Our sun is one of perhaps 400 billion stars in the Milky Way Galaxy. It is one of the 3% which are classified as a ‘G Class’ star.

Our sun began as a diffuse cloudof gas drifting in space. The gas,mostly hydrogen with lesser amounts of helium, contained all the atoms and molecules needed to build our solar system. The gas’ drift was not random, but rather was a movement guided by gravity within the cloud leading to a condensation of the gas.

The diffuse cloud of gas condensed from gravitational pull forming into a layers. The outer most layers were the halo. The inner most formed the corona.

As the gases continued to condense, they formed into a sphere of highly condensed gas.

The gases within the solar sphere became so dense they turned from their gaseous state into solid.

The hydrogen became so dense from its combined gravitation that it begins forcingthe Hydrogen atomsinto themselves.This forcing initiatesnuclear fusion,with the atomic interiors merging, and the electron exteriors being emitted as charged ion particles.

When the hydrogen began fusing, it began an unbroken seriesof nuclear fusion reactions converting hydrogen into helium; and other light atomic elements into heavier elements.

At this point, the Sun was born.

In this computer model,an accretion disk rotatesaround its central star.

Beyond the solar sphere, out on the planetary disk, the same condensation occurred. However, the quantity of hydrogen is such that it does not condense into a fusible mass. Instead, heavier elements predominate, condensing to form orbiting objects.

At the same time, all around the sphere, the gases flattened into a disk of continuously merging particles called an proto-planetary disk. This condensation process is called accretion.

The accretion process continued, merging the particles into ever larger planetesimals, and the planetesimals into orbiting asteroids, comets and even planets, as we know them today.

Solar flares erupting on the suncan shoot distances which are many times greater than the diameter of the sun.

At the center, the sun’s nuclear reactions are extremely violent, releasing microwaves and spewing solar flares of ionized particles.

The nuclear reactions raging on the sun throw out vast clouds of ionized matter and cosmic waves. These blast across the solar system in a plasma form called solar winds. Especially intense bursts are called solar flares.

From where we sit, the sun appears rather calm and stable.

But, up close, the violence of thesolar inferno becomes more visible.

On the sun’s surface, uncontained chains of nuclear fusion reactions rage continuously, projecting dense atomic particles in the form of plasma called solar Spicules.

As solar spicules merge, they explodeinto solar flares, blasting out millionsof miles away from the sun.

As the flares and solar winds explode across the solar system, they bombard all the asteroids, planetessimals and planets, including earth, with ionized nuclear debri.

The ionized debri rains down onto the earth’s magnetic fieldand is channeled along the earth’s magnetic field to thenorth and south poles.

High concentrationsof particles rain inon the Arctic and theAnarctic.

As the particlesrain down, theycreate the phenomenacalled the Aurora Borealis.

Aurora BorealisAs seen from a Polar geosynchronousSatellite.

In a close orbit of the Earth, the Aurora Borealis looks likethis…

From the Earth’s surface, theAurora Borealis looks like this…

From the Earth’s surface, the released energy in theatmosphere appears aslight, which arrays to observers as long curtains

Besides ionized atomic debri, the sun’s nuclear reactions emit microwaves across a wide spectrum; from short wave ultra violet rays, to longer infrared rays. These are absorbed by gases in the earth’s atmosphere and distributed as heat, generating climate and weather.

NASA photo shows infrared raysas most intense in the equatorial

region.

Eventually, the fusion reaction begins to use up the lighter elements. As the fusion slows, it is replaced by fission reactions; the breaking down of heavy atoms into inert ones.With all the lighter atoms converted into heavier elements,the fission reactions will dominate. This will cause the sun’s diameter to swell, and its color to go from yellow to red.

As the heavier elements are broken down into inert atoms, unable to react, they migrate to the star’s center to form a solid core. At a critical point, the last of the fissionable materials will erupt into a spectacular explosion called a nova.

Stars reach a critical pointin the content of theirfissionable materials andignite into novae.

Novae are so violent they stripplanets of their atmospheres,leaving them as barren burned cinders.

Novae blow through the orbitsof their solar systems.

The gases, and nuclear debrifrom the nova will spread outamong other diffuse gases emitted from other novae, blending with the gas background of the galaxy, forminglarge intra galactic clouds. From these nebulae, new stars will be born.

Fusion = H2HeCHeavy elementsFission= Heavy Elements Fe (Iron, which is inert to nuclear reaction)

The new stars containgreater amounts of Heavier, non-hydrogenatomic elementsthan the previous stars.The later generation stars,bearing more of the heavyatomic elements, burn Much longer, are morelikely to produce planets,and are more likely to contain the elements forplanetary biospheres.