Arctic winter sea ice extent 2nd lowest

Sea ice in the Arctic grew to its annual maximum extent – the largest ice-covered area of the year – last week. NASA scientists said 2018 joined 2015, 2016 and 2017 as the four lowest maximum extents on record.

The sea ice covering the Arctic Ocean melts and regrows in an annual cycle, thickening and expanding throughout the winter months and melting in the spring and summer. The ice cover generally reaches its maximum extent sometime in late February or March. After that, ice melts through the summer, hitting a low point in early or mid-September. Arctic sea ice has been declining both during the growing and melting seasons in recent decades.

On March 17, 2018, the Arctic sea ice cover peaked at 5.59 million square miles (14.48 million square km), making it the second lowest maximum on record, at about 23,200 square miles (60,000 square km) larger than the record low maximum reached on March 7, 2017, according an analysis by scientists at the National Snow and Ice Data Center (NSIDC) and NASA.

The last four years reached nearly equally low maximum extents, and this year continues the decades-long trend of diminishing sea ice in the Arctic. Claire Parkinson is senior climate scientist at NASA’s Goddard Space Flight Center in Greenbelt, Maryland. She said in a statement:

The Arctic sea ice cover continues to be in a decreasing trend and this is connected to the ongoing warming of the Arctic. It’s a two-way street: the warming means less ice is going to form and more ice is going to melt, but also, because there’s less ice, less of the sun’s incident solar radiation is reflected off, and this contributes to the warming.

On March 17, the Arctic sea ice cover peaked at 5.59 million square miles (14.48 million square km), making it the second lowest maximum on record. Image via NASA/ Nathan Kurtz.

Alek Petty is a sea ice researcher at Goddard. Petty said in a statement:

This old, thicker ice is what we expect to provide stability to the Arctic sea ice system, since we expect that ice not to be as vulnerable to melting out as thinner, younger ice. As ice in the Arctic becomes thinner and more mobile, it increases the likelihood for rapid ice loss in the summer.

Despite the fact that this year’s melt season will begin with a low winter sea ice extent, this doesn’t necessarily mean that we will see another record low summertime extent. Parkinson said:

A lot will depend on what the wind and temperature conditions will be in the spring and summer.

The decline of the Arctic sea ice cover has myriad effects, from changes in climate and weather patterns to impacts on the plants and animals dependent on the ice, and to the indigenous human communities that rely on them. The disappearing ice is also altering shipping routes, increasing coastal erosion and affecting ocean circulation.

Bottom line: The 2018 Arctic sea ice maximum extent is the second lowest on record, say NASA scientists.

Read more from NASA



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Sea ice in the Arctic grew to its annual maximum extent – the largest ice-covered area of the year – last week. NASA scientists said 2018 joined 2015, 2016 and 2017 as the four lowest maximum extents on record.

The sea ice covering the Arctic Ocean melts and regrows in an annual cycle, thickening and expanding throughout the winter months and melting in the spring and summer. The ice cover generally reaches its maximum extent sometime in late February or March. After that, ice melts through the summer, hitting a low point in early or mid-September. Arctic sea ice has been declining both during the growing and melting seasons in recent decades.

On March 17, 2018, the Arctic sea ice cover peaked at 5.59 million square miles (14.48 million square km), making it the second lowest maximum on record, at about 23,200 square miles (60,000 square km) larger than the record low maximum reached on March 7, 2017, according an analysis by scientists at the National Snow and Ice Data Center (NSIDC) and NASA.

The last four years reached nearly equally low maximum extents, and this year continues the decades-long trend of diminishing sea ice in the Arctic. Claire Parkinson is senior climate scientist at NASA’s Goddard Space Flight Center in Greenbelt, Maryland. She said in a statement:

The Arctic sea ice cover continues to be in a decreasing trend and this is connected to the ongoing warming of the Arctic. It’s a two-way street: the warming means less ice is going to form and more ice is going to melt, but also, because there’s less ice, less of the sun’s incident solar radiation is reflected off, and this contributes to the warming.

On March 17, the Arctic sea ice cover peaked at 5.59 million square miles (14.48 million square km), making it the second lowest maximum on record. Image via NASA/ Nathan Kurtz.

Alek Petty is a sea ice researcher at Goddard. Petty said in a statement:

This old, thicker ice is what we expect to provide stability to the Arctic sea ice system, since we expect that ice not to be as vulnerable to melting out as thinner, younger ice. As ice in the Arctic becomes thinner and more mobile, it increases the likelihood for rapid ice loss in the summer.

Despite the fact that this year’s melt season will begin with a low winter sea ice extent, this doesn’t necessarily mean that we will see another record low summertime extent. Parkinson said:

A lot will depend on what the wind and temperature conditions will be in the spring and summer.

The decline of the Arctic sea ice cover has myriad effects, from changes in climate and weather patterns to impacts on the plants and animals dependent on the ice, and to the indigenous human communities that rely on them. The disappearing ice is also altering shipping routes, increasing coastal erosion and affecting ocean circulation.

Bottom line: The 2018 Arctic sea ice maximum extent is the second lowest on record, say NASA scientists.

Read more from NASA



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Mizar and Alcor, famous double star

Mizar and Alcor. Image via F. Espenak/astropixels.

Mizar and its fainter companion star Alcor are one of the most famous double stars in the sky. You’ll spot Mizar first, as the middle star of the Big Dipper’s handle. Look closely, and you’ll see Alcor right next to Mizar.

Mizar and Alcor appear so closely linked in our sky’s dome that they’re often said to be a test of eyesight. But in fact even people with less than perfect eyesight can see the two stars, especially if they’re looking in a dark clear sky. This pair of stars in the Big Dipper’s handle is famously called “the horse and rider.” If you can’t see fainter Alcor with the unaided eye, use binoculars to see Mizar’s nearby companion.

At this time of year,the Big Dipper is in the northeast. The famous star Mizar is second to the end of the Dipper’s handle. Look closely, and you’ll see Alcor right next to Mizar.

Located in the handle of the Big Dipper, Mizar (brighter) and Alcor (fainter) are one of the most famous visual double stars in the sky. Image via ESO Online Digitized Sky Survey.

Mizar is perhaps the Big Dipper’s most famous star, glorified in the annals of astronomy many times over. Apart from Alcor, Mizar in itself became known a double star in 1650. In fact, it was the first double star to be seen through a telescope.

Few, if any, astronomers back then even dreamed that double stars were anything other than chance alignments of physically unrelated stars. Yet, in 1889, an instrument called a spectroscope revealed that Mizar’s brighter telescopic component consisted of two stars – making Mizar the first binary star ever discovered by spectroscopic means.

At a later date, Mizar’s dimmer telescopic component also showed itself to be a spectroscopic binary, meaning that Mizar consists of two sets of binaries – making it a quadruple star.

As for Alcor, it was long believed that Mizar and Alcor were not gravitationally bound and did not form a true binary star system. In 2009, though, two groups of astronomers independently reported that Alcor actually is itself a binary, consisting of Alcor A and Alcor B. Astronomers now believe that the Alcor binary system is gravitationally bound to the Mizar quadruple system – making six stars in all, where we see only two with the eye.

Thus Mizar and Alcor not only test eyesight, but the limits of our technological vision as well.

Bottom line: Famous double stars Mizar and Alcor are easy to find in the handle of the Big Dipper. Mizar is really four stars, and Alcor is really two stars. So what we see as two stars are really six in one!



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Mizar and Alcor. Image via F. Espenak/astropixels.

Mizar and its fainter companion star Alcor are one of the most famous double stars in the sky. You’ll spot Mizar first, as the middle star of the Big Dipper’s handle. Look closely, and you’ll see Alcor right next to Mizar.

Mizar and Alcor appear so closely linked in our sky’s dome that they’re often said to be a test of eyesight. But in fact even people with less than perfect eyesight can see the two stars, especially if they’re looking in a dark clear sky. This pair of stars in the Big Dipper’s handle is famously called “the horse and rider.” If you can’t see fainter Alcor with the unaided eye, use binoculars to see Mizar’s nearby companion.

At this time of year,the Big Dipper is in the northeast. The famous star Mizar is second to the end of the Dipper’s handle. Look closely, and you’ll see Alcor right next to Mizar.

Located in the handle of the Big Dipper, Mizar (brighter) and Alcor (fainter) are one of the most famous visual double stars in the sky. Image via ESO Online Digitized Sky Survey.

Mizar is perhaps the Big Dipper’s most famous star, glorified in the annals of astronomy many times over. Apart from Alcor, Mizar in itself became known a double star in 1650. In fact, it was the first double star to be seen through a telescope.

Few, if any, astronomers back then even dreamed that double stars were anything other than chance alignments of physically unrelated stars. Yet, in 1889, an instrument called a spectroscope revealed that Mizar’s brighter telescopic component consisted of two stars – making Mizar the first binary star ever discovered by spectroscopic means.

At a later date, Mizar’s dimmer telescopic component also showed itself to be a spectroscopic binary, meaning that Mizar consists of two sets of binaries – making it a quadruple star.

As for Alcor, it was long believed that Mizar and Alcor were not gravitationally bound and did not form a true binary star system. In 2009, though, two groups of astronomers independently reported that Alcor actually is itself a binary, consisting of Alcor A and Alcor B. Astronomers now believe that the Alcor binary system is gravitationally bound to the Mizar quadruple system – making six stars in all, where we see only two with the eye.

Thus Mizar and Alcor not only test eyesight, but the limits of our technological vision as well.

Bottom line: Famous double stars Mizar and Alcor are easy to find in the handle of the Big Dipper. Mizar is really four stars, and Alcor is really two stars. So what we see as two stars are really six in one!



from EarthSky https://ift.tt/1FtE7MH

Summer Triangle, signpost for all seasons

Tonight, look for the Summer Triangle. It’s not summer for our northern temperate latitudes, but the three brilliant stars of the Summer Triangle – Vega, Deneb and Altair – are out for at least part of the night every night of the year. Presently, the Summer Triangle shines in the eastern predawn sky. You can often see this star formation from light-polluted areas or on a moonlit night.

Like the Big Dipper, the Summer Triangle is an asterism – a pattern of stars that is not one of the officially recognized 88 constellations. To gauge the size of this signpost star formation, hold a ruler an arm’s length from your eye. The ruler pretty much fills the gap between Vega and Altair, the Summer Triangle’s first and second brightest stars, respectively.

On a moonless night, an edgewise view of the galactic disk - and the Dark Rift - pass right through the Summer Triangle. Photo credit: cipdatajeffb

On a moonless night, an edgewise view of the galactic disk – and the Dark Rift – passes right through the Summer Triangle. Photo credit: cipdatajeffb

Like all the stars, the stars of the Summer Triangle rise four minutes earlier every day, or two hours earlier every month. Why is this happening? It’s happening because Earth is orbiting the sun, and our night sky is pointing out on an ever-changing panorama of stars.

Around May Day – May 1 – the Summer Triangle will climb over the eastern horizon around local midnight (1 a.m. daylight saving time). When middle to late June comes rolling along, you’ll see the Summer Triangle sparkling in the east at evening dusk – a sure sign of summer’s return to the Northern Hemisphere.

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Nils Ribi caught this photo of the Summer Triangle on a northern autumn evening - November 8, 2014. View larger and read Nils' story of this photo.

Nils Ribi caught this photo of the Summer Triangle on a northern autumn evening – November 8, 2014. View larger and read Nils’ story of this photo.

Bottom line: The Summer Triangle can be seen for most of the year. Its three brilliant stars – Vega, Deneb and Altair – are up before dawn in March, before midnight in May and at dusk on the summer solstice.

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Tonight, look for the Summer Triangle. It’s not summer for our northern temperate latitudes, but the three brilliant stars of the Summer Triangle – Vega, Deneb and Altair – are out for at least part of the night every night of the year. Presently, the Summer Triangle shines in the eastern predawn sky. You can often see this star formation from light-polluted areas or on a moonlit night.

Like the Big Dipper, the Summer Triangle is an asterism – a pattern of stars that is not one of the officially recognized 88 constellations. To gauge the size of this signpost star formation, hold a ruler an arm’s length from your eye. The ruler pretty much fills the gap between Vega and Altair, the Summer Triangle’s first and second brightest stars, respectively.

On a moonless night, an edgewise view of the galactic disk - and the Dark Rift - pass right through the Summer Triangle. Photo credit: cipdatajeffb

On a moonless night, an edgewise view of the galactic disk – and the Dark Rift – passes right through the Summer Triangle. Photo credit: cipdatajeffb

Like all the stars, the stars of the Summer Triangle rise four minutes earlier every day, or two hours earlier every month. Why is this happening? It’s happening because Earth is orbiting the sun, and our night sky is pointing out on an ever-changing panorama of stars.

Around May Day – May 1 – the Summer Triangle will climb over the eastern horizon around local midnight (1 a.m. daylight saving time). When middle to late June comes rolling along, you’ll see the Summer Triangle sparkling in the east at evening dusk – a sure sign of summer’s return to the Northern Hemisphere.

EarthSky astronomy kits are perfect for beginners. Order today from the EarthSky store

Enjoying EarthSky so far? Sign up for our free daily newsletter today!

Nils Ribi caught this photo of the Summer Triangle on a northern autumn evening - November 8, 2014. View larger and read Nils' story of this photo.

Nils Ribi caught this photo of the Summer Triangle on a northern autumn evening – November 8, 2014. View larger and read Nils’ story of this photo.

Bottom line: The Summer Triangle can be seen for most of the year. Its three brilliant stars – Vega, Deneb and Altair – are up before dawn in March, before midnight in May and at dusk on the summer solstice.

Donate: Your support means the world to us



from EarthSky https://ift.tt/1EiQYis

The Peeps experiments: A seasonal celebration of science

Why experiment on Peeps? "Because they're there!" says Emory chemist Douglas Mulford.

It’s that time of year again when Peepus Marshmalleous, commonly known as Peeps, pop up everywhere — even in an Emory University chemistry lab.

Emory's groundbreaking Peeps research began in 1999 when researchers Gary Falcon and James Zimming investigated the effects of smoking and alcohol on Peeps health and performed the medical miracle of separating quintuplet Peep siblings, conjoined at birth. You can read more here: peepresearch

Douglas Mulford, senior lecturer and director of undergraduate studies for the Department of Chemistry, continues the tradition by treating students every Spring to a Peeps show. “Basically, it’s 45-minutes of every chemical thing that you can do to a Peeps,” Mulford explains. “It’s amazing what they can survive.” 

Watch a brief video summarizing the show, below. And check out Emory’s new Instagram account, Science Seen, for more quick, behind-the-scenes looks at science at Emory.



from eScienceCommons https://ift.tt/2GhgPVn
Why experiment on Peeps? "Because they're there!" says Emory chemist Douglas Mulford.

It’s that time of year again when Peepus Marshmalleous, commonly known as Peeps, pop up everywhere — even in an Emory University chemistry lab.

Emory's groundbreaking Peeps research began in 1999 when researchers Gary Falcon and James Zimming investigated the effects of smoking and alcohol on Peeps health and performed the medical miracle of separating quintuplet Peep siblings, conjoined at birth. You can read more here: peepresearch

Douglas Mulford, senior lecturer and director of undergraduate studies for the Department of Chemistry, continues the tradition by treating students every Spring to a Peeps show. “Basically, it’s 45-minutes of every chemical thing that you can do to a Peeps,” Mulford explains. “It’s amazing what they can survive.” 

Watch a brief video summarizing the show, below. And check out Emory’s new Instagram account, Science Seen, for more quick, behind-the-scenes looks at science at Emory.



from eScienceCommons https://ift.tt/2GhgPVn

Astronomers spy runaway star in Small Magellanic Cloud

Astrophotographer Justin Ng caught the edgewise view into our Milky Way galaxy, the bright star Canopus and the Large and Small Magellanic Clouds at sunrise, in September 2013, over East Java’s Mount Bromo. Canopus is a yellow supergiant, much like the recently discovered runaway star. Read more about this image.

Astronomers at Lowell Observatory in Flagstaff, Arizona said on March 27, 2018 that they’ve discovered a rare runaway star in the Small Magellanic Cloud, a small satellite galaxy of our Milky Way. The star is speeding across its little galaxy at a 300,000 miles per hour (500,000 km/hour). At that speed, it would take about half a minute to travel from Los Angeles to New York. The runaway star is designated J01020100-7122208, and it’s believed to have once been one of two stars orbiting around each other. Astronomers think that, when the companion star exploded as a supernova, the tremendous release of energy flung J01020100-7122208 into space at its high speed.

The star is the first runaway yellow supergiant star ever discovered, and only the second evolved runaway star to be found in another galaxy. A paper about its discovery has been accepted for publication in the peer-reviewed Astronomical Journal and is currently published online via Arxiv. A statement from Lowell Observatory said:

After ten million years of traveling through space, the star evolved into a yellow supergiant, the object that we see today. Its journey took it 1.6 degrees across the sky, about three times the diameter of the full moon. The star will continue speeding through space until it too blows up as a supernova, likely in another three million years or so. When that happens, heavier elements will be created, and the resulting supernova remnant may form new stars or even planets on the outer edge of the Small Magellanic Cloud.

Astronomy graduate student Kathryn Neugent of Lowell Observatory in Flagstaff and the University of Washington in Seattle, Washington led an international group of astronomers who discovered and studied the star. The Small Magellanic Cloud cannot be viewed from Earth’s Northern Hemisphere. The team made the discovery using the National Optical Astronomy Observatory’s 4-meter Blanco telescope, and the Carnegie Observatory’s 6.5-meter Magellan telescope, both located northern Chile.

Yellow supergiants are very rare objects because the yellow supergiant phase is thought to be so short. Yet we have some famous examples of yellow supergiants visible in Earth’s skies, including the North Star, Polaris, and the star Canopus, second-brightest star in the entire sky. Lowell Observatory said:

A massive star may live for as much as ten million years but the yellow supergiant phase itself lasts only ten to a hundred thousand years, an eye-blink in the life of a star. After this short time, yellow supergiants expand into giant red supergiants, like Betelgeuse, with sizes as large as the orbits of Mars or Jupiter. These stars eventually die in spectacular supernova explosions.

Thus the newly discovered runaway star is destined to end its life as its companion did, as a supernova, or exploding star.

Observations of the yellow supergiant runaway were conducted using the large 6.5-meter Magellan telescope at Las Campanas Observatory. The Large Magellanic Cloud (companion galaxy to the Small Magellanic Cloud, not shown) is visible right above the telescope enclosure. The bright band of light from lower left to upper right is the southern Milky Way. Photo by Kathryn Neugent via Lowell Observatory.

Bottom line: Astronomers using telescopes in northern Chile have discovered a rare runaway star in the Small Magellanic Cloud. The star is designated J01020100-7122208. It’s speeding across its little galaxy at a 300,000 miles per hour (500,000 km/hour).

Source: Runaway Yellow Supergiant Star in the Small Magellanic Cloud

Via Lowell Observatory



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Astrophotographer Justin Ng caught the edgewise view into our Milky Way galaxy, the bright star Canopus and the Large and Small Magellanic Clouds at sunrise, in September 2013, over East Java’s Mount Bromo. Canopus is a yellow supergiant, much like the recently discovered runaway star. Read more about this image.

Astronomers at Lowell Observatory in Flagstaff, Arizona said on March 27, 2018 that they’ve discovered a rare runaway star in the Small Magellanic Cloud, a small satellite galaxy of our Milky Way. The star is speeding across its little galaxy at a 300,000 miles per hour (500,000 km/hour). At that speed, it would take about half a minute to travel from Los Angeles to New York. The runaway star is designated J01020100-7122208, and it’s believed to have once been one of two stars orbiting around each other. Astronomers think that, when the companion star exploded as a supernova, the tremendous release of energy flung J01020100-7122208 into space at its high speed.

The star is the first runaway yellow supergiant star ever discovered, and only the second evolved runaway star to be found in another galaxy. A paper about its discovery has been accepted for publication in the peer-reviewed Astronomical Journal and is currently published online via Arxiv. A statement from Lowell Observatory said:

After ten million years of traveling through space, the star evolved into a yellow supergiant, the object that we see today. Its journey took it 1.6 degrees across the sky, about three times the diameter of the full moon. The star will continue speeding through space until it too blows up as a supernova, likely in another three million years or so. When that happens, heavier elements will be created, and the resulting supernova remnant may form new stars or even planets on the outer edge of the Small Magellanic Cloud.

Astronomy graduate student Kathryn Neugent of Lowell Observatory in Flagstaff and the University of Washington in Seattle, Washington led an international group of astronomers who discovered and studied the star. The Small Magellanic Cloud cannot be viewed from Earth’s Northern Hemisphere. The team made the discovery using the National Optical Astronomy Observatory’s 4-meter Blanco telescope, and the Carnegie Observatory’s 6.5-meter Magellan telescope, both located northern Chile.

Yellow supergiants are very rare objects because the yellow supergiant phase is thought to be so short. Yet we have some famous examples of yellow supergiants visible in Earth’s skies, including the North Star, Polaris, and the star Canopus, second-brightest star in the entire sky. Lowell Observatory said:

A massive star may live for as much as ten million years but the yellow supergiant phase itself lasts only ten to a hundred thousand years, an eye-blink in the life of a star. After this short time, yellow supergiants expand into giant red supergiants, like Betelgeuse, with sizes as large as the orbits of Mars or Jupiter. These stars eventually die in spectacular supernova explosions.

Thus the newly discovered runaway star is destined to end its life as its companion did, as a supernova, or exploding star.

Observations of the yellow supergiant runaway were conducted using the large 6.5-meter Magellan telescope at Las Campanas Observatory. The Large Magellanic Cloud (companion galaxy to the Small Magellanic Cloud, not shown) is visible right above the telescope enclosure. The bright band of light from lower left to upper right is the southern Milky Way. Photo by Kathryn Neugent via Lowell Observatory.

Bottom line: Astronomers using telescopes in northern Chile have discovered a rare runaway star in the Small Magellanic Cloud. The star is designated J01020100-7122208. It’s speeding across its little galaxy at a 300,000 miles per hour (500,000 km/hour).

Source: Runaway Yellow Supergiant Star in the Small Magellanic Cloud

Via Lowell Observatory



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How could global warming accelerate if CO2 is 'logarithmic'?

After publishing my experiences talking to science 'dismissives' (or 'skeptics', or whatever you'd like to call them) and then participating in the excellent Denial101x course, I was invited to join the volunteer team at SkepticalScience last year.

But before all that, one of the dismissives drew my attention to a climate science paradox:

  1. Scientists agree that the greenhouse effect is approximately logarithmic — which means that as we add more CO2 to the atmosphere, the effect of extra CO2 decreases.
  2. However, the IPCC projects that if we don't take steps to reduce our emissions, global warming won't just get worse, it will speed up:

IPCC AR5 warming projections

Figure 1: From IPCC AR5 synthesis report, page 11

How could both facts be true, I wondered? At the time I turned to "Ask A Climate Scientist" on Facebook and got a response from Steve Sherwood, an atmospheric scientist and one of the hundreds of IPCC report authors. I thought my first post here at SkS would be a good opportunity to share what I learned.

So what is this "logarithmic effect" exactly? It looks like this:

Figure 2: The surface receives about 3.7 W/m2 more energy each time CO2 is doubled.

In the last million years, CO2 levels have cycled between about 180 and 280 ppm during cycles about 100,000 years long. Because this happened in the steep part of the curve, a change of only 100 ppm (together with the Milankovich cycles) was enough to move the world in and out of the ice ages. Even though humans have increased the CO2 concentration by 130 ppm already, this extra 130 ppm has a smaller effect than the 100 ppm that was added naturally before.

But let's zoom in on the part that we actually care about: the modern era.

Figure 3

After zooming in, the logarithm doesn't make such a big difference: it's not far from a straight line. 560ppm will probably take us well beyond the Paris target of 1.5°C, so the 280-560 range is key; we would be unwise to let our civilization go beyond 560.

But human CO2 emissions are increasing exponentially—fast enough that when we plot atmospheric CO2 with a logarithmic scale, it still curves up, even over the last 30 years:

Figure 4

Exponential growth appears as a straight line on a logarithmic chart; an upward curve means, in some sense, faster than exponential growth.1 So if human emissions keep increasing as they have, it makes perfect sense that global warming would speed up.

"But wait," I hear you think, "surely it won't increase exponentially forever?" You're right, of course, it won't, but it could continue for awhile, and in total there are four factors that could work together to speed up warming:

  1. Rapid economic development
  2. Past emissions
  3. Carbon sink saturation
  4. Committed warming

1. The developing world is developing fast.

The late Hans Rosling explains this very well in his talk, "How Not to be Ignorant about the World". Poverty is decreasing faster than ever—which, I would think, means more power plants being built than ever before. Right now, about 1600 of those new power plants will burn coal. And as long as most of the world has a standard of living well below China's, there is plenty of room for growth to continue and perhaps even accelerate.

2. Past emissions (CO2 is cumulative)

Once we add CO2 to the atmosphere, we face the law of conservation of matter: it won't go away unless something removes it.

This is related to another paradox you might have heard: methane produces a much stronger greenhouse effect than CO2, yet scientists are less worried about it. Why? For one thing, it has a much lower concentration in the atmosphere, but what's really important here is that it has a short lifetime of only about 12 years before it is destroyed in the methane cycle. That makes the methane problem much less serious, as we expect nature will clean up the mess when we eventually reduce our methane output.

Carbon dioxide doesn't go away so easily. Here's a graph from Joos et al. (2013) estimating how slowly a large "pulse" (sudden addition) of CO2 would leave the atmosphere:

Figure 5

The black line is an average of many other studies and models. At first, the ocean and land absorb it "quickly", so about half of it is gone after "only" 50 years, locked up in seawater and plants. But the next 25% takes a full 950 years to go away! After 1000 years, the ocean has absorbed 59% (contributing to ocean acidification) and the land 16%, leaving 25% behind.

CO2 accumulation itself can't make global warming speed up, but what it does is prevent it from stopping by ensuring that the greenhouse forcing keeps going up. If you look at a graph of human emissions instead of atmospheric concentration, it's only roughly exponential. Human emissions temporarily stalled in the early 80s and early 90s, but since CO2 accumulates, the atmospheric curve just kept going up unabated.

3. Carbon sinks can saturate

Right now, carbon sinks (oceans, plants, and others) are removing about 2.4ppm of CO2 from the atmosphere each year, while we're adding about 5.2ppm, for a net increase of 2.5ppm per year.2

Figure 6: Where our emissions go (source)

While nature removes about half of our carbon emissions each year now, don't assume our good fortune will last. According to Jones et. al., 2013, there is disagreement between various climate models about the details, but on average, under the business-as-usual scenario known as RCP 8.5, the land is projected to absorb less CO2 as time goes on, and the fraction of our emissions absorbed by oceans will decrease too (even if the absolute absorption rate increases). In other words, just because we emit more doesn't guarantee nature absorbs more; sooner or later, CO2 will accumulate faster in the atmosphere. (On average about 2/3 of new emissions will stay in the atmosphere this century under RCP 8.5, where last century it was less than half.)

Basically, the oceans can absorb CO2 at first; increasing the CO2 in the air will always make oceans absorb more. However, as the oceans warm up, carbon solubility decreases—warm water can't hold as much of it, and the only reason ocean absorption will continue after that is that oceans are enormous and take time to "fill up", as the carbon spreads deeper and deeper. Given enough time, oceans would "saturate" and become unable to absorb more. Similarly, CO2 enhances plant growth to some extent, but growth is eventually balanced out by plant decomposition (which releases CO2), and the long-term effects of climate change won't necessarily be good for plants.

CO2 will eventually be removed permanently through a process called weathering—but this will take thousands of years.

4. Committed warming

Earth's climate system has feedback loops that magnify the warming effect of CO2. For example, as the arctic ice melts, it exposes ocean. The ocean is much darker than the ice, so more sunlight is absorbed instead of being reflected back to space. This enhances the arctic warming effect. This effect is time-delayed, since it takes many years for the arctic ocean to warm up (which in turn causes the ice to melt more quickly in the future, which in turn helps the ocean to heat up even more.)

"Committed warming" refers to future warming effects that would still happen even if CO2 levels stop increasing. A large source of delayed warming worldwide is the oceans, which, as you can see here, have not kept up with the warming of the land:

Figure 7

As our massive oceans slowly heat up, they will not only increase the global average surface temperature, but they will also warm up the land further, especially near the ocean where ocean temperature strongly affects the land.3

Figure 8 based on IPCC AR4 5.2.2.3

Due to this delayed warming, climate scientists have separate short-term and long-term estimates of global warming:

Figure 9: Warming from various CO2 levels based on a typical TCR estimate of 1.8°C and the most commonly-cited estimate of ECS, 3°C. Various scientific groups have produced a range of TCR and ECS estimates; the precise concentration of CO2 that corresponds to 1.5°C is unknown (the bars marked "Paris target" are drawn wide to represent the uncertainty, but are not scientifically accurate error bars). And of course, this graph is just a first-order approximation. The real climate will be warmed further by other greenhouse gases, especially methane, and the real climate has additional variability and unpredictability, as do all computer models of it.

As you can see, in the short term there is technically still time to fulfill the Paris agreement and keep global warming under 1.5°C—but this graph ignores methane, which moves the target closer. Unfortunately it is considered highly unlikely that we'll be able to stop at our 1.5°C goal.

The long term outlook is even worse: we've already passed 1.5.

The good news is that reaching the long-term "equilibrium" climate will take hundreds of years, giving us time to, hopefully, reverse course and avoid a lot of that committed warming. But it's very likely—especially after we pass 1.5°C—that humanity will someday need to figure out how to remove CO2 from the atmosphere on a large scale.

In summary:

Although CO2 has less effect at higher CO2 concentrations, this "logarithmic effect" will be overpowered by these 4 factors if we don't switch to clean energy quickly:

  1. Exponential growth of energy use
  2. Past CO2 emissions that nature has not yet absorbed
  3. Carbon sink saturation
  4. Committed warming

What if we manage to stop increasing our emissions? This related article indicates that if emissions hold steady, global warming will still continue upward linearly.

Good news though: the price of solar panels has passed an important milestone. Around the equator where sunlight is strongest, unsubsidized solar power plants have dropped below the price of coal. Hooray for Swanson's law! I also like to point out that a new kind of safe and cheap nuclear reactor will—if the public supports it—begin production in the 2020s. And on a graph of human CO2 emissions you can see emissions have stalled. Is this temporary, like it was in the early 80s and 90s, or are we finally at a turning point? Perhaps, but the IEA forecast still includes new fossil fuel plants in the coming years.

Footnotes

1 This may sound more dramatic than it is; the human emission increase has been exponential, not faster than exponential, so the upward curvature is caused by something else. I believe it's because we're in a transition region between roughly constant CO2 of the past (280 ppm) and the new pattern of exponentially increasing CO2. Inside the transition region, an upward curve is expected.

2 Note: due to uncertainties, the numbers don't add up perfectly (2.4+2.5≠5.2). These numbers are based on the average of the last 5 years of Global Carbon Budget data, i.e. 9.8 GtC emitted by humans per year, 1.39 GtC added via land-use change, 2.5 GtC removed by oceans and 2.63 GtC removed by land. These numbers are estimates, and the observed change is 2.51 ppm (5.32 GtC) per year, which is 0.33 ppm (0.71 GtC) different than expected. Data sources and uncertainty levels are listed here. The conversion factor is 2.13 GtC/ppm.

3 There is some good news: climate models say the oceans will never warm up as much as the land does. See Sutton et al. 2007 for details.

P.S. Why does CO2 have a logarithmic effect? It's complicated; see Myhre et al. (2008) or  Huang & Shahabadi (2014) for technical details.



from Skeptical Science https://ift.tt/2Gi890H

After publishing my experiences talking to science 'dismissives' (or 'skeptics', or whatever you'd like to call them) and then participating in the excellent Denial101x course, I was invited to join the volunteer team at SkepticalScience last year.

But before all that, one of the dismissives drew my attention to a climate science paradox:

  1. Scientists agree that the greenhouse effect is approximately logarithmic — which means that as we add more CO2 to the atmosphere, the effect of extra CO2 decreases.
  2. However, the IPCC projects that if we don't take steps to reduce our emissions, global warming won't just get worse, it will speed up:

IPCC AR5 warming projections

Figure 1: From IPCC AR5 synthesis report, page 11

How could both facts be true, I wondered? At the time I turned to "Ask A Climate Scientist" on Facebook and got a response from Steve Sherwood, an atmospheric scientist and one of the hundreds of IPCC report authors. I thought my first post here at SkS would be a good opportunity to share what I learned.

So what is this "logarithmic effect" exactly? It looks like this:

Figure 2: The surface receives about 3.7 W/m2 more energy each time CO2 is doubled.

In the last million years, CO2 levels have cycled between about 180 and 280 ppm during cycles about 100,000 years long. Because this happened in the steep part of the curve, a change of only 100 ppm (together with the Milankovich cycles) was enough to move the world in and out of the ice ages. Even though humans have increased the CO2 concentration by 130 ppm already, this extra 130 ppm has a smaller effect than the 100 ppm that was added naturally before.

But let's zoom in on the part that we actually care about: the modern era.

Figure 3

After zooming in, the logarithm doesn't make such a big difference: it's not far from a straight line. 560ppm will probably take us well beyond the Paris target of 1.5°C, so the 280-560 range is key; we would be unwise to let our civilization go beyond 560.

But human CO2 emissions are increasing exponentially—fast enough that when we plot atmospheric CO2 with a logarithmic scale, it still curves up, even over the last 30 years:

Figure 4

Exponential growth appears as a straight line on a logarithmic chart; an upward curve means, in some sense, faster than exponential growth.1 So if human emissions keep increasing as they have, it makes perfect sense that global warming would speed up.

"But wait," I hear you think, "surely it won't increase exponentially forever?" You're right, of course, it won't, but it could continue for awhile, and in total there are four factors that could work together to speed up warming:

  1. Rapid economic development
  2. Past emissions
  3. Carbon sink saturation
  4. Committed warming

1. The developing world is developing fast.

The late Hans Rosling explains this very well in his talk, "How Not to be Ignorant about the World". Poverty is decreasing faster than ever—which, I would think, means more power plants being built than ever before. Right now, about 1600 of those new power plants will burn coal. And as long as most of the world has a standard of living well below China's, there is plenty of room for growth to continue and perhaps even accelerate.

2. Past emissions (CO2 is cumulative)

Once we add CO2 to the atmosphere, we face the law of conservation of matter: it won't go away unless something removes it.

This is related to another paradox you might have heard: methane produces a much stronger greenhouse effect than CO2, yet scientists are less worried about it. Why? For one thing, it has a much lower concentration in the atmosphere, but what's really important here is that it has a short lifetime of only about 12 years before it is destroyed in the methane cycle. That makes the methane problem much less serious, as we expect nature will clean up the mess when we eventually reduce our methane output.

Carbon dioxide doesn't go away so easily. Here's a graph from Joos et al. (2013) estimating how slowly a large "pulse" (sudden addition) of CO2 would leave the atmosphere:

Figure 5

The black line is an average of many other studies and models. At first, the ocean and land absorb it "quickly", so about half of it is gone after "only" 50 years, locked up in seawater and plants. But the next 25% takes a full 950 years to go away! After 1000 years, the ocean has absorbed 59% (contributing to ocean acidification) and the land 16%, leaving 25% behind.

CO2 accumulation itself can't make global warming speed up, but what it does is prevent it from stopping by ensuring that the greenhouse forcing keeps going up. If you look at a graph of human emissions instead of atmospheric concentration, it's only roughly exponential. Human emissions temporarily stalled in the early 80s and early 90s, but since CO2 accumulates, the atmospheric curve just kept going up unabated.

3. Carbon sinks can saturate

Right now, carbon sinks (oceans, plants, and others) are removing about 2.4ppm of CO2 from the atmosphere each year, while we're adding about 5.2ppm, for a net increase of 2.5ppm per year.2

Figure 6: Where our emissions go (source)

While nature removes about half of our carbon emissions each year now, don't assume our good fortune will last. According to Jones et. al., 2013, there is disagreement between various climate models about the details, but on average, under the business-as-usual scenario known as RCP 8.5, the land is projected to absorb less CO2 as time goes on, and the fraction of our emissions absorbed by oceans will decrease too (even if the absolute absorption rate increases). In other words, just because we emit more doesn't guarantee nature absorbs more; sooner or later, CO2 will accumulate faster in the atmosphere. (On average about 2/3 of new emissions will stay in the atmosphere this century under RCP 8.5, where last century it was less than half.)

Basically, the oceans can absorb CO2 at first; increasing the CO2 in the air will always make oceans absorb more. However, as the oceans warm up, carbon solubility decreases—warm water can't hold as much of it, and the only reason ocean absorption will continue after that is that oceans are enormous and take time to "fill up", as the carbon spreads deeper and deeper. Given enough time, oceans would "saturate" and become unable to absorb more. Similarly, CO2 enhances plant growth to some extent, but growth is eventually balanced out by plant decomposition (which releases CO2), and the long-term effects of climate change won't necessarily be good for plants.

CO2 will eventually be removed permanently through a process called weathering—but this will take thousands of years.

4. Committed warming

Earth's climate system has feedback loops that magnify the warming effect of CO2. For example, as the arctic ice melts, it exposes ocean. The ocean is much darker than the ice, so more sunlight is absorbed instead of being reflected back to space. This enhances the arctic warming effect. This effect is time-delayed, since it takes many years for the arctic ocean to warm up (which in turn causes the ice to melt more quickly in the future, which in turn helps the ocean to heat up even more.)

"Committed warming" refers to future warming effects that would still happen even if CO2 levels stop increasing. A large source of delayed warming worldwide is the oceans, which, as you can see here, have not kept up with the warming of the land:

Figure 7

As our massive oceans slowly heat up, they will not only increase the global average surface temperature, but they will also warm up the land further, especially near the ocean where ocean temperature strongly affects the land.3

Figure 8 based on IPCC AR4 5.2.2.3

Due to this delayed warming, climate scientists have separate short-term and long-term estimates of global warming:

Figure 9: Warming from various CO2 levels based on a typical TCR estimate of 1.8°C and the most commonly-cited estimate of ECS, 3°C. Various scientific groups have produced a range of TCR and ECS estimates; the precise concentration of CO2 that corresponds to 1.5°C is unknown (the bars marked "Paris target" are drawn wide to represent the uncertainty, but are not scientifically accurate error bars). And of course, this graph is just a first-order approximation. The real climate will be warmed further by other greenhouse gases, especially methane, and the real climate has additional variability and unpredictability, as do all computer models of it.

As you can see, in the short term there is technically still time to fulfill the Paris agreement and keep global warming under 1.5°C—but this graph ignores methane, which moves the target closer. Unfortunately it is considered highly unlikely that we'll be able to stop at our 1.5°C goal.

The long term outlook is even worse: we've already passed 1.5.

The good news is that reaching the long-term "equilibrium" climate will take hundreds of years, giving us time to, hopefully, reverse course and avoid a lot of that committed warming. But it's very likely—especially after we pass 1.5°C—that humanity will someday need to figure out how to remove CO2 from the atmosphere on a large scale.

In summary:

Although CO2 has less effect at higher CO2 concentrations, this "logarithmic effect" will be overpowered by these 4 factors if we don't switch to clean energy quickly:

  1. Exponential growth of energy use
  2. Past CO2 emissions that nature has not yet absorbed
  3. Carbon sink saturation
  4. Committed warming

What if we manage to stop increasing our emissions? This related article indicates that if emissions hold steady, global warming will still continue upward linearly.

Good news though: the price of solar panels has passed an important milestone. Around the equator where sunlight is strongest, unsubsidized solar power plants have dropped below the price of coal. Hooray for Swanson's law! I also like to point out that a new kind of safe and cheap nuclear reactor will—if the public supports it—begin production in the 2020s. And on a graph of human CO2 emissions you can see emissions have stalled. Is this temporary, like it was in the early 80s and 90s, or are we finally at a turning point? Perhaps, but the IEA forecast still includes new fossil fuel plants in the coming years.

Footnotes

1 This may sound more dramatic than it is; the human emission increase has been exponential, not faster than exponential, so the upward curvature is caused by something else. I believe it's because we're in a transition region between roughly constant CO2 of the past (280 ppm) and the new pattern of exponentially increasing CO2. Inside the transition region, an upward curve is expected.

2 Note: due to uncertainties, the numbers don't add up perfectly (2.4+2.5≠5.2). These numbers are based on the average of the last 5 years of Global Carbon Budget data, i.e. 9.8 GtC emitted by humans per year, 1.39 GtC added via land-use change, 2.5 GtC removed by oceans and 2.63 GtC removed by land. These numbers are estimates, and the observed change is 2.51 ppm (5.32 GtC) per year, which is 0.33 ppm (0.71 GtC) different than expected. Data sources and uncertainty levels are listed here. The conversion factor is 2.13 GtC/ppm.

3 There is some good news: climate models say the oceans will never warm up as much as the land does. See Sutton et al. 2007 for details.

P.S. Why does CO2 have a logarithmic effect? It's complicated; see Myhre et al. (2008) or  Huang & Shahabadi (2014) for technical details.



from Skeptical Science https://ift.tt/2Gi890H

Physicists show why it's hard to clog a drain with soft particles

Emory sophomore Mia Morrell conducted the experiments with hydrogel balls. "You can learn a lot from them because they provide a simple model for physics, kind of like fruit flies do for biology," she says.

By Carol Clark

For decades, scientists have studied how groups of solid objects — everything from falling grains of sand to a rushing crowd of panicked people — can get stuck as they try to pass through a small opening. The classic result is known as “faster is slower.” When the objects flow out, if an arch of the objects forms across the opening, then a large pressure can stabilize the arch and cause a clog.

Now scientists have shown that when the objects are squishy instead of solid, the reverse is true. The journal Physical Review E published the findings by physicists at Emory University, demonstrating that when soft particles feel a larger pressure, they squish together and the arch breaks, and so clogging is less likely.

“We’ve quantified the clogging dynamics of soft objects for the first time and identified the parameters that seem to explain why it’s completely opposite physics to that of hard objects,” says Emory physics professor Eric Weeks, whose lab conducted the research. “One surprising result is that, while friction is often suspected to be important for arch formation, our particles are frictionless and yet still form arches.”

Questions about how clogs form have implications for everything from improving highway design and the flow of traffic to avoiding jam-ups of people fleeing a burning building.

The dynamics of soft objects that the Weeks lab investigated could give insights into biological processes such as the flow of cells, bacteria and other “squishy” particles through blood vessels.

“It’s new physics and yet it’s so simple,” Weeks says. “We used tools such as a basic physics formula from 1882 and some cheap hydrogel balls that we ordered from Amazon.”

"Hydrogels have interesting properties and that makes them fun to work with," says Mia Morrell, a sophomore in the Weeks lab.

Weeks, who specializes in the study of soft condensed materials, became intrigued by the growing number of studies on how solid objects clog. It sounds counterintuitive — after a rush of solid particles through an opening forms an arch, greater pressure behind them solidifies that arch. But the process appears to work similarly to a keystone arch in architecture: The pressure from the weight of stones above presses the stones in the arch below more firmly together.

Weeks and his students decided to explore the process of soft-particle clogging. Graduate students Xia Hong and Meghan Kohne worked on experiments involving tiny oil droplets and then computer simulations.

Motivated by those preliminary results, Emory senior Haoran Wang (who graduated in 2017) conducted early experiments with the marble-sized, water-filled hydrogel balls. They are sometimes called plant balls since they are commonly used to hold up stems in flower vases. Wang built a two-dimensional, Plexiglas hopper that allowed gravity to pull the hydrogel balls down through two triangular wedges that could be adjusted in width to change the size of the opening between them.

Mia Morrell, a sophomore, continued the work when she joined the Weeks lab last year.

“I loved doing the hydrogel experiments because it’s really hands-on — not just sitting at a desk,” Morrell says, adding that the project also required her to learn how to become handy with a drill and a laser cutter.

The hydrogel balls start out as deflated polymer husks. They are left in a tray of water until they swell up into squishy, slippery, plastic spheres that feel almost like living tissue.

“Hydrogels have interesting properties and that makes them fun to work with,” Morrell says. “You can learn a lot from them because they provide a simple model for physics, kind of like fruit flies do for biology.”

Morrell loaded the hydrogels into the two-dimensional hopper. She tilted the hopper to vary the effects of gravity and checked to see if the particles would clog as they flowed through it. This process required her to reload the hopper more than 400 times to investigate different conditions.

The Hertzian force law, an 1882 formula by Heinrich Hertz, allowed the researchers to measure the displacement and compression force of individual hydrogel spheres and compare the hydrogel results with the oil droplet experiments and the computer simulations. The comparison showed that these different systems all have the same physical behavior, apparently universal to soft particles.

“We quantified the dynamics of soft particles in a two-dimensional environment under the influence of gravity and what happens when you present them with an obstacle,” Morrell says. “What we learned from this single system may have many broader applications.”

Related:
Physicists crack another piece of the glass puzzle
Crystal-liquid interface made visible for the first time

from eScienceCommons https://ift.tt/2pQhiT0
Emory sophomore Mia Morrell conducted the experiments with hydrogel balls. "You can learn a lot from them because they provide a simple model for physics, kind of like fruit flies do for biology," she says.

By Carol Clark

For decades, scientists have studied how groups of solid objects — everything from falling grains of sand to a rushing crowd of panicked people — can get stuck as they try to pass through a small opening. The classic result is known as “faster is slower.” When the objects flow out, if an arch of the objects forms across the opening, then a large pressure can stabilize the arch and cause a clog.

Now scientists have shown that when the objects are squishy instead of solid, the reverse is true. The journal Physical Review E published the findings by physicists at Emory University, demonstrating that when soft particles feel a larger pressure, they squish together and the arch breaks, and so clogging is less likely.

“We’ve quantified the clogging dynamics of soft objects for the first time and identified the parameters that seem to explain why it’s completely opposite physics to that of hard objects,” says Emory physics professor Eric Weeks, whose lab conducted the research. “One surprising result is that, while friction is often suspected to be important for arch formation, our particles are frictionless and yet still form arches.”

Questions about how clogs form have implications for everything from improving highway design and the flow of traffic to avoiding jam-ups of people fleeing a burning building.

The dynamics of soft objects that the Weeks lab investigated could give insights into biological processes such as the flow of cells, bacteria and other “squishy” particles through blood vessels.

“It’s new physics and yet it’s so simple,” Weeks says. “We used tools such as a basic physics formula from 1882 and some cheap hydrogel balls that we ordered from Amazon.”

"Hydrogels have interesting properties and that makes them fun to work with," says Mia Morrell, a sophomore in the Weeks lab.

Weeks, who specializes in the study of soft condensed materials, became intrigued by the growing number of studies on how solid objects clog. It sounds counterintuitive — after a rush of solid particles through an opening forms an arch, greater pressure behind them solidifies that arch. But the process appears to work similarly to a keystone arch in architecture: The pressure from the weight of stones above presses the stones in the arch below more firmly together.

Weeks and his students decided to explore the process of soft-particle clogging. Graduate students Xia Hong and Meghan Kohne worked on experiments involving tiny oil droplets and then computer simulations.

Motivated by those preliminary results, Emory senior Haoran Wang (who graduated in 2017) conducted early experiments with the marble-sized, water-filled hydrogel balls. They are sometimes called plant balls since they are commonly used to hold up stems in flower vases. Wang built a two-dimensional, Plexiglas hopper that allowed gravity to pull the hydrogel balls down through two triangular wedges that could be adjusted in width to change the size of the opening between them.

Mia Morrell, a sophomore, continued the work when she joined the Weeks lab last year.

“I loved doing the hydrogel experiments because it’s really hands-on — not just sitting at a desk,” Morrell says, adding that the project also required her to learn how to become handy with a drill and a laser cutter.

The hydrogel balls start out as deflated polymer husks. They are left in a tray of water until they swell up into squishy, slippery, plastic spheres that feel almost like living tissue.

“Hydrogels have interesting properties and that makes them fun to work with,” Morrell says. “You can learn a lot from them because they provide a simple model for physics, kind of like fruit flies do for biology.”

Morrell loaded the hydrogels into the two-dimensional hopper. She tilted the hopper to vary the effects of gravity and checked to see if the particles would clog as they flowed through it. This process required her to reload the hopper more than 400 times to investigate different conditions.

The Hertzian force law, an 1882 formula by Heinrich Hertz, allowed the researchers to measure the displacement and compression force of individual hydrogel spheres and compare the hydrogel results with the oil droplet experiments and the computer simulations. The comparison showed that these different systems all have the same physical behavior, apparently universal to soft particles.

“We quantified the dynamics of soft particles in a two-dimensional environment under the influence of gravity and what happens when you present them with an obstacle,” Morrell says. “What we learned from this single system may have many broader applications.”

Related:
Physicists crack another piece of the glass puzzle
Crystal-liquid interface made visible for the first time

from eScienceCommons https://ift.tt/2pQhiT0