The ‘Methusaleh’ Star

This Digitized Sky Survey image shows the oldest star with a well-determined age in our galaxy. Called the Methuselah star, HD 140283 is 190.1 light-years away. Astronomers refined the star’s age to about 14.3 billion years (which is older than the universe), plus or minus 800 million years. Image released March 7, 2013. (Image: © Digitized Sky Survey (DSS), STScI/AURA, Palomar/Caltech, and UKSTU/AAO)

If the universe is 13.8 billion years old, how can a star be more than 14 billion years old?

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I wonder if the touch-and-go operations change the trajectory of the asteroids such that it might have missed us but it’s now kind of pushed into a collision course with earth? Probably not but it’s interesting to think about. Or terrifying. Whichever you prefer.

The World Needs Nuclear Power, And We Shouldn’t Be Afraid Of It

By: Ethan Seigel, Starts With A Bang

The uncomfortable truth is this: we are a space-age civilization that has chosen to eschew technological advances in energy generation because of fear and inertia. We are powering the 21st century with 18th century technology, which has had disastrous effects on our environment that we have ignored for far too long. While there are many possible ways forward to address this problem, nuclear power has the proven track record of success necessary and the flexibility to be an integral, and potentially the primary, resource in humanity’s arsenal in the fight against climate change.

For many years, we have let fear, rather than facts, control the narrative over nuclear power. While the conventional story around nuclear power focuses on the few disasters that have occurred, nuclear’s track record tells a different story: one of unparalleled safety, successful waste management, and abundant, affordable, green energy. The world needs nuclear power now more than ever. If we can overcome our entrenched biases against it, we just might solve one of the biggest problems facing our world for generations to come.

– Ethan Seigel

Not in my backyard. NIMBY. That’s what they always say: nuclear is great, clean, and safe, but not for me. Well, it’s time to get over that prejudice. It’s time to embrace the technologies we have to solve the problems that we’re incredibly delinquent in addressing responsibly.

We didn’t make the decisions that caused climate change, global warming, and ocean acidification. But we sure can make the decisions to fix them.

The Lives, Times, And Deaths Of Stars

Who among us doesn’t covertly read tabloid headlines when we pass by them? OK, you don’t. But the rest of us, yeah we probably do. But if you’re really looking for a dramatic story, instead of looking to Hollywood, turn you face to the sky and check out the real stars (do not look directly into the sun). From birth to death, the burning spheres of gas that light the night sky and the one that powers our daytime lives experience the most extreme conditions our cosmos has to offer.

All stars are born in clouds of dust and gas like the Pillars of Creation in the Eagle nebula (pictured below). In these stellar nurseries, clumps of gas form, pulling in more and more mass as time passes. As they grow, these clumps start to spin and heat up. Once they get heavy and hot enough (somewhere in the realm of 27 million degrees Fahrenheit or 15 million degrees Celsius), nuclear fusion starts in their cores. This process occurs when protons, the nuclei of hydrogen atoms, squish together to form helium nuclei. This releases a LOT of energy, which heats the star and pushes against the force of gravity. And with this violent reaction, a star is born.

Credit: NASA, ESA and the Hubble Heritage Team (STScl/AURA)

From that point on, a stars lifecycle depends on how much mass they have. Scientists typically divide stars into three categories: low-mass, high-mass and the lesser used intermediate-mass. We’ll discuss the first two for simplicity’s sake.

Low-mass Stars: These stars have a mass about eight times that of our Sun’s or less and can burn steadily for billions of years. As it reaches the end of its life, its core runs out of hydrogen to convert into helium. Because the energy produced by fusion is the only force fighting gravity’s tendency to pull matter together, the core begins to collapse. But squeezing the core also increases its temperature and pressure, so much so that its helium starts to fuse into carbon, which also releases energy. The core rebounds a little, but the star’s atmosphere expands a lot. This eventually causes the star to turn into a red giant star and destroy any nearby planets. Our sun will also go through this process but it’s a few billion years away so we don’t have to worry about it just yet.

Red giants are unstable and begin pulsating, periodically inflating and ejecting some of their atmospheres. Eventually, all of the star’s out layers blow away, creating an expanding cloud of dust and gas misleadingly called a planetary nebula (there are no planets involved save for the ones that were orbiting the star and were already destroyed).

Credit: NASA, ESA and the Hubble Heritage Team (STScl/AURA)

All that’s left of the star is its core, now called a white dwarf. This star is a roughly Earth-sized stellar cinder that gradually cools over billions of years. If you could scoop up a teaspoon of its material, it would weigh more than a pickup truck. (Scientists recently found a potential planet closely orbiting a white dwarf. It somehow managed to survive the star’s chaotic, destructive history!)

High-mass Stars: These stars have a mass eight times the sun’s or more and may only live for millions of years. (Rigel, a blue super-giant in the constellation Orion, pictured below, is eighteen times the Sun’s mass.)

Credit: Rogelio Bernal Andreo

A high-mass star starts out doing the same things as a low-mass star, but it doesn’t stop at fusing helium into carbon. When the core runs out of helium in a high-mass star, it shrinks, heats up and starts converting its carbon into neon, which releases energy. Later, the core fuses the neon it produced into oxygen. Then, as the neon runs out, it fuses the oxygen into silicon. Finally, the silicon is fused into iron. All of these processes produce energy that keeps the core from collapsing, but each new fuel buys it less and less time. By the point silicon fuses into iron, the star runs out of fuel in a matter of days. The next step would be fusing iron into some heavier element, but doing so requires energy instead of releasing it.

The stars iron core collapses until forces between the nuclei push the brakes, and then it rebounds back to its original size. This change creates a shock way that travels through the star’s outer layers. The result is a huge explosion called a supernova.

What’s left behind depends on the star’s initial mass. Remember, a high-mass star is any star with a mass more than eight times that of our sun. That’s a HUGE range! A star on the lower end of this spectrum leaves behind a city-sized, super-dense neutron star. (Some of these weird objects can spin faster than blender blades and have powerful magnetic fields. A teaspoon of their material would weigh as much as a mountain!!)

At even higher masses, the star’s core turns into a black hole, one of the most bizarre cosmic objects out there. Black holes have such strong gravity that light can’t escape them. If you tried to get a teaspoon of material to weigh, you wouldn’t get it back once you crossed the event horizon — unless it could travel faster than the speed of light and we don’t know of anything that can!

The explosion also leaves behind a cloud of debris called a supernova remnant. These and planetary nebulae from low-mass stars are the sources of many of the elements we find on Earth. Their dust and gas will eventually one day become a part of other stars starting the whole process over again. So the next time you feel incredibly lost or alone, remember that we’re all connected by the star stuff we’re made from!

That’s a very brief summary of the lives, times and deaths of stars.

Article Credit: NASA Universe