Difference between revisions of "Star"
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− | + | : '''''Sun''' redirects here. For information on [[Earth]]'s sun, see [[Sol]].'' | |
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+ | A '''star''' (or "'''sun'''") is a massive [[energy]]-producing sphere of [[plasma]] and gas located in [[space]]. The region around a star that is held by its gravity, including any [[planet]]s, [[moon]]s, comets, and [[asteroid]]s, is called a [[star system]]. | ||
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− | + | ==Stellar Life Cycle== | |
+ | [[Image:Sol.jpg|thumb|<center>[[Sol]], Earth's star</center>]] | ||
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===Formation=== | ===Formation=== | ||
− | Stars are born out of huge gaseous [[nebula]]e. Inside these nebulae, centers of higher density form, slowly accumulating more mass as the center's gravity increases, to form a [[protostar]]. | + | Stars are born out of huge gaseous [[nebula]]e. Inside these nebulae, centers of higher density form, slowly accumulating more mass as the center's gravity increases, to form a [[Wikipedia:Protostar|protostar]]. Pressure in the interior of the protostar rises, in turn increasing the density and temperature until the gas turns to plasma, where the atomic nuclei and the electrons are dissociated from each other. At a sufficient temperature and pressure, [[Wikipedia:Nuclear fusion|nuclear fusion]] is initiated at the core, producing light: the star is born. |
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− | ===Star | + | [[Image:Risan_sunset.jpg|thumb|<center>The two suns of Risa</center>]] |
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+ | ===Star Evolution=== | ||
Stars can be made up of various different elements depending on their age. | Stars can be made up of various different elements depending on their age. | ||
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− | + | '''Young stars''' mainly consist of hydrogen, which is fused to helium thereby increasing the star's helium ratio over time and producing large quantities of energy. <br>This energy, in turn, creates extreme pressure, preventing the star from collapsing under its own gravity. | |
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− | + | Due to its larger surface area, the star turns red and is then called a [[Wikipedia:Red giant|red giant]]. After the sun runs out of light elements and the number of fusion reactions decreases, its own gravity causes it to collapse and to expel its outer layers of matter, creating beautiful "planetary nebulae". The remnant of the star is called [[Wikipedia: White dwarf|white dwarf]]. | |
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Every star has to pass these stages of evolution. However, depending on their masses, some suns experience further changes. | Every star has to pass these stages of evolution. However, depending on their masses, some suns experience further changes. | ||
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Below 1.5 [[Sol]] masses: After 1-10 billion years any nuclear reactions inside the white dwarf finally cease and the star turns to a "black dwarf", a very small stellar corpse. | Below 1.5 [[Sol]] masses: After 1-10 billion years any nuclear reactions inside the white dwarf finally cease and the star turns to a "black dwarf", a very small stellar corpse. | ||
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− | Above 1.5 Sol masses: The white dwarf swells again, fusing all elements up to | + | Above 1.5 Sol masses: The white dwarf swells again, fusing all elements up to iron. After the last iron is depleted, the star turns into a [[Wikipedia:Supernova|supernova]], where the outer layers of the sun explode, which, in turn, causes a massive shock wave. The remains of this explosion are a vast matter nebula and a tiny [[Wikipedia:Neutron star|neutron star]], which is so dense, that all [[Wikipedia:Proton|protons]] and [[Wikipedia:Electron|electrons]] are neutralized to [[Wikipedia:Neutron|neutrons]]. A special form of neutron stars are [[pulsar]]s. |
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− | + | As a sun gets older, it begins to fuse heavier elements, like helium, as the lighter elements like hydrogen are depleted. <br>This, however, releases more energy, causing the star to swell, which increases its surface area from which the energy is emitted. This phase marks the beginning of the star's end. | |
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If the remnant of a supernova is more massive than 2.5 Sol masses, it collapses to a [[black hole]]. | If the remnant of a supernova is more massive than 2.5 Sol masses, it collapses to a [[black hole]]. | ||
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==Stellar classification== | ==Stellar classification== | ||
− | Stars are assigned to different [[spectral | + | Stars are assigned to different [[Star Classification Table|spectral classes]]. |
===Parts of stars=== | ===Parts of stars=== | ||
− | * [ | + | * [https://memory-alpha.fandom.com/wiki/Corona corona] |
− | * [ | + | * [https://memory-alpha.fandom.com/wiki/Stellar_core stellar core] |
− | * [ | + | * [https://memory-alpha.fandom.com/wiki/Chromosphere chromosphere] |
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===Types of stars=== | ===Types of stars=== | ||
*[[Protostar]] | *[[Protostar]] | ||
− | *Star | + | *'''Star''' |
− | **[[ | + | **[[wikipedia:F-type main-sequence star|F-type star]] |
− | **[[ | + | **[[wikipedia:Flare star|Flare star]] |
− | **[[G-type star]] | + | **[[wikipedia:G-type main-sequence star|G-type star]]<br>Also called a "''yellow dwarf star''" |
+ | **[[wikipedia:Hypergiant|Hypergiant]] | ||
**[[Neutron star]] | **[[Neutron star]] | ||
− | **[[O-type star]] | + | **[[wikipedia:O-type star|O-type star]] |
− | **[[Pulsar]] | + | **[[Pulsar (Star)|Pulsar]] |
− | **[[Red dwarf]] | + | **[[wikipedia:Red dwarf|Red dwarf]] |
**[[Red giant]] | **[[Red giant]] | ||
− | **[[Supergiant]] | + | **[[wikipedia:Supergiant|Supergiant]] |
− | **[[White dwarf | + | **[[wikipedia:White dwarf|White dwarf]] |
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*[[Black hole]] | *[[Black hole]] | ||
− | == | + | == Fun Facts == |
− | *[[ | + | *In [[2367]], [https://memory-alpha.fandom.com/wiki/Timicin Dr. Timicin] of the planet [https://memory-alpha.fandom.com/wiki/Kaelon_II Kaelon II] tried to save his system's dying star by regulating its ever-increasing temperature with the bombardment of [[photon torpedo]]es. <br>However, the experiment failed after testing the procedure with a star in an uninhabited solar system. |
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+ | *The resulting electromagnetic pulse from the supernova of [[Beta Magellan]] in [[2364]] was so feared by the computer-dependent [[Bynar]] in the nearby [[Beta Magellan system]] that they commandeered the [[USS Enterprise, NCC-1701-D|Enterprise-D]] as a temporary dump for their planetary computer. | ||
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+ | *In [[2373]], a series of supernovae witnessed by the {{USS|Voyager}} in the [[Delta Quadrant]] turned out to be the real-time result of "battles" during a civil war in the [[Q Continuum]]. <br>They were actually created by spatial disruptions in the Continuum, which created a negative-density false vacuum that sucked nearby matter into the Continuum. | ||
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+ | [[category: science]] |
Latest revision as of 02:12, 9 November 2021
A star (or "sun") is a massive energy-producing sphere of plasma and gas located in space. The region around a star that is held by its gravity, including any planets, moons, comets, and asteroids, is called a star system.
Contents
Stellar Life Cycle
Formation
Stars are born out of huge gaseous nebulae. Inside these nebulae, centers of higher density form, slowly accumulating more mass as the center's gravity increases, to form a protostar. Pressure in the interior of the protostar rises, in turn increasing the density and temperature until the gas turns to plasma, where the atomic nuclei and the electrons are dissociated from each other. At a sufficient temperature and pressure, nuclear fusion is initiated at the core, producing light: the star is born.
Star Evolution
Stars can be made up of various different elements depending on their age.
Young stars mainly consist of hydrogen, which is fused to helium thereby increasing the star's helium ratio over time and producing large quantities of energy.
This energy, in turn, creates extreme pressure, preventing the star from collapsing under its own gravity.
Due to its larger surface area, the star turns red and is then called a red giant. After the sun runs out of light elements and the number of fusion reactions decreases, its own gravity causes it to collapse and to expel its outer layers of matter, creating beautiful "planetary nebulae". The remnant of the star is called white dwarf.
Every star has to pass these stages of evolution. However, depending on their masses, some suns experience further changes.
Below 1.5 Sol masses: After 1-10 billion years any nuclear reactions inside the white dwarf finally cease and the star turns to a "black dwarf", a very small stellar corpse.
Above 1.5 Sol masses: The white dwarf swells again, fusing all elements up to iron. After the last iron is depleted, the star turns into a supernova, where the outer layers of the sun explode, which, in turn, causes a massive shock wave. The remains of this explosion are a vast matter nebula and a tiny neutron star, which is so dense, that all protons and electrons are neutralized to neutrons. A special form of neutron stars are pulsars.
As a sun gets older, it begins to fuse heavier elements, like helium, as the lighter elements like hydrogen are depleted.
This, however, releases more energy, causing the star to swell, which increases its surface area from which the energy is emitted. This phase marks the beginning of the star's end.
If the remnant of a supernova is more massive than 2.5 Sol masses, it collapses to a black hole.
Stellar classification
Stars are assigned to different spectral classes.
Parts of stars
Types of stars
- Protostar
- Star
- F-type star
- Flare star
- G-type star
Also called a "yellow dwarf star" - Hypergiant
- Neutron star
- O-type star
- Pulsar
- Red dwarf
- Red giant
- Supergiant
- White dwarf
- Black hole
Fun Facts
- In 2367, Dr. Timicin of the planet Kaelon II tried to save his system's dying star by regulating its ever-increasing temperature with the bombardment of photon torpedoes.
However, the experiment failed after testing the procedure with a star in an uninhabited solar system.
- The resulting electromagnetic pulse from the supernova of Beta Magellan in 2364 was so feared by the computer-dependent Bynar in the nearby Beta Magellan system that they commandeered the Enterprise-D as a temporary dump for their planetary computer.
- In 2373, a series of supernovae witnessed by the USS Voyager in the Delta Quadrant turned out to be the real-time result of "battles" during a civil war in the Q Continuum.
They were actually created by spatial disruptions in the Continuum, which created a negative-density false vacuum that sucked nearby matter into the Continuum.