Theories on the Destruction of Earth

SUN:
SUPERNOVA
NASA/Gates
Version
Supernova for Dummies Version
Conclusion
NASA/Gates version:

As the mass
of the star's iron core approaches 1.4 solar masses (due to
continued silicon and sulfur burning in a thin shell adjacent to
the iron core), a dramatic sequence of events is being triggered:
Gravity, which up to now was balanced by the outward force of the
pressure, decisively gains the upper hand and .In less than a
second, the core collapses from a size of about 5,000 miles to
one of about a dozen miles, and an enormous amount of energy is
released. This collapse happens so fast that the star's outer
layers have no time to react and participate in it. What is
released during core collapse is truly gigantic. It is equivalent
to the energy produced by 100 stars like the Sun, during their
entire lifetimes of more than 10 billion years! Most of the
energy released during the collapse of the iron core is carried
off into space by elusive particles. A small fraction of the
energy is deposited into the lower layers of the envelope
surrounding the core and triggers the supernova
explosion.
The energy deposited in the lower layers of the envelope creates
a super strong shock wave that runs outward through the envelope
toward the star's surface. As the shock wave runs outward, it
heats the envelope, induces explosive nuclear burning, and ejects
the envelope at speeds of thousands of miles per second (i.e., in
excess of 10 million miles/hour). It is during this phase that
elements heavier than iron are being manufactured. When the shock
wave reaches the star's surface, it very quickly heats the
surface layers and brightens them. Within a day or two the
exploding star becomes brighter than a billion Suns. This is the
moment when distant observers first learn that a supernova is
exploding (unless they have been lucky enough to detect some of
the neutrinos that were emitted earlier during core collapse). A
star appears where, as viewed over the great distances of
interstellar or intergalactic space, none was seen before --
hence, the term nova, which means "new." The result of these
events is a compact stellar remnant and a rapidly expanding
gaseous shell. The stellar remnant is a neutron star or a black
hole. The expanding gaseous shell plows into the surrounding
interstellar medium, and pushes, compresses, and intermingles
with it. Such regions of the interstellar medium are known
as After some weeks, the brightness of the explosion
diminishes, although the supernova may remain visible for many
months or years, even across intergalactic distances. About 20 to
30 supernovae are discovered each year in galaxies beyond the
Milky Way. Most are too faint to be seen without a telescope due
to their great distances.

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Supernova for Dummies
version:
Scientists
say that a star's lifetime is around 10 billion years old, and
right now the Sun is about 5 billion years old, so it should be
(you can do the statistical math). When the Sun goes supernova,
be ready to say bye bye to mommy.
After 10 billion years is up the Sun will start to expand and
swell up like a fat man at an all you can eat bar. As it
increases in size, it will devour Mercury, Venus and com a little
too close to home. As the temperature increases we will be
toasted beings, actually dead ones. The crust of the sun would
remain rather cool than normal, only about 3,000 kelvin. Its
normal temperature is about 6,000 kelvin. Within a quick time the
star's core collapses and then explodes, leaving a black hole,
matter and some heat from the sun being blown out into
space. The explosion can be seen from many galaxies away due to
the bright light it emits. Strong gravitational pulling occurs as
the black hole sucks everything into oblivion. Now on your merry
little journey to oblivion, planets, comets and mass objects may
collide creating catastrophes within a catastrophe.

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Conclusion:
In conclusion, a supernova will come and there is nothing we can
do about it but experience the massive pain it will inflict.
Whenever it comes GOD HELP US ALL.
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