The Evolution of the star of the mass similar to that of the mass of the Sun wil

Question

The Evolution of the star of the mass similar to that of the mass of the Sun will most likely take following steps: 1_______ the stage before the ignition of the nuclear reactions converting _______ into _______. 2 _______ Star -- star is in equilbrium during this stage: the force of _______ is equal to the force of _______ pressure stabilizing the star's radius. The conversion of the _______ into _______ via nuclear _______ is providing the radiation in the stellar _______. This stage typically last up to _______ billion years. 3 _______ -- as result of depletion of the _______ in the stellar _______, and increased density of _______ the star can now convert _______ into the _______. This set of reactions provide the net energy that is much _______ than the one fuelling the previous stage. As result the force of _______is higher than the force of _______ acting on he star which leads to the _______ of star's radius. The star of Sun's mass will last in this stage for up to 10 _______ years.

Explanation / Answer

Small stars have a mass upto one and a half times that of the Sun.
Stage 1- Stars are born in a region of high density Nebula, and condenses into a huge globule of gas and dust and contracts under its own gravity.
This image shows the Orion Nebula or M42 .
Stage 2 - A region of condensing matter will begin to heat up and start to glow forming Protostars. If a protostar contains enough matter the central temperature reaches 15 million degrees centigrade.
This image is the outflow (coloured red)and protostar.
Stage 3 - At this temperature, nuclear reactions in which hydrogen fuses to form helium can start.
Stage 4 - The star begins to release energy, stopping it from contracting even more and causes it to shine. It is now a Main Sequence Star.
The nearest main sequence star to Earth, the Sun
Stage 5 - A star of one solar mass remains in main sequence for about 10 billion years, until all of the hydrogen has fused to form helium.
Stage 6 - The helium core now starts to contract further and reactions begin to occur in a shell around the core.
Stage 7 - The core is hot enough for the helium to fuse to form carbon. The outer layers begin to expand, cool and shine less brightly. The expanding star is now called a Red Giant.
The star expands to a Red Giant, below
Stage 8 - The helium core runs out, and the outer layers drift of away from the core as a gaseous shell, this gas that surrounds the core is called a Planetary Nebula.
A Planetary Nebula
(Below, NGC 6543).
Stage 9 - The remaining core (thats 80% of the original star) is now in its final stages. The core becomes a White Dwarf the star eventually cools and dims. When it stops shining, the now dead star is called a Black Dwarf.
Massive Stars - The Life of a Star of about 10 Solar Masses
Massive stars have a mass 3x times that of the Sun. Some are 50x that of the Sun
Stage 1 - Massive stars evolve in a simlar way to a small stars until it reaces its main sequence stage (see small stars, stages 1-4). The stars shine steadily until the hydrogen has fused to form helium ( it takes billions of years in a small star, but only millions in a massive star).
Stage 2 - The massive star then becomes a Red Supergiant and starts of with a helium core surrounded by a shell of cooling, expanding gas.
The massive star is much bigger in its expanding stage.
(A Red Supergiant,below).
Stage 3 - In the next million years a series of nuclear reactions occur forming different elements in shells around the iron core.
Stage 4 - The core collapses in less than a second, causing an explosion called a Supernova, in which a shock wave blows of the outer layers of the star. (The actual supernova shines brighter than the entire galaxy for a short time).
The set of images below shows the star going into a stage called Supernova and contracting to become a neutron star
The images above were from the HEASARC Homepage
Stage 5 - Sometimes the core survives the explosion. If the surviving core is between 1.5 - 3 solar masses it contracts to become a a tiny, very dense Neutron Star. If the core is much greater than 3 solar masses, the core contracts to become a Black Hole.

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