Neutron Stars : A Neutron Star

In this paper I will explain how astronomers determine the composition, temperature, speed, and rotation rate of distant objects using various methods. I will explain the properties of stars. I will also summarize the complete lifecycle of the Sun and determine where the Sun is currently in its lifecycle.

Orion has two of the brightest stars, be Betelgeuse and Rigel. Betelgeuse is a red supergiant. The gravity of the star squeezes its core tightly, heating it to billions of degrees. It then fuses the helium to make heavier elements. When that happens, the star no longer produces energy in the core. Without the reactions in its core to push outward, gravity quickly causes the core to collapse, forming a neutron star.

TOPIC SENTENCE NEEDED. These stars are the mass of the sun squished down to the size of a city. They meausure 20 kilometer or 12.5 miles across. One sugar cube of a Neutron star weighs about 1 trillion or 1 billions tons. There is another type of neutron star called a magnetar. The magnetic field of a neutron star is trillions times stronger than the magnetic field. A magnetars magnetic field is 1000 times stronger. Their known to erupt with no warning.

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.

In 1974, Joseph Taylor and Russell Hulse found such a pair of neutron stars in our own galaxy.[cite] One of the stars is a pulsar, meaning it beams regular pulses of radio waves toward Earth. Taylor

Soon Mason felt he was ready, so he exploded! After Mason exploded into a supernova, his mass compressed him into a neutron star. Mason then lived a long and happy life as a neutron star, until one day. On one eventful day, a neighboring neutron star, named HeavenLea got a little too close to Mason and they started spinning very fast, pulled together by gravity. Until eventually, Mason and HeavenLea crashed, creating even more heat and pressure than a normal supernova! This crash resulted in some of the strongest elements like

There are many different stars that exist in our galaxy but all of them fail in comparison to Wolf-Rayet stars. Discovered in 1867 by two astronomers, Charles Wolf, and Georges Rayet, they are the largest and brightest classification of stars currently observed today. Using a Foucault telescope, Wolf and Rayet were able to see a distinct spectrum of light that had never been observed before and thus Wolf-Rayet stars were born. Also called WR stars, there are characteristics that make these stars distinct from any other in the galaxy. One of the most well known Wolf-Rayet Stars is WR-104. It has distinct pinwheel shape and is referred to by some astronomers as a real life “death star”. The reason for this designation comes from the idea that

Sir Herschel was studying double stars for the purpose of understanding the motion of stars and to find the means of their parallax shifts. When looking at one of the stars, he noted that this one moved completely different than the others, in fact it was moving faster, telling him that it was much closer to our planet than any other star out there. By accident, he observed a star to be which he thought as a comet.

This article talks about how a star explodes. When a star explodes, it either completely blows up or it leaves a black hole behind. Some stars explode with titanic explosions called Supernovae. Supernovae are put into two categories, Type I and Type II. A well known Type I is called Type Ia. Type Ia is when a white dwarf star blown up. One theory as to why this happens is called stellar cannibalism. This is when a white dwarf star has a star that is near it, it might steal gas from the star. Type II supernovae however, are most likely born in galaxy spiral arms. Type II supernova's brightness usually stays bright for up to two months. Then it goes down over the next few months. I would definitely like to read more about the explosion of stars,

With a very basic telescope he could see dark spots on the sun and the movement of these spots, with these observation, he could confirmed that the sun revolved on its own axis.

The central part (the 'core') of the star undergoing 'supernova' explosion, collapses into a neutron star of mass in the range of 1.1 – 2 solar masses. During the collapse, atoms of the progenitor stars break, and subatomic particles become free and then positively charged protons convert to charge neutral neutrons (in addition to already existing neutrons) by adsorbing negatively charged electrons. Neutron stars are very dense objects. Their density can be as high as 1014 gm per cubic centimetre. They are also highly magnetised, their magnetic fields are usually in the range of 108 to 1016 Gauss (the strength of refrigerator magnets is around 50 Gauss). Neutron stars also spin very fast, rotating up to a few hundred times in a

Supernovas are the explosion of a star when it reaches the end of its life. There are two ways a star can go supernova. The first way or a Type I supernova occurs in the Binary system which is when two stars orbit the same point. The two stars are a white dwarf and a red giant. A white dwarf is a small dense star that is around the size of a planet and a red giant is a star at its last stages of life. If these two stars are close enough, matter will be transferred to the white dwarf from the red giant. When the star’s core reaches its limit of matter, a thermonuclear detonation will occur leaving nothing behind unless there were leftover elements in the white dwarf or there were elements made in the supernova explosion. One of the elements made in the explosion is radioactive nickel.

For a source that was many light years always as Scorpios was, to have the amount of x-ray emissions that was detected implied that it must have been generating huge quantities of x-rays. The simplest explanation for this was if material was heated to extreme temperatures as it was being accelerated by gravity onto a nearby object. If this would be true then the companion object had to be very small and very dense. The next pivotal discovery come with the launch of the Unuru x-ray satellite on December 12th 1970. Its given job was to map the x-ray sky; the satellite found 339 sources. Some where galaxies, some supernova remnants, but most were x-ray binary stars. Here, ordinary stars stream their material onto nearby neutron stars which gets extremely hot as it falls, therefore emitting x-rays. One of these sources however known as Cygnus X1 did not fall into this category. Neutron stars are formed from the collapse of stars less than 3 times the mass of the Sun. From the uhuru satellite the data, it shows that the companion to this star appeared to be live to be 5 to 8 times the mass of the Sun, this object was too large to be a neutron

Planets have mass and therefore have an effect on their stars orbit causing it to wobble. The wobble in the case of a pulsar star is seen as the periodic delay in the arrival of the pulses from the pulsar star (Wolszczan 1994). Due to the nature of a Pulsar star we can detect perturbations in its orbit through its pulses but to detect perturbations in other stars orbits, astronomers use a stars radial velocity.

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.