Climate Change Satellite gets Green Light for Launch

The European Space Agency’s Soil Moisture and Ocean Salinity (SMOS) satellite has been cleared for takeoff, following nearly a year in limbo while the mission team awaited the go-ahead from a private launch company.

Originally expected to launch in 2008, SMOS has been in storage at Thales Alenia Space’s facilities in Cannes, France since last May, awaiting a  launch appointment at the Russian Plesetsk Cosmodrome, north of Moscow. If all goes according to plan, the craft will now launch between July and October, the second ESA mission in a series of six designed to observe Earth from space and bolster an understanding of climate change. The first of the satellites in its new Living Planet Program, The Gravity field and steady-state Ocean Circulation Explorer (GOCE), is scheduled to go up March 16. 

 

Over its lifetime of about 20 months, GOCE will map global variations in the gravity field – crucial for deriving accurate measurements of ocean circulation and sea-level change, both of which are affected by climate change.

SMOS, circulating at a low orbit of around 750 km (466 miles) above the Earth,  will be the first mission dedicated to mapping soil moisture and ocean salinity. Salinity in the oceans has a significant impact on ocean circulation, which in turn helps drive the global climate. Among other applications, understanding the salinity and temperature of the seas will lead to easier predictions of the zones where hurricanes intensify. A specialized radiometer has been developed for the mission that is capable of observing both soil moisture and ocean salinity by capturing images of emitted microwave radiation around the frequency of 1.4 GHz (L-band). SMOS will carry the first-ever, polar-orbiting, space-borne, 2-D interferometric radiometer. The mission is designed to last three years.

Here’s a rundown of the final four planned crafts in the series:

  • ADM-Aeolus (Atmospheric Dynamics Mission), with a 2010 launch date, will collect data about the global wind profile to improve weather forecasting.
  • CryoSat-2, set to launch in late 2009, will determine variations in the thickness of the Earth’s continental ice sheets and marine ice cover to further our understanding of the relationship between ice and global warming. CryoSat-2 replaces CryoSat, which was lost at launch in 2005.
  • Swarm, due for launch in 2010, is a constellation of three satellites to study the dynamics of the magnetic field to gain new insights into the Earth system by studying Earth’s interior and its environment.  
  • EarthCARE (Earth Clouds Aerosols and Radiation Explorer), lanching in 2013, is a joint European-Japanese mission that aims to improve the representation and understanding of the Earth’s radiative balance in climate and numerical weather forecast models.
Source: ESA

Last Summer’s Fireball in Pieces on the Ground?

 
The Bejar bolide photographed from Torrelodones, Madrid, Spain. The incoming fireball is the streak to the right of the floodlit house. The bright light at the top is the overexposed Moon. Credit: J. Perez Vallejo/SPMN.

Astronomers have analyzed the cometary fireball that blazed across the sky over Europe last year and concluded it was a dense object, about a meter (3.2 feet) across and with a mass of nearly two tons — large enough that some fragments probably survived intact and fell to the ground as meteorites.

Last July, people in Spain, Portugal and France watched the brilliant fireball produced by a boulder crashing down through the Earth’s atmosphere. In a paper to be published in the journal Monthly Notices of the Royal Astronomical Society, astronomer Josep M. Trigo-Rodríguez, of the Institute of Space Sciences in Spain, and his co-authors present dramatic images of the event. The scientists also explain how the boulder may originate from a comet which broke up nearly 90 years ago, and suggest that chunks of the boulder (and hence pieces of the comet) are waiting to be found on the ground.

“If we are right, then by monitoring future encounters with other clouds of cometary debris, we have the chance to recover meteorites from specific comets and analyse them in a lab,” Dr Trigo-Rodríguez said. “Handling pieces of comet would fulfil the long-held ambitions of scientists — it would effectively give us a look inside some of the most enigmatic objects in the Solar System.”

Fireballs (or bolides) are the name given by astronomers to the brightest meteors, popularly referred to as shooting stars. On the afternoon of July 11, a brilliant fireball was recorded over southwestern Europe. At maximum intensity, the object was more than 150 times brighter than the full Moon. It was first picked up at a height of 61 miles (98.3 km) and disappeared from view 13 miles (21.5 km) above the surface of the Earth, tracked by three stations of the Spanish Fireball Network above Bejar, near Salamanca in Spain. At the same time, a professional photographer took a picture of the fireball from the north of Madrid.

A close-up image of the Bejar bolide, photographed from Torrelodones, Madrid, Spain. Credit: J. Perez Vallejo/SPMN.
A close-up image of the Bejar bolide, photographed from Torrelodones, Madrid, Spain. Credit: J. Perez Vallejo/SPMN.

From these images, the astronomers have demonstrated that before its fiery demise, the boulder traveled on an unusual orbit around the Sun, which took it from beyond the orbit of Jupiter to the vicinity of Earth. This orbit is very similar to that of a cloud of meteoroids known as the Omicron Draconids, which on rare occasions produces a minor meteor shower and probably originates from the breakup of Comet C/1919 Q2 Metcalf in 1920. The authors suggest the boulder was once embedded in the nucleus of that comet.

Comet C/1919 Q2 Metcalf was discovered by Joel Metcalf from Vermont in August 1919, and was visible until February 3, 1920. The orbit was not well determined and no subsequent appearances are known. The Omicron Draconids meteor stream was discovered to be following a similar orbit to this comet by Allan F. Cook in 1973. The stream characteristically produces bright fireballs and rare meteor outbursts.

In the mid-1980s, the astronomers Tamas I. Gombosi and Harry L.F. Houpis first suggested that the nuclei of comets consist of relatively large boulders cemented together by a ‘glue’ of smaller particles and ice. If the rocky and icy nucleus of a comet disintegrates, then these large boulders are set loose into space. If the Bejar bolide was formed in this way, it confirms the glue model for at least some comets.

Source: Royal Astronomical Society

How Does the Earth Protect Us From Space?

Earth's Magnetosphere. Credit: NASA

Our Earth keeps us very safe from a dangerous Universe that’s always trying to kill us in new and interesting ways.

Risk: Cosmic rays are high energy particles fired at nearly the speed of light by the Sun, supermassive black holes and supernovae. They have the ability to blast right through your body, damaging DNA as they go. Long term exposure to cosmic rays increases your chances of getting cancer. Fortunately, we have our atmosphere to protect us. As cosmic rays crash into the atmosphere, they collide with the oxygen and nitrogen molecules in the air.

Risk: Gamma rays and X-rays. As you know, radiation can damage the body. Just a single high-energy photon of gamma rays can cause significant damage to a living cell. Once again, though, the Earth’s atmosphere is there to protect us. The molecules in the atmosphere absorb the high-energy photons preventing any from reaching us on the ground. In fact, X-ray and gamma ray observatories need to be built in space because there’s no way we can see them from the ground.

Risk: Ultraviolet radiation. The Sun is bathing the Earth in ultraviolet radiation; that’s why you get a sunburn. But the ozone layer is a special region of the atmosphere that absorbs much of this radiation. Without the ozone layer we would be much more exposed here on the surface of the Earth to UV rays, leading to eye damage and greater incidence of skin cancer.

Risk: Solar flares. Violent explosions on the surface of the Sun release a huge amount of energy as flares. In addition to a blast of radiation, it often sends out a burst of plasma traveling at nearly the speed of light. The Earth’s magnetosphere protects us here on Earth from the effects of the plasma, keeping it safely away from the surface of the planet. And our atmosphere keeps the X-ray/gamma ray radiation out.

Risk: Cold temperatures. Space itself is just a few degrees above absolute zero, but our atmosphere acts like a blanket, keeping warm temperatures in. Without the atmosphere, we’d freeze almost instantly.

Risk: Vacuum. Space is airless. Without the Earth, there’d be no air to breath, and the lack of pressure damages cells and lets water evaporate out into space. Vacuum would be very, very bad.

If you’d like to hear more about cosmic rays, listen to this episode of Astronomy Cast.

References:
NASA: Danger of Solar and Cosmic Radiation in Space
NASA: Ultraviolet Waves

Weekend SkyWatcher’s Forecast – February 13-15, 2009

Greetings, fellow SkyWatchers! With the Moon gone from the early evening skies and the weather beginning to warm for northern climes, isn’t it about time you at least took a pair of binoculars out and scanned the skies with me? Some of mankind’s greatest astronomers were born over the next three days, included J.L.E. Dreyer, Fritz Zwicky, William Pickering and Galileo Galilei! Although our weekend targets are simple and you’ve probably already seen them before – how long has it been since you’ve last looked? Or tried with alternative sized optics? Ah… Yes. You begin to see the light! Come on. Dust those old binoculars off and head out into the back yard. I’ll be waiting…

dreyerFriday, February 13, 2009 – A bad luck day? Not hardly. It was rather fortunate, because Johan Ludvig Emil Dreyer, was born on this date in 1852. At age 30, Danish astronomer Dreyer became director of the Armagh Observatory—not a grand honor, considering the observatory was so broke it couldn’t afford to replace its equipment. Like all good directors, Dreyer somehow managed to get a new 10″ refractor but no funds for an assistant to practice traditional astronomy. However, J.L.E. was dedicated and within 6 years had compiled all observations known to him into one unified work called the New General Catalogue of Nebulae and Clusters of Stars (NGC). Originally containing 7,840 objects, and supplemented in 1895 and 1908 with another 5,386 designations, the NGC remains the standard reference catalog. Although Dreyer’s personal observations included such nebulous descriptions as ‘‘a vault of stars,’’ modern astronomers continue to use his abbreviations as a kind of shorthand.

Honor Dreyer tonight by discovering one of his catalog objects suited for all optics – NGC2287.

m41

Located about two finger-widths south of Alpha Canis Majoris (RA 06 46 00 Dec -20 46 00), only an open cluster this bright could stand up against brilliant Sirius. From a dark-sky location, your unaided eye can even spot this magnitude 4.5 “star vault” as a hazy patch. Aristotle saw it as early as 325 BC! Officially discovered by Hodierna, we know it best by the designation Messier Object 41. Even from 2,300 light-years away, the cluster’s brightest star, an orange giant, stands out clearly from the stellar nest. With large aperture, you’ll notice other K-type stars, all very similar to Sol. Although small scopes and binoculars won’t reveal too much color, you might pick up on the blue signature of young, hot stars. NGC 2287 could be anywhere from 190 to 240 million years old, but its stars shine as brightly now as they did in Aristotle’s day. . .and Dreyer’s!

Saturday, February 14, 2009 – Happy Valentine’s Day! On this date in 1747, astronomer James Bradley presented his evidence of Earth’s wobble, called nutation. The study took 19 years, but won Bradley the Copley Medal! In 1827, George Clark was born. The name might not ring a bell, but it was indeed a bell—melted down—that he used to create his first brass telescope. George’s family went on to produce the finest—and largest—telescopes of their time.

zwickyIn 1898 crabby astronomer Fritz Zwicky came along, his name synonymous with the theory of supernovae. The Swiss-born Caltech professor was also a salty character, often intimidating his colleague Walter Baade and referring to others as ‘‘spherical bastards.’’ Although Zwicky was difficult to work with, he was also brilliant—predicting the phenomenon of gravitational lensing.

Tonight we’ll look at a supernova remnant as we venture to the Crab Nebula. Finding M1 is easy: it can be seen with as little as 7X magnification. Locate Zeta Tauri (about halfway between Orion’s ‘‘head’’ and the southernmost bright star in Auriga) and aim about 1 degree northwest (RA 05 34 31 Dec -22 00 52).

m1Viewing M1 with small optics helps to understand why Charles Messier decided to compile his famous catalog. Unaware of its earlier discovery, Messier located a fuzzy object near the ecliptic and assumed it was the return of Halley’s Comet. Considering his primitive telescope, we can’t fault his observation. But Chuck was a good astronomer. When he realized the object wasn’t in motion, he began compiling a log of things not to be confused with comets—the famous Messier objects. Enjoy looking at this spectacular deep-sky jewel, and we’ll study it in depth another time. Of course, Zwicky would have cursed me for saying that observing without science is an ‘‘empty brain exercise and therefore a waste of time.’’ But on the date of his birth, I took his advice. . . ‘‘Give me a topic and I’ll give you an idea!’’

galileoSunday, February 15, 2009 – Are you ready to do a little IYA 2009 outreach? Then start now. This date’s astronomical births begin in 1564 with Galileo Galilei—pioneer of physics and astronomy—who didn’t invent the telescope but certainly perfected it. Arrested for heresy, Galileo entreated fellow scientists to discover the universal truths for themselves. His cry was ignored. To his friend, Johannes, he wrote: ‘‘I wish, my dear Kepler, that we could have a good laugh together at the extraordinary stupidity of the mob. What do you think of the foremost philosophers of this University? In spite of my oft-repeated efforts and invitations, they have refused, with the obstinacy of a glutted adder, to look at the planets or Moon or my telescope.’’

The birth of lunar and planetary observer William Pickering followed in 1858. During Pickering’s professional years at Harvard, he noted that the entire constellation of Orion is encased in faint nebulosity. Later verified by E.E. Barnard, this nebula is now known as Barnard’s Loop.

barnards_loop

With a very dark sky and excellent transparency, you can trace the ‘‘Loop’’ with binoculars. The area is so large and it’s pointless to provide coordinates, but the brightest portion extends eastward between Alpha and Kappa. Because the Orion complex contains so many rapidly evolving stars, it stands to reason a supernova has occurred there. Barnard’s Loop is probably the ancient shell leftover from such a cataclysmic event. If taken as a whole, it would encompass 10 degrees of sky! More difficult for Northern Hemisphere viewers is IC 2118, a huge reflection nebula west of Rigel known as the ‘‘Witch Head.’’ Once photographed by Pickering, IC 2118 is more sensitive to film than to the eye,
but that doesn’t mean you can’t see it. Sky conditions are the decisive factor, so look closely around the eastern edge where the fueling stars are brightest. You just might surprise yourself!

Until next week? Dreams really do come true when you keep on reaching for the stars!

This week’s awesome photos are: J.L.E. Dreyer (historical image), NGC 2287: M41 (credit—Palomar Observatory, courtesy of Caltech), Fritz Zwicky (historical image), Messier Object 1 (credit—Palomar Observatory, courtesy of Caltech), Galileo (historical image) and Eastern edge of IC 2118 (credit—Palomar Observatory, courtesy of Caltech).

What is the Smallest Star?

OGLE-TR-122b. Image credit: ESO

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The biggest stars in the Universe are the monster red hypergiants, measuring up to 1,500 times the size of the Sun. But what are the smallest stars in the Universe?

The smallest stars around are the tiny red dwarfs. These are stars with 50% the mass of the Sun and smaller. In fact, the least massive red dwarf has 7.5% the mass of the Sun. Even at this smallest size, a star has the temperature and pressures in its core so that nuclear fusion reactions can take place.

One example of red dwarf star is the closest star to Earth, Proxima Centauri, located just 4.2 light-years away. Proxima Centauri has 12% the mass of the Sun, and it’s estimated to be just 14.5% the size of the Sun. The diameter of Proxima Centauri is about 200,000 km. Just for comparison, the diameter of Jupiter is 143,000 km, so Proxima Centauri is only a little larger than Jupiter.

But that’s not the smallest star ever discovered.

The smallest known star right now is OGLE-TR-122b, a red dwarf star that’s part of a binary stellar system. This red dwarf the smallest star to ever have its radius accurately measured; 0.12 solar radii. This works out to be 167,000 km. That’s only 20% larger than Jupiter. You might be surprised to know that OGLE-TR-122b has 100 times the mass of Jupiter, but it’s only a little larger.

And that is the smallest known star. But there are certainly smaller stars out there. The smallest theoretical mass for a star to support nuclear fusion is 0.07 or 0.08 solar masses, so smaller stars are out there.

We have written many articles about stars here on Universe Today. Here’s an article about the biggest star in the Universe.

If you’d like more information on stars, check out Hubblesite’s News Releases about Stars, and here’s the stars and galaxies homepage.

We have recorded several episodes of Astronomy Cast about stars. Here are two that you might find helpful: Episode 12: Where Do Baby Stars Come From, and Episode 13: Where Do Stars Go When they Die?

Why Do Stars Die?

Not a black dwarf ... yet (white dwarf Sirius B)

Stars are mostly balls of hydrogen gas that came together from a nebula of gas and dust. They generate their energy through the process of fusion. This is where atoms of hydrogen are combined together to form helium atoms. And in the process, the star generates a tremendous amount of energy in the form of radiation. So, why do stars die?

This radiation starts up being trapped inside the star, and it can take more than 100,000 years to work its way out. You might not realize it, but light can emit a force when it bumps up against something. So all the light inside the star emits a pressure that opposes the force of gravity pulling all the material inward.

A star can exist in relative stability in this way for billions of years. Eventually, though, the star runs out of hydrogen fuel. At this point, a new reaction takes over, as helium atoms are fused together into heavier and heavier elements, like carbon and oxygen.

Once the helium is used up, a medium-mass star like our Sun just runs out of fuel. It can no longer sustain a fusion reaction. And without the pressure of the light ballooning it out, the star contracts down into a white dwarf – made mostly out of carbon.

A white dwarf star shines because it’s still very hot, but it slowly cools down over time. Eventually it will become cool enough that it’s invisible. And if we could wait long enough, the star would become a black dwarf star. The Universe hasn’t existed long enough for us to have any black dwarfs, but there are plenty of white dwarfs.

We have written many articles about stars here on Universe Today. Here’s an article about a hypergiant star that’s about to die.

If you’d like more information on stars, check out Hubblesite’s News Releases about Stars, and here’s the stars and galaxies homepage.

We have recorded several episodes of Astronomy Cast about stars. Here are two that you might find helpful: Episode 12: Where Do Baby Stars Come From, and Episode 13: Where Do Stars Go When they Die?

Why Do Stars Shine?

Sirius A
Sirius. Image credit: Hubble

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Head outside on a dark night and look up into the night sky. If you’re away from the bright city lights and it’s a clear night, you should see beautiful stars shining in the night. Just think, the light from those stars has traveled light-years through space to reach your eyes. But why do stars shine at all? Where is the light coming from?

All stars, and our own Sun is just an example, are hot balls of glowing plasma held together by their own gravity. And the gravity of a star is very intense. Stars are continuously crushing themselves inward, and the gravitational friction of this causes their interiors to heat up. A star like the Sun is a mere 5,800 Kelvin at its surface, but at its core, it can be 15 million Kelvin – now that’s hot!

The intense pressure and temperature at the core of a star allow nuclear fusion reactions to take place. This is where atoms of hydrogen are fused into atoms of helium (through several stages). This reaction releases an enormous amount of energy in the form of gamma rays. These gamma rays are trapped inside the star, and they push outward against the gravitational contraction of the star. That’s why stars hold to a certain size, and don’t continue contracting. The gamma rays jump around in the star, trying to get out. They’re absorbed by one atom, and then emitted again. This can happen many times a second, and a single photon can take 100,000 years to get from the core of the star to its surface.

When the photons have reached the surface, they’ve lost some of their energy, becoming visible light photons, and not the gamma rays they started out as. These photons leap off the surface of the Sun and head out in a straight line into space. They can travel forever if they don’t run into anything.

When you look at a star like Sirius, located about 8 light-years away, you’re seeing photons that left the surface of the star 8 years ago and traveled through space, without running into anything. Your eyeballs are the first thing those photons have encountered.

So why do stars shine? Because they have huge fusion reactors in their cores releasing a tremendous amount of energy.

We have written many articles about stars here on Universe Today. Here’s an article about an artificial star that astronomers create, and here’s an article about a star that recently shut down nuclear fusion in its core.

If you’d like more information on stars, check out Hubblesite’s News Releases about Stars, and here’s the stars and galaxies homepage.

We have recorded several episodes of Astronomy Cast about stars. Here are two that you might find helpful: Episode 12: Where Do Baby Stars Come From, and Episode 13: Where Do Stars Go When they Die?

References:
University of Illinois
NASA

Size of Stars

VY Canis Majoris. The biggest known star.
Size comparison between the Sun and VY Canis Majoris, which once held the title of the largest known star in the Universe. Credit: Wikipedia Commons/Oona Räisänen

As you probably can guess, our Sun is an average star. Stars can be bigger than the Sun, and stars can be smaller. Let’s take a look at the size of stars.

The smallest stars out there are the tiny red dwarfs. These are stars with no more than 50% the mass of the Sun, and they can have as little as 7.5% the mass of the Sun. This is the minimum mass you need for a star to be able to support nuclear fusion in its core. Below this mass and you get the failed star brown dwarfs. One fairly well known example of a red dwarf star is Proxima Centauri; the closest star to Earth. This star has about 12% the mass of the Sun, and about 14% the size of the Sun – about 200,000 km across, which is only a little larger than Jupiter.

Our own Sun is an example of an average star. It has a diameter of 1.4 million kilometers… today. But when our Sun nears the end of its life, it will bloat up as a red giant, and grow to 300 times its original size. This will consume the orbits of the inner planets: Mercury, Venus, and yes, even Earth.

An example of a larger star than our Sun is the blue supergiant Rigel in the constellation Orion. This is a star with 17 times the mass of the Sun, which puts out 66,000 times as much energy. Rigel is estimated to be 62 times as big as the Sun.

Bigger? No problem. Let’s take a look at the red supergiant Betelgeuse, also in the constellation Orion. Betelgeuse has 20 times the mass of the Sun, and it’s nearing the end of its life; astronomers think Betelgeuse might explode as a supernova within the next 1,000 years. Betelgeuse has bloated out to more than 1,000 times the size of the Sun. This would consume the orbit of Mars and almost reach Jupiter.

But the biggest star in the Universe is thought to be the monster VY Canis Majoris. This red hypergiant star is thought to be 1,800 times the size of the Sun. This star would almost touch the orbit of Saturn if it were in our Solar System.

We have written many articles about stars here on Universe Today. Here’s an article about the biggest star in the Universe, and here’s a more detailed article about red dwarfs.

If you’d like more information on stars, check out Hubblesite’s News Releases about Stars, and here’s the stars and galaxies homepage.

We have recorded several episodes of Astronomy Cast about stars. Here are two that you might find helpful: Episode 12: Where Do Baby Stars Come From, and Episode 13: Where Do Stars Go When they Die?

References:
http://www.telescope.org/pparc/res8.html
http://en.wikipedia.org/wiki/Proxima_Centauri
http://www.windows2universe.org/sun/statistics.html
http://earthsky.org/brightest-stars/blue-white-rigel-is-orions-brightest-star

Mass of Stars

Sirius A
Sirius. Image credit: Hubble

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Stars can range in mass from the least massive red dwarf stars to the monstrous hypergiant stars. Let’s take a look at the mass of stars at various sizes.

The least massive stars in the Universe are the red dwarf stars. These are stars with less than 50% the mass of the Sun, and they can be as small as 7.5% the mass of the Sun. This tiny mass is the minimum amount of gravitational force you need for a star to be able to raise the temperature in its core to the point that nuclear fusion can begin. If an object is less than this 7.5%, or about 80 times the mass of Jupiter, it can never get going; astronomers call these failed stars brown dwarfs. Instead of having nuclear fusion in their cores, brown dwarfs are heated by the gravitational friction of their ongoing collapse.

Above 50% the mass of the Sun, and you start to get colors other than red. The least massive stars are orange, and then yellow, and then white. Our own Sun is about the least massive example you can have of a white star (it looks yellow, but that’s just because of the Earth’s atmosphere).

The most massive stars are the blue giants, supergiants and hypergiants. Rigel, for example, is the brightest star in the constellation Orion. It has 17 times the mass of the Sun, and gives off 66,000 times the energy of the Sun.

But an even more extreme example is the blue hypergiant Eta Carinae, located about 8,000 light-years away. Eta Carinae is thought to have 150 times the mass of the Sun and puts out 4 million times as much energy. It’s probably less than 3 million years old, and astronomers guess that it will detonate as a supernova within 100,000 years. The most massive stars live the shortest lives.

We have written many articles about stars here on Universe Today. Here’s an article about the upper limits on star mass, and the discovery of a Jupiter-sized star.

If you’d like more information on stars, check out Hubblesite’s News Releases about Stars, and here’s the stars and galaxies homepage.

We have recorded several episodes of Astronomy Cast about stars. Here are two that you might find helpful: Episode 12: Where Do Baby Stars Come From, and Episode 13: Where Do Stars Go When they Die?