Black Holes

General aspect of searching black holes and understanding of the subject.
For
ages people have been determined to explicate on everything. Our search for
explanation rests only when there is a lack of questions. Our skies hold
infinite quandaries, so the quest for answers will, as a result, also be
infinite. Since its inception, Astronomy as a science speculated heavily upon
discovery, and only came to concrete conclusions later with closer inspection.

Aspects of the skies which at one time seemed like reasonable explanations are
now laughed at as egotistical ventures. Time has shown that as better
instrumentation was developed, more accurate understanding was attained. Now it
seems, as we advance on scientific frontiers, the new quest of the heavens is to
find and explain the phenomenom known as a black hole. The goal of this paper is
to explain how the concept of a black hole came about, and give some insight on
how black holes are formed and might be tracked down in our more technologically
advanced future. Gaining an understanding of a black hole allows for a greater
understanding of the concept of spacetime and maybe give us a grasp of both
science fiction and science fact. Hopefully, all the clarification will come by
the close of this essay. A black hole is probably one of the most misunderstood
ideas among people outside of the astronomical and physical communities. Before
an understanding of how it is formed can take place, a bit of an introduction to
stars is necessary. This will shed light (no pun intended) on the black hole
philosophy. A star is an enormous fire ball, fueled by a nuclear reaction at its
core which produces massive amounts of heat and pressure. It is formed when two
or more enormous gaseous clouds come together which forms the core, and as an
aftereffect the conversion, due to that impact, of huge amounts of energy from
the two clouds. The clouds come together with a great enough force, that a
nuclear reaction ensues. This type of energy is created by fusion wherein the
atoms are forced together to form a new one. In turn, heat in excess of millions
of degrees farenheit are produced. This activity goes on for eons until the
point at which the nuclear fuel is exhausted. Here is where things get
interesting. For the entire life of the star, the nuclear reaction at its core
produced an enormous outward force. Interestingly enough, an exactly equal
force, namely gravity, was pushing inward toward the center. The equilibrium of
the two forces allowed the star to maintain its shape and not break away nor
collapse. Eventually, the fuel for the star runs out, and it this point, the
outward force is overpowered by the gravitational force, and the object caves in
on itself. This is a gigantic implosion. Depending on the original and final
mass of the star, several things might occur. A usual result of such an
implosion is a star known as a white dwarf. This star has been pressed together
to form a much more massive object. It is said that a teaspoon of matter off a
white dwarf would weigh 2-4 tons. Upon the first discovery of a white dwarf, a
debate arose as to how far a star can collapse. And in the 1920ís two leading
astrophysicists, Subrahmanyan Chandrasekgar and Sir Arthur Eddington came up
with different conclusions. Chandrasekhar looked at the relations of mass to
radius of the star, and concluded an upper limit beyond which collapse would
result in something called a neutron star. This limit of 1.4 solar masses was an
accurate measurement and in 1983, the Nobel committee recognized his work and
awarded him their prize in Physics. The white dwarf is massive, but not as
massive as the next order of imploded star known as a neutron star. Often as the
nuclear fuel is burned out, the star will begin to shed its matter in an
explosion called a supernovae. When this occurs the star loses an enormous
amount of mass, but that which is left behind, if greater than 1.4 solar masses,
is a densely packed ball of neutrons. This star is so much more massive that a
teaspoon of itís matter would weigh somewhere in the area of 5 million tons in
earthís gravity. The magnitude of such a dense body is unimaginable. But even
a neutron star isnít the extreme when it comes to a starís collapse. That
brings us to the focus of this paper. It is felt, that when a star is massive
enough, any