A Star is Born and Enlightenment

Sayedena Muhammad Najm Thagib The Piercing Star {s}
said follow anyone of my Sahabi They are Like Stars.

Awliya when they reach Enlightment all creation will see that light as
a Star.


What is a Star?


The basic difference between a star and a planet is that a star emits
light produced in its interior by fusion reactions (nuclear
`burning'), whereas a planet only shines by reflected light.

The Sun { Qalb Level of the Heart } is our own special star yet, as
stars go, it is a very average star.

There are stars far brighter, fainter, hotter and cooler than the Sun.
Basically, however, all the stars we can see in the sky are objects
similar to the Sun.

The Sun (and any other star) is a great ball of gas held together by
its own gravity. The force of gravity is continually trying to force
the Sun towards its centre and if there were not some other force
counteracting it the Sun would collapse.


The necessary outward pressure is produced by the radiation from the
nuclear energy generation in the Sun's interior.

How do stars originate?

Stars form from concentrations in huge interstellar gas clouds. {amma}

These contract due to their own gravitational pull. As the cloud gets
smaller it loses some of the energy stored in it as potential
gravitational energy.


This is turned into heat which in the early days of the embryo star
can easily escape and so the gas cloud stays cool.


As the cloud's density rises it gets more and more difficult for the
heat to get out and so the centre gets hot.
If the cloud is big enough the temperature rise is sufficient for
nuclear reactions to take place.
This generates more heat and the `burning' of hydrogen into helium
takes place, as in the Sun.

The object is then a star.
a Wali is Born

Qalb/Sun

The Early Evolution of a Star

In its early stages the embryo star is still surrounded by the remains
of the original gas cloud, from which it formed.


By this stage the cloud remnant takes the form of a disk around the
star.

The radiation from the star gradually dissipates this disk, possibly
leaving behind a system of smaller objects, planets.

The Main-Sequence
The star now settles down to a long period of stability while the
hydrogen at its centre is converted into helium with the release of an
enormous amount of energy.

This stage is called the main-sequence stage, a reference to the
classical color-magnitude or

Most stars lie in a well defined band in the diagram and the only
parameter that determines where in the band they lie is the star's
mass.

The more massive a star is the quicker it `burns' up its hydrogen and
hence the brighter, bigger and hotter it is.

The rapid conversion of hydrogen into helium also means that the
hydrogen gets used up sooner for the more massive stars than for the
smaller ones.


Stars do not all evolve in the same way. Once again it is the star's
mass that determines how they change.

MEDIUM MASS STARS: Stars similar in mass to the Sun `burn' hydrogen
into helium in their centres during the main-sequence phase but
eventually there is no hydrogen left in the centre to provide the
necessary radiation pressure to balance gravity.

The centre of the star thus contracts until it is hot enough for
helium to be converted into carbon.

The hydrogen in a shell continues to `burn' into helium but the outer
layers of the star have to expand.


RED GIANT [ Red LEvel of the Heart}
This makes the star appear brighter and cooler and it becomes a red
giant.  { Sir secret }

During the red giant phase a star often loses a lot of its outer
layers which are blown away by the radiation coming from below.

Eventually, in the more massive stars of the group the carbon may be
`burnt' to even heavier elements but eventually the energy generation
will fizzle out and the star will collapse to what is called a
`degenerate white dwarf'.

White- Level of the Heart Secret of Secrets
Sir Sir White


SMALL MASS STARS: Our knowledge of the evolution of these stars is
purely theoretical because their main sequence stage lasts longer than
the present age of the Universe, so none of the stars in this mass
range has evolved this far!

We believe that the evolution will proceed as for the medium mass
stars except that the temperature in the interior will never rise high
enough for helium `burning' to start.


The hydrogen will continue to `burn' in a shell but will eventually be
all used up. The star will then just get cooler and cooler ending up
after about 1,000,000,000,000 years as a `black dwarf'.  The Khafa

HIGH MASS STARS: There are very few stars with masses greater than
five times the mass of the Sun but their evolution ends in a very
spectacular fashion. As was said above, these stars go through their
evolutionary stages very quickly compared to the Sun.



Like medium mass stars, they `burn' all the hydrogen at their centres
and continue with a hydrogen `burning' shell and central helium
`burning'.

They become brighter and cooler on the outside and are called red
supergiants.



Carbon `burning' can develop at the star's centre and a complex set of
element `burning' shells can develop towards the end of the star's
life.



During this stage many different chemical elements will be produced in
the star and the central temperature will approach 100,000,000 degrees
Kelvin.

For all the elements up to iron the addition of more nucleons to the
nucleus produces energy and so yields a small contribution to the
balance inside the star between gravity and radiation.



To add more nucleons to the iron nucleus requires energy and so once
the centre of the star consists of iron no more energy can be
extracted.

{{ Beginning of the State of Fana or Annihilation }}]

The star's core then has no resistance to the force of gravity and
once it starts to contract a very rapid collapse will take place.

The protons and electrons combine to give a core composed of neutrons
and a vast amount of gravitational energy is released.

This energy is sufficient to blow away all the outer parts of the star
in a violent explosion and the star becomes a supernova.

{ Khafa Secrets of Qiyama Zilzalahh Quaking of Mass}

The light of this one star is then as bright as that from all the
other 100,000,000,000 stars in the galaxy.

{{Going to the Ahkfa the Black Holes.}}}

During this explosive phase all the elements with atomic weights
greater than iron are formed and, together with the rest of the outer
regions of the star are blown out into interstellar space.

The central core of neutrons is left as a neutron star which could be
a pulsar.

What is remarkable about this is that the first stars were composed
almost entirely of hydrogen and helium and there were no oxygen,
nitrogen, iron, or any of the other elements that are necessary for
life.

These were all produced inside massive stars and were all spread
throughout space by such supernovae events. We are made up of material
that has been processed at least once, and probably several times,
inside stars.
Binding energy

The basic building blocks of atoms are protons neutrons and electrons.
Protons and neutrons can be split into quarks but this takes place at
energies higher than are found in stars.

The binding energy of atomic nuclei plotted against the atomic number
of the nuclei. Energy is released by the fusion of light elements into
heavier elements (elements on the left) or the fission of heavy
elements into lighter elements (elements on the right).

Iron is the highest element on the graph, and the most stable. It
cannot release energy through either fusion or fission.

Protons carry a positive charge and reside with neutrons in the
nucleus of an atom. At room temperature the atom contains the same
number of electrons as there are protons in the nucleus, which makes
the atom electrically neutral.


It is the electrons that define the physical and chemical properties
of the elements as we experience them on Earth.

An atom of hydrogen has one proton and one orbiting electron while an
atom of iron-56 has 26 electrons surrounding a nucleus containing 26
protons and 30 neutrons. The normal notation is 56Fe. It is the number
of protons that defines the identity of an element. For each element
the number of neutrons can vary and atoms with the same number of
protons but differing numbers of neutrons are referred to as isotopes.
For example iron has stable isotopes with 28, 30 and 31 neutrons.

The neutrons and protons are held together in the nucleus by the
'strong force'.

The strong force only acts over very small distances but is able to
overcome the electrostatic repulsion between protons.

The most tightly bound nuclei are those close to iron in the periodic
table of elements. The tightness of this binding is measured by the
binding energy per nucleon where 'nucleon' is a collective name for
neutrons and protons.

It is also sometimes called the mass defect per nucleon. This reflects
the fact that the total mass of the nucleus is less than the sum of
the mass of the individual neutrons and protons that formed the
nucleus.

The difference in mass is equivalent to the energy released in forming
the nucleus. The graph plots binding energy as a function of atomic
number or number of nucleons per atom.

The general decrease in binding energy beyond iron is caused by the
fact that, as the nucleus gets bigger, the ability of the strong force
to counteract the electrostatic force between the protons becomes
weaker.

The peaks in binding energy at 4,8,16 and 24 nucleons is a consequence
of the great stability of helium-4 a combination of two protons and
two neutrons. The maximum binding energy at iron means that elements
lighter than iron release energy when fused.


This is the source of energy in stars and hydrogen bombs. From the
graph it can be seen that the greatest release of energy occurs fusing
hydrogen to form helium. { Dhikr HUuuuu}


Elements heavier than iron only release energy when split, as was the
case with the plutonium and uranium used in the first atomic bombs.


Elements heavier than iron are made in stars by capturing neutrons
onto atomic nuclei. This takes place in some red giants and in
supernovae explosions. A new isotope is created when an atom captures
a neutron. If this isotope is unstable then a neutron can convert into
a proton, releasing an electron.

This is called beta decay and is a form of radioactive decay also
observed on Earth. By converting a neutron into a proton the atom has
increased its atomic number by one and become the adjacent element in
the periodic table.

It may then capture another neutron, and so on, so that using iron as
seed nuclei it is possible to build all the elements heavier than iron
in the periodic table.


The difference between element synthesis in red giants and supernovae
is that in supernovae the flux of neutrons is greater and it is
possible for the atom to capture a second, or third neutron, before it
has a chance to beta-decay. This leads to the production of a
different set of elements to those produced in red giants, where the
flux of neutrons is much less.