Population and Migration

Population

The world faces many complex population and migration dynamics over the next 50 years. The world population is estimated to grow by 1.2% annually, reaching over nine billion by 2050, according to the United Nations. The planet will soon experience the largest generation of youth in human history. Yet in some parts of the world, population growth rates are declining, with some countries experiencing negative growth rates.Zero population growth is not good for us. Many societies are ageing, and in some nations, the increasing proportion of elderly in the population is placing pressure on existing public sector pension systems and social welfare programs. These dynamics pose challenges for governments. International migration may help to mitigate the effects of population ageing in some countries but cannot completely compensate for it.

We should not endorse population “stabilization” or “control.” The “ideal” family size should be determined by the desires of couples, not governments. All decisions on children’s number, spacing, and timing should be made without coercion.

Migration

There are more than 175 million migrants in the world today. People leave their countries for many reasons, including war and civil conflict, the desire for economic improvement, family reunification and environmental degradation.

The United States supports safe, orderly and legal migration. Our policy on international migration should focus on the human rights of migrants, protection for asylum-seekers, opposition to uncontrolled and illegal migration, support for anti-trafficking efforts, and encouragement of the rapid integration of legal immigrants.

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Posted in Discussions, Human Geography, opinions, Population | 3 Comments

New Book on Global Warming

If you don’t think climate change produces winners as well as losers, consider this: In the 12th and 13th centuries England exported wine to France. Vineyards also flourished in improbable regions like southern Norway and eastern Prussia. A centuries-long spell of mild, predictable weather blessed Western Europe with abundant crops, healthy populations and budget surpluses sufficient to finance projects like Chartres Cathedral.

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Lesley Newhart

Brian Fagan

THE GREAT WARMING

Climate Change and the Rise and Fall of Civilizations

By Brian Fagan

Illustrated. Bloomsbury Press. 282 pages. $26.95.

William P. O’Donnell/The New York Times

 

This is the credit side of a global balance sheet carefully itemized by Brian Fagan in “The Great Warming,” his fascinating account of shifting climatic conditions and their consequences from about A.D. 800 to 1300, often referred to as the Medieval Warm Period. The debit side is appalling: widespread drought, catastrophic rainfall, toppled dynasties, ruined civilizations. Abandoned Maya temples in the Yucatan and the desolation of Angkor Wat, supreme achievement of the Khmer empire, bear witness to climatic change against which royal power and priestly magic proved impotent.

Mr. Fagan, an anthropologist who has written on climate change in “The Long Summer” and “The Little Ice Age,” proceeds methodically, working his way across the globe and reading the evidence provided by tree rings, deep-sea cores, coral samples, computer weather models and satellite photos. The picture that emerges remains blurry — scientists still understand little about such weather-changers as El Niño and La Niña — but it has sharpened considerably over the past 40 years, enough for Mr. Fagan to present a coherent account of profound changes in human societies from the American Southwest to the Huang He River basin in China.

Longer summers and milder winters in Europe, especially stable from 1100 to 1300, allowed Norse explorers to range as far as Greenland and Labrador. At the same time a population boom in the rest of Europe led to radical deforestation, as trees were cleared to create farmland. By the end of the Medieval Warm Period half the forests that covered four-fifths of Western and Central Europe in A.D. 500 had disappeared.

Across vast swaths of the globe, however, severe, persistent droughts lasted not just for years but for generations. The Sierras of modern-day California experienced the severest droughts of the past 4,000 to 7,000 years. Acorn trees died, and along with them peoples largely dependent on acorns for food. Although data remain sketchy, it seems probable that extended droughts dried up pastureland on the Central Asian steppe, propelling the armies of Genghis Khan westward.

In the southern Yucatan arid conditions proved too much for the elaborate reservoirs, called “water mountains,” that the Maya used to irrigate their fields. Mr. Fagan permits himself an ominous aside: “The analogies to modern-day California, with its aqueducts for water-hungry Los Angeles, or to cities such as Tucson, Ariz., with its shrinking aquifers and falling water table, are irresistible.”

Mr. Fagan is as interested in human adaptation as he is in weather. While California’s acorn eaters suffered, peoples in the Southwestern deserts expanded their diet to include new edible plants. In the Sahara caravan organizers simply adjusted their routes according to changing rainfall patterns.

“The camel and its load-carrying saddle proved an effective weapon against heat and drought even in the worst years, when extreme aridity affected cattle people living far south of the desert,” Mr. Fagan writes.

Northern China got the worst of both worlds during the Medieval Warm Period: violent climatic swings that resulted in lengthy dry spells or torrential rainfall. Meanwhile, in the South Pacific, faltering trade winds allowed Polynesian voyagers to head east, eventually reaching Rapa Nui (Easter Island) around 1200.

Mr. Fagan has a somewhat rigid, formulaic way of presenting his material. Well aware that the general reader can handle only limited amounts of ice-core data, he tries to generate period atmosphere by including present-tense “you are there” episodes. “The hushed crowd in the plaza gazes upward to the temple at the summit of the pyramid,” one section begins. A little drama certainly helps, but he overworks this device. The book is overpopulated with sweating plowmen and fishermen peering into the mist.

The causes of the Medieval Warm Period remain unclear, and there is debate over what the actual temperatures were. Mr. Fagan draws one unambiguous conclusion from the evidence, however, in a final chapter on the present-day implications of the great warming of a thousand years ago. Drought is the great enemy, “the silent and insidious killer associated with global warming,” he writes.

Population density has placed enormous pressure on increasingly scarce water resources. As a result modern droughts, brought on by El Niño events, have taken an enormous toll in lives and wreaked measureless economic devastation. Prepare for worse.

“Judging from the arid cycles of a thousand years ago, the droughts of a warmer future will become more prolonged and harsher,” Mr. Fagan writes. “Even without greenhouse gases, the effects of prolonged droughts would be far more catastrophic today than they were even a century ago.”

For a spark of hope Mr. Fagan offers the example of Chimor, a kingdom in coastal Peru tormented by El Niño flooding and severe droughts throughout the Medieval Warm Period. The Chimu people thrived nonetheless by diversifying their food supply and protecting their scarce water resources. In a historically arid region with uncertain food supplies, they successfully tapped their centuries of experience with irrigation, soil conservation and water management. Look no further for a global-warming role model.

source:http://www.nytimes.com

Posted in books, Global Warming | 1 Comment

White Dwarfs

Where do White Dwarfs Come From?

Where a star ends up at the end of its life depends on the mass it was born with. Stars that have a lot of mass may end their lives as black holes or neutron stars. A low and medium mass star (with mass less than about 8 times the mass of our Sun) will become a white dwarf. A typical white dwarf is about as massive as the Sun, yet only slightly bigger than the Earth. This makes white dwarfs one of the densest forms of matter, surpassed only by neutron stars.

Black Hole Neutron Star White Dwarf
Black Hole Neutron Star White Dwarf

Medium mass stars, like our Sun, live by fusing the hydrogen within their cores into helium. This is what our Sun is doing now. The heat the Sun generates by its nuclear fusion of hydrogen into helium creates an outward pressure. In another 5 billion years, the Sun will have used up all the hydrogen in its core.

This situation in a star is similar to a pressure cooker. Heating something in a sealed container causes a build up in pressure. The same thing happens in the Sun. Although the Sun may not strictly be a sealed container, gravity causes it to act like one, pulling the star inward, while the pressure created by the hot gas in the core pushes to get out. The balance between pressure and gravity is very delicate.

When the Sun runs out of hydrogen to fuse, the balance tips in the favor of gravity, and the star starts to collapse. But compacting a star causes it to heat up again and it is able fuse what little hydrogen remains in a shell wrapped around its core.

image of Betelgeuse

January 15, 1996,
Hubble Space Telescope
Captures First Direct Image
of a Star, A. Dupree (CfA)
and NASA.
This burning shell of hydrogen expands the outer layers of the star. When this happens, our Sun will become a red giant; it will be so big that Mercury will be completely swallowed! When a star gets bigger, its heat spreads out making its overall temperature cooler. But the core temperature of our red giant Sun increase until it’s finally hot enough to fuse the helium created from hydrogen fusion. Eventually, it will transform the helium into carbon and other heavier elements. The Sun will only spend one billion years as a red giant, as opposed to the nearly 10 billion it spent busily burning hydrogen.

We already know that medium mass stars, like our Sun, become red giants. But what happens after that? Our red giant Sun is still eating up helium and cranking out carbon. But when it’s finished its helium, it isn’t quite hot enough to be able to burn the carbon it created. What now?

Since our Sun isn’t hot enough to ignite the carbon it its core, it succumbs to gravity again. When the core of the star contracts, it causes a release of energy that makes the envelope of the star expand. Now the star has become an even bigger giant than before! Our Sun’s radius has become larger than Earth’s orbit!

The Sun is not very stable at this point and loses mass. This continues until the star finally blows its outer layers off. The core of the star, however, remains intact, and becomses the white dwarf. The white dwarf is surrounded by an expanding shell of gas in an object known as planetary nebula. They are called this because early observers thought they looked like the planets Uranus and Neptune. There are some planetary nebulae that can be viewed through a backyard telescope. In about half of them, the central white dwarf can be seen using a moderate sized telescope.

image of N2610 image of N6543

Planetary nebulae seem to mark the transition of a medium mass star from red giant to white dwarf. Stars that are comparable in mass to our Sun will become white dwarfs within 75,000 years of blowing their envelopes. Eventually they, like our Sun, will cool down, radiating heat into space, fading into black lumps of carbon. It may take 10 billion years, but our Sun will reach the end of the line and quietly become a black dwarf. White dwarfs can tell us about the age of the universe. If we can estimate the time it takes for a white dwarf to cool into a black dwarf, that would give us a lower limit on the age of the universe and our galaxy. But because it takes billions of years for white dwarfs to cool, we don’t think the universe is old enough yet for many, if any, white dwarfs to have become black dwarfs. Finding black dwarfs would certainly alter our understanding of the cooling process in white dwarfs.

Observations of White Dwarfs

There are several ways to observe white dwarf stars. The first white dwarf to be discovered was found because it is a companion star to Sirius, a bright star in the constellation Canis Major. In 1844, astronomer Friedrich Bessel noticed that Sirius had a slight back and forth motion, as if it was orbiting an unseen object. In 1863, the optician and telescope maker Alvan Clark spotted this mysterious object. This star was later determined to be a white dwarf. This pair are now referred to as Sirius A and B, B, being the white dwarf. The orbital period of this system is about 50 years. Since white dwarfs are very small and thus very hard to detect, binary systems are a helpful way to locate them. As with the Sirius system, if a star seems to have some sort of unexplained motion, we may find that the single star is really a multiple system. Upon close inspection we may find that it has a white dwarf companion. image of Sirius B
The arrow is pointing to white dwarf, Sirius B.

The Hubble Space Telescope, with its 2.4 meter mirror and advanced optics, has been successfully viewing white dwarfs with its Wide Field and Planetary Camera. In August of 1995, this camera observed more than 75 white dwarfs in the globular cluster M4 in the constellation Scorpius. These white dwarfs were so faint that the brightest of them was no more luminous than a 100 watt light bulb seen at the moon’s distance. M4 is located 7,000 light years away, but is the nearest globular cluster to Earth. It is also approximately 14 billion years old, which is why so many of its stars are near the end of their lives.

HST image of white dwarfs in M4
Optical Image (left) and a portion of the Hubble Space Telescope observation (right) of the globular cluster M4. The white dwarfs are circled in the HST image.
Optical telescopes are not the only way to view white dwarfs. The white dwarf HZ 43 was observed by the X-ray satellite ROSAT. X-rays come from inside the visible surface of the white dwarf. This region is very dense and can be as hot as 100,000 degrees in a very young white dwarf. A white dwarf’s outer layers contain just helium and hydrogen, and so are essentially transparent to the X-rays that are emitted by the much hotter inner layers. ROSAT image of HZ 43

source:http://imagine.gsfc.nasa.gov

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Neutron Stars

ROSAT HRI image of Puppis A

Neutron stars are compact objects that are created in the cores of massive stars during supernova explosions. The core of the star collapses, and crushes together every proton with a corresponding electron turning each electron-proton pair into a neutron. The neutrons, however, can often stop the collapse and remain as a neutron star.

Neutron stars are fascinating objects because they are the most dense objects known. They are only about 10 miles in diameter, yet they are more massive than the Sun. One sugar cube of neutron star material weighs about 100 million tons, which is about as much as a mountain.

Like their less massive counterparts, white dwarfs, the heavier a neutron star gets the smaller it gets. Imagine if a 10 pound bag of flour was smaller than a 5 pound bag!

Neutron stars can be observed occasionally, as with Puppis A above, as an extremely small and hot star within a supernova remnant. However, they are more likely to be seen when they are a pulsar or part of an X-ray binary.

source:http://imagine.gsfc.nasa.gov

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