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Star
The Pleiades, an open cluster of stars in the constellation of Taurus. NASA photo
Contents
1 Observation history
2 Star designations
3 Units of measurement
4 Formation and evolution
4.1 Protostar formation
4.2 Main sequence
4.3 Post-main sequence
4.3.1 Massive stars
4.3.2 Collapse
5 Distribution
6 Characteristics
6.1 Age
6.2 Chemical composition
6.3 Diameter
6.4 Kinematics
6.5 Mass
6.6 Rotation
6.7 Temperature
7 Radiation
7.1 Luminosity
7.2 Magnitude
8 Classification
9 Variable stars
10 Structure
11 Nuclear fusion reaction pathways
12 See also
13 References
14 Further reading
15 External links
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This article is about the astronomical object. For other uses, see Star (disambiguation).
Look up Star in
Wiktionary, the free dictionary.A star is a massive, luminous ball of plasma. Stars group together to form galaxies, and they dominate the visible universe. The nearest star to Earth is the Sun, which is the source of most of the energy on Earth, including daylight. Other stars are visible in the night sky, when they are not outshone by the Sun. A star shines because nuclear fusion in its core releases energy which traverses the star's interior and then radiates into outer space. Almost all elements heavier than hydrogen and helium were created inside the cores of stars.
Astronomers can determine the mass, age, chemical composition and many other properties of a star by observing its spectrum, luminosity and motion through space. The total mass of a star is the principal determinant in its evolution and eventual fate. Other characteristics of a star that are determined by its evolutionary history include the diameter, rotation, movement and temperature. A plot of the temperature of many stars against their luminosities, known as a Hertzsprung-Russell diagram (H-R diagram), allows the current age and evolutionary state of a particular star to be determined.
A star begins as a collapsing cloud of material that is composed primarily of hydrogen along with some helium and heavier trace elements. Once the stellar core is sufficiently dense, some of the hydrogen is steadily converted into helium through the process of nuclear fusion. The remainder of the star's interior carries energy away from the core through a combination of radiative and convective processes. These processes keep the star from collapsing upon itself and the energy generates a stellar wind at the surface and radiation into outer space.[1]
Once the hydrogen fuel at the core is exhausted, a star of at least 0.4 times the mass of the Sun[2] expands to become a red giant, fusing heavier elements at the core, or in shells around the core. It then evolves into a degenerate form, recycling a portion of the matter into the interstellar environment where it will form a new generation of stars with a higher proportion of heavy elements.
Binary and multi-star systems consist of two or more stars that are gravitationally bound, and generally move around each other in stable orbits. When two such stars have a relatively close [orbit], their gravitational interaction can have a significant impact on their evolution.
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