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Stellar Evolution [See Link] - or Life of a Star.

Stellar evolution is the process by which a star undergoes a sequence of radical changes during its lifetime. Depending on the mass of the star, this lifetime ranges from only a few million years (for the most massive) to trillions of years (for the less massive), considerably more than the age of the universe.

Birth:

Star formation begins with the gravitational collapse of a giant molecular cloud. As the gases coalesce, heat and pressure increase until they condense into a rotating sphere of superhot gases. This is known as a protostar.

Protostars with masses less than roughly 1.6×1029 kg never reach temperatures high enough for nuclear fusion and become brown dwarfs.

For larger protostars, the core temperature will eventually reach 10 megakelvins, and nuclear fusion will begin.. The onset of nuclear fusion leads relatively quickly to a hydrostatic equilibrium in which energy released by the core exerts a "radiation pressure" balancing the weight of the star's matter, preventing further gravitational collapse.

The star thus evolves rapidly to a stable state.

Main Sequence.

Small, relatively cold, low mass red dwarfs burn hydrogen slowly and will burn for hundreds of billions of years

Massive hot supergiants will live for just a few million years.

A mid-sized star like the Sun will remain on the main sequence for about 10 billion years.

Maturity:

After millions to billions of years, depending on the initial mass of the star, the continuous fusion of hydrogen into helium causes a build-up of helium in the core. Eventually, the core exhausts its supply of hydrogen. Depending on the mass of the star, the outcome can vary.

Low Mass will become red dwarfs, such as Proxima Centauri, some of which will live thousands of times longer than the Sun.

Mid Sized will become red giants, such as Aldebaran and Arcturus .

Massive Stars will become red supergiants, such as VY Canis Majoris, Betelguise and Antares.

Stellar Remnants (The End)

After a star has burned out its fuel supply, depending on its mass, one of three things can happen.

For a star with a mass similar to the Sun, it will turn into a white dwarf and radiate the remaining heat into space for billions of years. Finally ending it's life as a black dwarf. (Though none exist at the moment, as the universe is not old enough).

For larger stars, depending on the chemical composition and temperature, the star explodes as a supernova. and either collapses into a neutron star or, if the remaining mass is large enough, the pressure will be insufficient to stop the total collapse and the star will become a black hole.

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Although at the end of a stars life - another "type" of star is born, they are different to the "normal" type of star and are "star" in name only. Most "remnants" of stars should be classed as degenerate stars.

Our Sun (a star) will first turn into a red giant star [See related question] and then a white dwarf star [See related question]

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The life cycle of a star is simply determined by what element said star is currently fusing. Our sun is currently burning through its vast supply of Hydrogen, and when that runs out it will switch to Helium, and so forth. Every time the mass of the element it's fusing increases, the energy given off by the fusion process also increases. This causes a star to swell, forming its red giant phase. Unfortunately any given star will eventually reach the point where the temperature and pressure within its core are not sufficient to fuse the element it's left with, and the star will die by either going supernova or shedding off it's gaseous outer layers and leaving behind a white dwarf.

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The nuclear reactions creating our Sun's energy all take place in the core. This energy then radiates outward to the surface. If you do some simple geometry, you'll see that the intensity of the energy from these nuclear reactions must be lower at the surface than at the core, where that energy starts. Lower energy intensity, lower temperature.

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A Protostar.

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No. White holes were a hypothesis which has never been shown to be correct.

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The ions leaving the sun are accelerated prior to entering the corona. The accelerated ions have a higher velocity and this higher velocity creates a higher temperature through collisions.

The corona is hotter than the photosphere because the sun's magnetic field carries energy upward from the surface and into the chromosphere and corona. The opposite effect is observed when the magnetic fields cause sunspots to form, resulting in cooler surfaces.

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The collapse of a star is based on its age. When it runs out of "Fuel" its inside contracts as the outside expands. it can then super nova or collapse into a tiny star.

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When the star becomes a "Red giant" is when the helium flash occurs.

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The answer is yes . Its only a matter of time before the Earth and the Sun both run out of energy but not in our lifetime.

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s

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No, you don't have to confuse "more massive" with "bigger". The most massive star in the eta Carinae system may have 100 times the mass of the Sun and be dozens of times bigger than our star but it is far smaller than VY CMa.

VY CMa is a red supergiant that has swollen to an extremely large size due to shell burning of different layers on its last stages of life. VY CMa is a cool star. On the other hand eta Carinae is very hot and it is in a different evolutionary state.

It is so massive that it will never reach the red supergiant state because it is losing mass at a fast rate. Also the companion play a role and alters the evolution.

Eventually eta Car will become a WR star (a naked core) and explode as a supernova. The same fate is expected for VY CMa but since it has already become a rec supergiant it is very likely that it won't become a WR star. This shows that VY CMa is far less massive than eta Car.

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Various isotopes of Hydrogen are fusible into Helium.

Helium is fusible into Carbon.

Carbon, various isotopes of Hydrogen, and Helium are fusible into Nitrogen and Oxygen.

After this the reactions get complex, but the final results are Nickel and Iron.

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Nebula

protostar

mid sized star

red giant

nova

white dwarf

black dwarf:)

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They are not hot.

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Just as the orbital period of the planets in the Solar System depend on the planets' distances from the sun, the answer to this question depends on how close to the black hole the star is.

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One item of note is that fairly recent studies indicate that the majority of stars in the galaxy are the faint and small red dwarfs; estimates of the population in our Milky Way galaxy say they constitute something between three quarters to over 85%, although most are too dim to see. Observations of nearby elliptical galaxies showed their abundance to be around twenty times that of our own galaxy. This changed some ideas about the universe and their abundance even tripled some estimates of the total number of stars.

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For galaxies without the gravitational underpinning of a central supermassive black hole, the mutual gravitational attraction of the stars plays a lead role in determining its general shape, rotation, and other characteristics. Recently, low-luminosity stars such as red dwarfs have been found to contribute a significant quantity of mass to galaxies; there is also gas, dust, and non-visible matter ("dark matter") adding to the gravitational pull.