Black Hole Research Paper

On the other end of the spectrum, the death of a super-massive star is one of the most brilliant displays of pure power in the universe which includes an amazing light show which has no equal. A super-massive star is exactly what it sounds like, a star so big that it dwarfs our own star in every way. When a super-massive sun begins to run out of out of hydrogen it begins to collapse, but due to its immense gravity and size, the collapse produces such an abrupt implosion that the last remnants of nuclear fusion remaining push all the mass of the star back out into space (Britt, 2007). This can be compared to someone jumping onto a trampoline whose elastic has enough elasticity to force one back into the air. This occurrence is known as a supernova explosion, which is the largest explosion in the known universe. A supernova explosion can even be seen from other galaxies, as scientists have done witnessed from observations using the Hubble telescope. The star is so big, however, that it only blows its outer atmosphere away, still leaving a massive amount of matter that is doomed to collapse again, and this time it will be a one-way ticket to oblivion. The super-massive star finally collapses and its own incredible mass crushes it’s internally and now turns it into a neutron star. An average neutron star is about ten miles in diameter, or the size of Manhattan. Although this

What happens to a star during the rest of its life depends of how massive

Type II supernovaes, which are more common, occurs when a star runs out of nuclear fuel and collapses under its own gravity. In a Type II supernovae, once the star’s core surpasses a certain mass (The Chandrasekhar limit) the star begins to impolode. The core then heats up and becomes denser. Eventually the implosion bounces back off the core, expelling the stellar material into space. What’s left is a neutron star.

Although the basic formation process is understood, one perennial mystery in the science of black holes is that they appear to exist on two radically different size scales. On the one end, there are the countless black holes that are the remnants of massive stars. Peppered throughout the Universe, these "stellar mass" black holes are generally 10 to 24 times as massive as the Sun. Astronomers spot them when another star draws near enough for some of the matter surrounding it to be snared by the black hole 's gravity, churning out x-rays in the process. Most stellar black holes, however, lead isolated lives and are impossible to detect. Judging from the number of stars large enough to produce such black holes, however, scientists estimate that there are as many as ten million to a billion such black holes in the Milky

Once the helium in the core is exhausted, the star emits its outer layers into space, contracts down, and emerges as a White Dwarf. Ultimately, the White Dwarf will lose all of its energy, collapse due to gravity, and enter a Black Dwarf stage. No Black Dwarfs have been observed in our universe because the time it takes for a White Dwarf to cool completely is likely to be trillions of years. A Black Dwarf is simply an explanation for what would result following the death of a White Dwarf.

Type I supernova: star accumulates matter from a nearby neighbour until a runaway nuclear reaction ignites.

Common types of black holes are produced by certain dying stars. A star with a mass greater than 20 times the mass of our sun can produce a black hole at the end of its life. Black holes are usually only created by the death of a very massive star. When a very massive star dies, it explodes into a supernova. The outer parts of the star are launched violently into space while the core completely collapses under its own weight. If the core remaining after the giant explosion from the supernova is very massive, there

A black hole is a region of spacetime and it has strong gravitational that affects nothing. Nothing can escape from inside it such as particles nor light radiation. General relativity predicts that a compact mass can deform spacetime to form a black hole. The point of no escape is called the event horizon. The event horizon has an enormous affect on the fate and circumference of an object crossing it. Black holes reflect no light. When it meets a star it consumes it and turns into a colorful circle that you can see.

The American scientist John Wheeler coined the phrase “black hole” in 1969 to describe a massively compact star with such a strong gravitational field that light cannot escape. When a star’s central reserve of hydrogen is depleted, the star begins to die. Gravity causes the center to contract to higher and higher temperatures, while the outer regions swell up, and the star becomes a red giant. The star then evolves into a white dwarf, where most of its matter is compressed into a sphere roughly the size of Earth. Some stars continue to evolve, and their centers contract to even higher densities and temperatures until their nuclear reserves are exhausted and only their gravitational energy remain. The core then rushes

Like our sun, it will eventually run out of hydrogen and helium fuel at the star’s core. However, it will have enough mass and pressure to fuse carbon (S2). Next, over time, heavier elements build up at the center and it becomes layered like an onion (S2). The elements will become lighter and move towards the outside of the star. The core will heat up and become dense. The core will become extremely heavy; so heavy that its gravitational force will not be able withstand it; causing it to explode. The explosion spews out stellar material throughout space

Black holes are born from the aftermath of a supernova. But supernovas can also turn into neutron stars if there is not enough mass to make a black hole because a neutron star just does not have the amount of matter to make a black hole it still has an extremely high gravitational pull and magnetic field. A black hole has such a high gravitational pull that light can not even escape. The reason for a black hole’s extremely high gravitational pull is that it has a great extent of mass packed into a tiny space that it makes a super gravitational pull (Dunbar, Brian). So because of the super high gravity black holes are extremely dangerous and hard to examine.

Stars are born in a very complicated way. First the gravitational collapse of a cool, dense molecular cloud sends fragments into space. The fragments then contract and form stellar cores. The stellar cores then rotate and condense as they increase in temperature, to the point that a nuclear reaction occurs. The new born star burns hydrogen into helium for 90 percent of its life and is a sequence star. A star’s mass changes as it burns more hydrogen.Once there is no more hydrogen for the star to burn off of, energy generation will stop and the core will start contracting. As the internal temperature increases a shell of hydrogen gets ignited. The star begins to expand enormously and increases in luminosity. The star expands so large that if our star started to expand like this it would swallow Mercury and

In simple terms, a black hole is a visually undetectable region of space that exerts a gravitational force so powerful that not even light can escape [Wald 1984, pp. 299–300], thus exhibiting the characteristics of an ideal black body in the sense that it absorbs all the radiation that falls on it [Schutz, Bernard F. (2003). Gravity from the ground up. Cambridge University Press. p. 110]. In addition, all black holes are enveloped by spherical “boundaries” known as “event horizons”, which defines a point from beyond which it is impossible to escape once it is crossed.

It will eject its own beautiful nebula and then fade away as a white dwarf star”. Eventually these low-mass bodies will burn through their hydrogen and will grow dimmer and cooler and eventually the lights will go out.

Main sequence stars like our own sun enduring in a state of nuclear fusion during which they will produce energy for billions of years by replacing hydrogen to helium. Stars change over billions of years. When their main sequence phase ends they pass through other states of existence according to their size and other characteristics. The larger a star's mass, the shorter its lifespan is. As stars move toward the end of their lives, much of their hydrogen will be converted to helium. Helium sinks to the star's core and raises the star's temperature—causing its outer shell to expand. These large, puffy stars are known as Red Giants. The red giant phase is actually a prelude to a star shedding its outer layers and becoming a small, dense body called a White Dwarf. White dwarfs cool down for billions and billions of years, until they finally go dark and produce no energy at all. Once this happens, scientists have yet to observe, such stars become known as Black Dwarfs. A few stars avoid this evolutionary path and instead go out with a bang, exploding as Supernovae. These violent explosions leave behind a small core that will then turn into something called a Neutron Star or even, if the remainder is large enough, it is then turned into something called a Black Hole.