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The Hungry Star That Can’t Stop Snacking!

When a small star like our Sun begins to use up its necessary supply of hydrogen fuel, it first swells to obscene proportions and becomes known as a. Red Giant stars. This bloated, red-colored remnant of a small star balloon as bright as the Sun is so large that – if it were surrounded by the inner planets and sad – it would engulf them through its expansion, burning the outer layer of gas. warm, and consume them. In June 2014, a team of astronomers announced at the summer meeting of the American Astronomical Society, held in Boston, Massachusetts, that they had discovered a star. Red Giant star that is about to eat with not only one, but rOAcursed planet!

The two sad worlds, named Kepler-56b SY Kepler-56c is destined to be swallowed up by his greedy parent’s star in the “short” – by cosmic standards, that is. Both planets will disappear in about 130 million and 155 million years.

“As far as we know, this is the first time that two known exoplanets in a single system predict a ‘time of death,'” said Dr. Gongjie Li, the leader of the investigation, in the newspaper on June 2, 2014. Dr. Li the Harvard-Smithsonian Center for Astrophysics (CfA) in Cambridge, Massachusetts.

He presented his study at a press conference during the 224th meeting of the AAS.

The hungry star Kepler-56 is in the process of morphing into a bloated, greedy person Red Giant. It is already very swollen, and is now more than four times the size of our Sun. As it grows, it will continue to expand outwards. Not only will the red star get bigger, but its waves will also be stronger, leading its planet to its tragic end.

Even before their stars collapse, these two planets will experience intense heat from their expanding parent stars. Their atmospheres, if any, will begin to boil – and these poor planets will become egg-shaped by powerful radio waves.

the Kepler-56 The system is much more than a sad example of what happens at the end of a small star main sequence (burning hydrogen) “life”. It also provides a disturbing glimpse into the future of our own solar system. In about five billion years our Sun will also swell into a rage Red Giantblowing itself to a terrible size, covered first Mercury, then Venus – and then, perhaps, the Earth.

Sun On Steroids

Our solar system arose from the debris left over from the ancient, long-dead nuclear cores of previous generations of stars. Our Sun appeared in a very cold pocket, hidden in a vast, dark molecular cloud. Such a cold cloud haunts the vast, barred Milky Way Galaxy, and is like the strange cradle of its burning baby stars. Eventually, dense pockets of stars, embedded in dark molecular clouds – mostly gas, but also small amounts of dust – will collapse under their own gravity to give birth to bright new stars. . In the depths of such a large, cold, dark cloud, the thin and fragile threads gradually coalesce, and coalesce into a lump that grows over thousands of years. Then, that’s it happens – suddenly the dense pocket is compressed enough, due to the collapse of gravity, that the hydrogen atoms floating inside begin to fuse together. This ignites the fire of the little star, and the star will continue to burn as long as the star is “alive”!

All 400 billion stars in the Galaxy, including our Sun, were born this way – by the collapse of heavy pockets embedded in cold, dark molecular clouds. These dark clouds are scattered across the Milky Way, carrying gas and dust from long-gone ancient stars that have long since died.

Our Sun is old, main sequence, a simple little star. It was born about 4.56 billion years ago, and it looks like a big golden blob, shining in daylight. There are eight large planets, many moons and moons, and a variety of small objects – both rocks and ice – around our Star, which resides in the far reaches of a typical, albeit majestic, large Galaxy.

However, in another 5 billion years – or more – our Sun will be gone Red Giant! A star of the low mass of our Sun “lives for 10 billion years on the planet main sequence. However, at this time, the Sun and stars like it – which live in the middle active period – are still moving and moving well enough to go about the burning of hydrogen in the furnace of stars. nuclear fusion. Nuclear fusion gradually produce heavier atomic particles from lighter ones, in a process called stellar nucleosynthesis.

When our Sun and other stars like it finally burn through their necessary supply of hydrogen fuel, their shape changes. They are now former stars. At the heart of an older Sun-like star, there is a hidden core of helium. The helium heart is surrounded by a shell where the hydrogen is still fusing into helium. At this point, the shell begins to expand outwards, and the core continues to expand, as the star expands more and more. Eventually, the helium core itself begins to collapse under the weight of its own weight, and it gets hotter and hotter until eventually, it becomes hot enough in the center to start a new phase of nuclear fusion. In this new process, helium combines to form the heavier atomic element, carbon. In another five billion years, our doomed Star will have a small, very hot core that will emit more energy than it does now. Our Sun’s outer gas layer will be red and swollen, and it will no longer be the beautiful, glowing golden ball we see lighting up the daytime sky. The fiery red, bloated and aged Sun will transform into a Red Giant, with a terrible desire that will make him make snacks for his children in the planet. The temperature of this burning gas would be slightly cooler than it is in space today. This explains the can be said a cool red color–as opposed to a brighter, warmer yellow.

When our Sun goes away Red Giant it will still be warm enough to convert the cold people in the distance Kuiper belt–like a dwarf planet Pluto and its icy plants – to a tropical paradise. But this humid tropical shelter will not last forever. The core of our aging, dying sun will continue to shrink as it no longer emits radiation as a result of the process of nuclear fusion–and will reach the end of this long starry path, because all further evolution will be determined by gravity alone. Eventually, our Sun will throw its outer layers of gas into interstellar space – but the core will remain the same, and all of the Sun’s material will collapse into this tiny object. it is a residue that is the same size as the size. Land. Our Sun has undergone a sea change, and in its death will become a type of star corpse known as a white dwarf. This strange, dense relic, the fiery, burning Star, will be surrounded by a beautiful shell of colorful gas, which used to be the outer layer – called a planet nebula. nebula planets, which is around white dwarf, They got their strange names because ancient astronomers thought they resembled the planets Uranus and Neptune.

Right now, our planet is sitting pretty – even close to the inner edge of our star. residential area, where water can exist in its current state, and therefore life can develop. the residential area will spread even more when our star is very bright. Even now, it is relentless, slow, ever increasing, deadly bright. In about 2 billion years, if humans had managed to survive, the remnants of our species would have had to flee our planet before the Star could escape us. Mars will be the first choice for transit – for a while, anyway. However, about 3 billion years later, the rest of humanity will have to migrate again, because the Sun will also eat that planet. The previously frigid moons of the outer planets may be a safe haven for now – but, by now, whatever remains of our species knew better than to travel to the interstellar space to find exoplanet homes. Our Sun will shed its outer layers, and transform into a white dwarf with a strong gravitational pull. But before our Star enters that beautiful night, the outer layers will become covered with a bright, glowing gas – a planet nebulasometimes called “the butterfly of the cosmos”.

The Star Who Can’t Eat With Just One

Alas, both Kepler-56b SY Kepler-56c is closer to its killer parent star than Mercury is to our Sun. Kepler-56b It orbits its star once every 10.5 days Kepler-56c rotates every 21.4 days. These two doomed planets, therefore, will meet their fate sooner than Mercury about 5 billion years from now. Dr. Li and his team calculated the evolution of the star’s size (using the publicly available MESA code) and the planet’s orbit to predict when the planets will evaporate.

The only survivor of the old planetary system Kepler-56d, which is a gas giant planet in a 3.3 Earth year orbit around its star. It will surely be far away, if the worlds of its two sisters become history.

the Kepler-56 The planetary system is also famous for being the first “tilted” system of multi-planet sports discovered. From the equator of the parent star we can see the orbits of the inner planet siblings. This was very surprising, because the planets were born from a disc of gas and dust of the same size (protoplanetary accretion disk) as stars, they should therefore be in the same plane as the star’s equator – like the planets in our own solar system.

The team was able to better determine the tilt of these planets, compared to previous studies. Astronomers have found that the maximum tilt is 37 or 131 degrees.

Dr. Li and his team also looked at the inclination of the outer, luckier planets and determined that their orbits may also be tilted toward their stars. Future observations should help astronomers identify this interesting structure, and ultimately explain how it came to be tilted.

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