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The Supernova Next Door

A wild and dazzling supernova explosion heralds the explosive, violent death of a star, and these starfires can shine so brightly that they can even outshine their entire host galaxy—at least for a time. On January 21, 2014, an exceptionally nearby stellar explosion became the brilliant object of pursuit for astronomers around the world—as well as several NASA spacecraft. Explosion, dab SN 2014J dazzled the galaxy M82, located “only” 12 million light-years away from our planet. SN 2014J is the closest optical supernova to light up the sky in twenty years — and is potentially the closest Type Ia supernova to flare up in the lifetime of today’s missions, astronomers said — providing a rare opportunity to study such cosmic phenomena.

SN 2014J is the brightest supernova to be seen from our planet since the giant starburst that erupted in 1987 – just 168,000 light-years away. In fact, the supernova of January 2014 was so dazzling that it was brilliant enough to be spotted by a small telescope looking at the dark, cloud-shrouded sky hovering over North London. On January 21, 2014, Dr. Steve Fossey, an astronomer at University College London, takes a group of 21 students through a routine lesson with the 35cm telescope at the University of London’s City Observatory. When he showed his students images of the galaxy M82, also known as A galaxy of cigars because of its shape, they spotted something strange—a bright star nestled at the very edge of the galaxy’s disk. M82 hangs just above the bowl Ursa Major (The Big Dipper) constellation and has long been a favorite target of deep-sky astronomers.

The brilliant star that Dr. Fossey and his students saw in the image taken during the 10-minute follow-up that she appeared to be a newcomer. Dr. Fossey did not recall ever seeing him, and he was not present in the images he and his students searched for on the Internet. “It seemed kind of weird,” said Dr. Fossey on January 23, 2014 Scientific American.

According to students who noticed SN 2014Jthe exciting discovery was a wonderful surprise.

“One minute we’re eating pizza, then five minutes later we helped discover a supernova. I couldn’t believe it. It reminds me why I got interested in astronomy in the first place,” student Tom Wright said in a January 2014 press release.

Another student, Ben Cooke, also noted in a January 2014 press release that “the chance of finding something new in the sky is astronomical, but this was especially stunning because it was one of the first images we took with this telescope.”

Something new in the sky

All stars, large and small, “live through” all their hydrogen burning, main sequence it “lives” by maintaining a very critical and fragile balance between two constantly opposing forces –gravitation and radiation pressure. The radiation pressure developed by the star pushes everything external and away from the star, and keeps this huge, seething, dazzling ball of turbulent gas bouncing against the squeeze gravitation, who mercilessly and tirelessly tries to tear everything down internal. The radiation pressure stars on main sequence results from the process nuclear fusion, which begins by burning hydrogen, the lightest and most abundant atomic element in the universe, into helium – the second lightest atomic element. This process, stellar nucleosynthesis, it is constantly combining heavier atomic elements from lighter ones. In fact, all atomic elements heavier than helium (called metals astronomers), were created in searing heat nuclear fusion the heart of the billions and billions and billions of star-dwellers in our vast cosmic wonderland—or else in the spectacular supernova explosions heralding the end of that long interstellar journey.

Most supernovae ignite when a lone star exhausts its necessary supply of hydrogen fuel and explodes into pieces, meeting its fiery final demise. The progenitor of a supernova is often a massive star with an extremely heavy core that tips the scale to about 1.4 solar masses (so-called Chandrasekhar limit). Smaller, less richly endowed members of the stellar community, such as our own Sun, do not normally die in the incredible brilliance and violence of a supernova fire like their more massive stellar relatives. Small stars like our own fade away with relative calm and incredible beauty. Our Sun is currently a common garden variety and is rather small main sequence Star. Surrounding our Sun, happily situated on the far outskirts of the majestic, great barred spiral galaxy, our Milky Way, are eight major planets, a host of beautiful moons, and a host of other smaller objects—a beautiful, starlit wheel spinning in space . Our Sun, like all stars, will not live forever. Like all stars, it is doomed to run out of hydrogen fuel at some point. Stars with a relatively small mass of our Sun can “live out”. main sequence it lives for about 10 billion years, happily fusing the hydrogen stores in its core into heavier stuff.

However, our Sun is not exactly a spring chicken. In fact, it is a middle-aged Star. It’s not old, but it’s not young either. However, it is enjoying a happy and productive middle age and is still tenacious enough to continue merrily fusing hydrogen in its hot heart for another 5 billion years or so – unfortunately, it has already lived for about 4.56 billion years!

When small stars like ours finally manage to fuse together most of their supply of nutritious hydrogen fuel, they swell into glowing, bloated red giant stars. An older Sun-like star at this point carries a worn-out heart of helium, surrounded by a shell that still has some lingering hydrogen that is fusing into helium. The shell expands outward, and the aging heart of the star gradually grows larger and larger as the doomed star ages and ages. Next, the helium heart itself begins to shrink under its own weight—while heating up, until it eventually becomes so extremely hot at its center that the helium begins to fuse into an even heavier one. atomic element – carbon. A tiny Sun-like star squirms with a tiny, burning heart that produces more energy than it did once, long, long ago, when it was alive young main sequence star. The outer gaseous layers of the doomed old star swelled and turned red. Tragically, in our own solar system, when our Sun finally became bloated, old, red giantit will ferociously cannibalize some of its own planetary offspring – first Mercury, then Venus, and then (perhaps) our Earth. The temperature on the fiery surface of this hideous, hungry red giant it will be significantly cooler than when our Sun was still a bright, young, life-sustaining star!

The death of small stars like our Sun is relatively gentle, characterized by a “soft” blowing of their outer gaseous layers of glowing, multi-colored gases into interstellar space. These objects are so magically beautiful that astronomers who are mesmerized by this spectacle often refer to them as the “butterflies of the cosmos”.

This is how our Sun will perish – with great beauty and in relative peace. But that’s because our Sun is a lonely star. She has no companion star around to disrupt her hermetic happiness. The corpse Sun will be a dense, small stellar relic called a white dwarfand his shroud will be glittering, glittering, a “butterfly” with flying wings of many colors.

However, something quite different happens when a Sun-like star has another star as its companion – rudely disturbing its peaceful solitude. This can cause very explosive things. Small stars usually do not carry enough mass to go supernova. However, this kind of explosion can happen if there are two star relics white dwarfs collide and merge or if a recluse white dwarf she lives in close contact with her sister-star companion – and victim. An unlucky companion star can be either a main sequence star or swollen red giant In both cases, white dwarf, with a vampiric hunger, slurps material from the star’s companion—and gulps as much as he can until he can finally drink no more. The white dwarf “goes critical” just like the big boys and blasts into oblivion in a supernova called a Type Ia.

Supernova next door

Astronomers think so SN 2014J is a member Type Ia class and that it can help explain how these supernovae develop. Type Ia supernovae are “standard candles”—that is, astronomers use them as cosmic measuring sticks to help them determine the increasing expansion of the universe.

Observations from SN 2014J spectroscopy revealed its status as a Type Ia. This type of supernova brightens quickly. Although many such supernovae are observed each year, they are usually much further away than these Cigar galaxy.

Astronomers around the world will now be watching closely to see exactly how SN 2014J brightens. They used the brightness consistency of the Type Ia supernovae in the past to very precise distance measurements. In fact, these cosmic “standard candles” were instrumental in the discovery dark energy in the 1990s. Dark energy is a mysterious force, a property of space itself, that causes the expansion of the universe to accelerate.

The Cigar The close proximity of the galaxy means that there are many existing images of it from earlier times SN 2014J exploded, including some that were derived from Hubble Space Telescope. Astronomers will carefully study these images to look for what existed in the region before the star exploded. The Cigar the galaxy is heavily shrouded in dust – the light from the supernova shines on the dust in such a way that it can also teach astronomers something about the galaxy. One team of astronomers there is currently searching for radioactive elements such as nickel, which some theories predict form Type Ia supernovae.

One of the first telescopes to look at SN 2014J was in NASA orbit Quick observatory that took an image of the supernova and its host galaxy with its Ultraviolet/optical telescope.

“Finding and publishing new supernova discoveries is often the weak link in getting fast observations, but once we know about it, we can observe a new object within hours,” said Dr. Neil Gehrels press January 27, 2014. Dr. Gehrels is a Quick observatory principal investigator at NASA Goddard Space Flight Center.

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