Grb Discovery

”GX 339-4, illustrated here, is among the most dynamic binaries in the sky, with four major outbursts in the past seven years. In the system, an evolved star no more massive than the sun orbits a black hole estimated at 10 solar masses. “ [5]

The star has been losing fuel and is burning out, so the star will begin to collapse. When collapsing part of the star will shoot into space and scientist believe this is how a supermassive black hole forms. When the hole is forming, dust and gas is collected from the galaxy surrounding the black hole. Light cannot be released because matter is squeezed together in a small space. Stellar black holes are small but dense and can have 20 times more mass than the sun. Mass is the property of a physical body. When a black hole is forming it is possible for mass to be pulled from stars around the whole. This will help the hole grow in power and

The amazing amount of radiation coming from the disk of gas is ripping the galaxy apart.

Elizabeth Gibney discusses the history of fast radio bursts and astronomer’s strategy to finding them in the universe in her article, “Fast Radio Bursts are Astronomy’s Next Big Thing.” She begins by defining fast radio bursts as “fleeting blasts of energetic cosmic radiation of unknown cause.” (Gibney) Gibney briefly reviles that even though FBRs were discovered a decade ago, the phenomenon has just recently been accepted as genuine.

​The definition of a black hole according to Sea and Sky is “The collapsed core of a massive star. Stars that are very massive will collapse under their own gravity when their fuel is exhausted. The collapse continues until all matter is crushed out of existence into what is known as a singularity. The gravitational pull is so strong that not even light can escape.” Seasky.org, cited 2016: “Black hole”. Glossary of Astronomy. [Available online at http://www.seasky.org/astronomy/astronomy-glossary.html#B]. Black holes are not visible to the human eye. Since they are so dense, light is not able to escape them resulting in them being invisible. Special tools are required for them to be discovered and located with telescopes. This is done by seeing how stars close to them act different from others.

What is left after the huge explosion is another dwarf star, a neutron star, or the fierce black hole. A neutron star is about the size of a city like Los Angeles, but has the mass of about two suns. This means it is incredibly dense and has an unbelievable gravitational pull, almost 2 billion times that on earth. In fact, this pull is so strong that it bends radiation and allows astronomers to see the back of the star. They also spin up to 48 thousand times per minute due to the energy from the supernova.

It is the brightest astronomical radio source in the sky. It was discovered in 1947 and is the strongest radio source outside the solar system. Its explosion ejected cloud material that is 10 light years across and is expanding at a rate of 4,000-6,000 km/s. Its temperature s about 50 million degrees F. The first light of this supernova reached us about 300 years ago! Coordinates: RA 23h 23m 26.7s | Dec +58° 49' 03.00"

A stellar black hole is formed when a gianormous star collapses upon itself. When a stellar black hole forms, a supernova, or an exploding star is created as well. This supernova releases that rest of the exploding star into space. As a result a stellar black hole is created. Once a stellar black hole is created, they can be up to 20 times bigger than the

“We decided to see if the pulsations of these stars could be detected even if we couldn’t separate their light from the sea of unchanging stars that are their neighbors.”

Stellar Black Holes: It is consisted when the middle of a very massive star collapses on itself. This collapse also causes a supernova that explode a part of the star into space. (Mathew,2012)

Neutron stars are a sight to witness on their own and we are fascinated by them in every way imaginable, including everything else in space, however, there is one sight that we have never seen before that includes such a star and, that being a neutron star merger. A merger being the collision of two stars, in this case two neutron stars, that create a black hole as well as an innumerable amount of energy however, scientists have determined that the amount of energy the merger exhibited was some 200 millions times that of our Sun but, in the form of gravitational waves. This collision had only just reached our small Earth a few days but, collided a few billion years ago some 130 million light years away from planet Earth. We managed to pick

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

The galactic cosmic-ray (GCR) intensity is modulated by long-term effects such as ≈ 11-year solar-activity cycle and ≈ 22 year solar magnetic cycle as well as by short-term effects such as passage of corotating flows (high-speed streams) and transient disturbances (e.g. interplanetary coronal mass ejections). Recurrent depressions in GCR intensity due to corotating fields and flows and Forbush decreases due to transient disturbances have been studied in the past (see, e.g. Lockwood, 1971; Rao, 1972; Iucci et al., 1989; Venkatesan and Badruddin, 1990; Cane, 2000; Kudela et al., 2000; Gupta and Badruddin, 2009; Oh and Yi, 2009; Kane, 2010; Wawrzynczak and Alania, 2010; Abbrescia et al., 2011; Modzelewska and Alania, 2012; Sabbah and Kudela, 2011, and references therein).

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.

In the Blandford-Znajek process the black hole essentially acts as a massive conductor rotating with a high spin in a massive magnetic field created by the accretion disk. An induced voltage exists at the poles of the black hole and its equator, resulting in the disspiation of power by the deceleration of the rotation of the black hole; the resulting in power generated equals to