lull in this shower around the 2014 to 2016 time frame. Performances from the Eta Aquarids over the past few years as per data from the IMO seem to bear this out, with a peak around 2009;

2012=ZHR 69

2011=ZHR 63

2010=No data

2009=ZHR 90

2008=65

Still, 55 per hour is a respectable shower. Keep in mind, the ZHR stands for the “Zenithal Hourly Rate” and is an ideal number. This is the number of meteors an observer could expect to see under dark skies with no light pollution with the radiant directly overhead. Also, remember that no single observer can monitor the entire sky at once!

This is also one of the last big annual showers of the season until the Perseids in mid-August. The Gamma Delphinids (June 11^th) and the June Bootids (Jun 27^th and the June Lyrids (June 15^th) are the only minor showers in June. July also sees another minor shower radiating from the constellation Aquarius, the Delta Aquarids which peak on July 30^th. The daytime Arietids in June would put on a fine annual showing if they didn’t occur in… you guessed it… the daytime.

This weekend’s Eta Aquarids will put on a better display for the southern hemisphere, one of the very few showers for which this is true.

It’s a poorly understood mystery. Why does the northern celestial hemisphere seem to contain a majority of major meteor shower radiants? The Geminids, the Leonids, the Perseids, the Quadrantids… all of these showers approach the Earth from above the celestial equator, and even from above the ecliptic plane. The Eta Aquarids are one of the very few major showers that goes against this trend.

Is it all just a coincidence? Perhaps. Like total solar eclipses, meteor showers are as much a product of our position in time as well as space. New streams are shed as comets visit the inner solar system, some for the very first time. These older trails interact with and are dispersed by subsequent passages near planets. The 12 year fluctuation of the Eta Aquarids is thought to be related to the orbit of Jupiter which has a similar period.

For example, one meteor shower known as the Andromedids was prone to epic storm outbursts until the early 20^th century. Now the stream is a mere trickle. Meteor showers evolve over time, and perhaps their seeming affinity for the northern hemisphere of our planet is a mere perception of our epoch. Maybe a future study could discern a bias due to the number of prograde versus retrograde cometary orbits, or perhaps statistical scrutiny could reveal that no such partiality actually exists.

All food for thought as you keep vigil these early May mornings for the meteoric “Drops from the Water Jar…” Be sure to post those meteor pics to the Universe Today’s Flickr forum, report those meteor counts to the International Meteor Organization, and tweet those fireball sightings to #Meteorwatch!