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00:04:01 1 Observation history
00:15:35 2 Designations
00:18:42 3 Units of measurement
00:20:59 4 Formation and evolution
00:24:19 4.1 Star formation
00:27:24 4.2 Main sequence
00:31:00 4.3 Post–main sequence
00:33:02 4.3.1 Massive stars
00:34:46 4.3.2 Collapse
00:37:28 4.3.3 Binary stars
00:38:18 5 Distribution
00:41:30 6 Characteristics
00:41:53 6.1 Age
00:43:07 6.2 Chemical composition
00:44:36 6.3 Diameter
00:46:05 6.4 Kinematics
00:47:53 6.5 Magnetic field
00:49:52 6.6 Mass
00:52:51 6.7 Rotation
00:54:53 6.8 Temperature
00:56:19 7 Radiation
00:59:00 7.1 Luminosity
01:00:16 7.2 Magnitude
01:04:43 8 Classification
01:07:34 9 Variable stars
01:09:45 10 Structure
01:14:41 11 Nuclear fusion reaction pathways



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"I cannot teach anybody anything, I can only make them think."
- Socrates


SUMMARY
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A star is type of astronomical object consisting of a luminous spheroid of plasma held together by its own gravity. The nearest star to Earth is the Sun. Many other stars are visible to the naked eye from Earth during the night, appearing as a multitude of fixed luminous points in the sky due to their immense distance from Earth. Historically, the most prominent stars were grouped into constellations and asterisms, the brightest of which gained proper names. Astronomers have assembled star catalogues that identify the known stars and provide standardized stellar designations. However, most of the estimated 300 sextillion (3×1023) stars in the Universe are invisible to the naked eye from Earth, including all stars outside our galaxy, the Milky Way.
For at least a portion of its life, a star shines due to thermonuclear fusion of hydrogen into helium in its core, releasing energy that traverses the star's interior and then radiates into outer space. Almost all naturally occurring elements heavier than helium are created by stellar nucleosynthesis during the star's lifetime, and for some stars by supernova nucleosynthesis when it explodes. Near the end of its life, a star can also contain degenerate matter. Astronomers can determine the mass, age, metallicity (chemical composition), and many other properties of a star by observing its motion through space, its luminosity, and spectrum respectively. The total mass of a star is the main factor that determines its evolution and eventual fate. Other characteristics of a star, including diameter and temperature, change over its life, while the star's environment affects its rotation and movement. A plot of the temperature of many stars against their luminosities produces a plot known as a Hertzsprung–Russell diagram (H–R diagram). Plotting a particular star on that diagram allows the age and evolutionary state of that star to be determined.
A star's life begins with the gravitational collapse of a gaseous nebula of material composed primarily of hydrogen, along with helium and trace amounts of heavier elements. When the stellar core is sufficiently dense, hydrogen becomes steadily converted into helium through nuclear fusion, releasing energy in the process. The remainder of the star's interior carries energy away from the core through a combination of radiative and convective heat transfer processes. The star's internal pressure prevents it from collapsing further under its own gravity. A star with mass greater than 0.4 times the Sun's will expand to become a red giant when the hydrogen fuel in its core is exhausted. In some cases, it will fuse heavier elements at the core or in shells around the core. As the star expands it throws a part of its mass, enriched with those heavier elements, into the interstellar environment, to be recycled later as new stars. Meanwhile, the core becomes a stellar remnant: a white dwarf, a neutron star, or if it is sufficiently massive a black hole.
Binary and multi-star systems consist of two or m ...

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