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From Wikipedia, the free encyclopedia. Redirected from List of female porn stars. Wikimedia list article. This is a dynamic list and may never be able to satisfy particular standards for completeness.

You can help by expanding it with reliably sourced entries. Candy Barr. Tamaki Katori. Abella Danger Adriana Chechik A. Stars with sizeable sunspots may show significant variations in brightness as they rotate, and brighter areas of the surface are brought into view.

Bright spots also occur at the magnetic poles of magnetic stars. Stars with ellipsoidal shapes may also show changes in brightness as they present varying areas of their surfaces to the observer.

These are very close binaries, the components of which are non-spherical due to their mutual gravitation. As the stars rotate the area of their surface presented towards the observer changes and this in turn affects their brightness as seen from Earth.

The surface of the star is not uniformly bright, but has darker and brighter areas like the sun's solar spots. The star's chromosphere too may vary in brightness.

As the star rotates we observe brightness variations of a few tenths of magnitudes. They are apparently single giant stars with spectral types G and K and show strong chromospheric emission lines.

A possible explanation for the rapid rotation of FK Comae stars is that they are the result of the merger of a contact binary.

BY Draconis stars are of spectral class K or M and vary by less than 0. Stars in this class exhibit brightness fluctuations of some 0. Few pulsars have been detected in visible light.

These neutron stars change in brightness as they rotate. Because of the rapid rotation, brightness variations are extremely fast, from milliseconds to a few seconds.

The first and the best known example is the Crab Pulsar. Extrinsic variables have variations in their brightness, as seen by terrestrial observers, due to some external source.

One of the most common reasons for this is the presence of a binary companion star, so that the two together form a binary star. When seen from certain angles, one star may eclipse the other, causing a reduction in brightness.

Algol variables undergo eclipses with one or two minima separated by periods of nearly constant light. The prototype of this class is Algol in the constellation Perseus.

Double periodic variables exhibit cyclical mass exchange which causes the orbital period to vary predictably over a very long period.

The best known example is V Scorpii. The light curves of this class of eclipsing variables are constantly changing, making it almost impossible to determine the exact onset and end of each eclipse.

W Serpentis is the prototype of a class of semi-detached binaries including a giant or supergiant transferring material to a massive more compact star.

The stars in this group show periods of less than a day. The stars are so closely situated to each other that their surfaces are almost in contact with each other.

Stars with planets may also show brightness variations if their planets pass between Earth and the star.

These variations are much smaller than those seen with stellar companions and are only detectable with extremely accurate observations. From Wikipedia, the free encyclopedia.

For the novel by Robert A. Heinlein and Spider Robinson, see Variable Star. This article needs additional citations for verification.

Please help improve this article by adding citations to reliable sources. Unsourced material may be challenged and removed.

Main article: Variable star designation. Main article: Stellar pulsation. Main article: Cepheid variable. Main article: Classical Cepheid variable.

Main article: Type II Cepheids. Main article: RR Lyrae variable. Main article: Delta Scuti variable.

Main article: SX Phoenicis variable. Main article: Rapidly oscillating Ap star. Main article: Long period variable. Main article: Mira variable.

Main article: Semiregular variable. Main article: Slow irregular variable. Main article: Beta Cephei variable.

Main article: Slowly pulsating B-type star. Main article: PV Telescopii variable. Main article: RV Tauri variable.

Main article: Alpha Cygni variable. Main article: Gamma Doradus variable. Main article: Pulsating white dwarf. Main article: Pre—main-sequence star.

Main article: Orion variable. Main article: FU Orionis star. Main article: Luminous blue variable. Main article: Yellow hypergiant.

Main article: R Coronae Borealis variable. Main article: Wolf—Rayet star. Main article: Gamma Cassiopeiae variable. Main article: Flare star.

Main article: RS Canum Venaticorum variable. Main articles: Cataclysmic variable star and Symbiotic variable star. Main article: Supernova.

Main article: Luminous red nova. Main article: Nova. Main article: Dwarf nova. Main article: Intermediate polar.

Main article: Polar cataclysmic variable star. Main article: Z Andromedae variable. Main article: AM Canum Venaticorum star. Main article: Alpha-2 Canum Venaticorum variable.

Main article: SX Arietis variable. Main article: Pulsar. Main article: Algol variable. Main article: Double periodic variable.

Main article: Beta Lyrae variable. Main article: W Ursae Majoris variable. Star portal. Space Science Reviews. Bibcode : SSRv.. Cambridge Archaeological Journal.

Bibcode : CArcJ.. The Astrophysical Journal. Bibcode : ApJ Bibcode : PLoSO.. Odessa Astronomical Publications.

Bibcode : OAP Retrieved 15 April Retrieved Jocelyn Bell An Introduction to the Sun and Stars. Cambridge University Press. New Astronomy.

Bibcode : NewA Accessed October 2, Annual Review of Astronomy and Astrophysics. As a general rule, the more massive the star, the shorter its life span.

Birth takes place inside hydrogen-based dust clouds called nebulae. Over the course of thousands of years, gravity causes pockets of dense matter inside the nebula to collapse under their own weight.

Because the dust in the nebulae obscures them, protostars can be difficult for astronomers to detect. As a protostar gets smaller, it spins faster because of the conservation of angular momentum—the same principle that causes a spinning ice skater to accelerate when she pulls in her arms.

Increasing pressure creates rising temperatures, and during this time, a star enters what is known as the relatively brief T Tauri phase.

Most of the stars in our galaxy, including the sun, are categorized as main sequence stars. They exist in a stable state of nuclear fusion, converting hydrogen to helium and radiating x-rays.

This process emits an enormous amount of energy, keeping the star hot and shining brightly. Some stars shine more brightly than others.

Their brightness is a factor of how much energy they put out—known as luminosity —and how far away from Earth they are. Color can also vary from star to star because their temperatures are not all the same.

Hot stars appear white or blue, whereas cooler stars appear to have orange or red hues. By plotting these and other variables on a graph called the Hertzsprung-Russell diagram, astronomers can classify stars into groups.

Along with main sequence and white dwarf stars, other groups include dwarfs, giants, and supergiants. Supergiants may have radii a thousand times larger than that of our own sun.

Stars spend 90 percent of their lives in their main sequence phase.

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Wikimedia Commons. They are the building blocks of galaxies, of which there are billions in the universe.

The life cycle of a star spans billions of years. As a general rule, the more massive the star, the shorter its life span.

Birth takes place inside hydrogen-based dust clouds called nebulae. Over the course of thousands of years, gravity causes pockets of dense matter inside the nebula to collapse under their own weight.

Because the dust in the nebulae obscures them, protostars can be difficult for astronomers to detect.

As a protostar gets smaller, it spins faster because of the conservation of angular momentum—the same principle that causes a spinning ice skater to accelerate when she pulls in her arms.

Increasing pressure creates rising temperatures, and during this time, a star enters what is known as the relatively brief T Tauri phase.

Most of the stars in our galaxy, including the sun, are categorized as main sequence stars. They exist in a stable state of nuclear fusion, converting hydrogen to helium and radiating x-rays.

This process emits an enormous amount of energy, keeping the star hot and shining brightly. Some stars shine more brightly than others.

Their brightness is a factor of how much energy they put out—known as luminosity —and how far away from Earth they are.

Color can also vary from star to star because their temperatures are not all the same. Hot stars appear white or blue, whereas cooler stars appear to have orange or red hues.

By plotting these and other variables on a graph called the Hertzsprung-Russell diagram, astronomers can classify stars into groups.

Along with main sequence and white dwarf stars, other groups include dwarfs, giants, and supergiants. Supergiants may have radii a thousand times larger than that of our own sun.

Stars spend 90 percent of their lives in their main sequence phase. Now around 4. As stars move toward the ends of their lives, much of their hydrogen has been converted to helium.

Helium sinks to the star's core and raises the star's temperature—causing its outer shell of hot gases to expand. These large, swelling stars are known as red giants.

The red giant phase is actually a prelude to a star shedding its outer layers and becoming a small, dense body called a white dwarf. White dwarfs cool for billions of years.

Some, if they exist as part of a binary star system , may gather excess matter from their companion stars until their surfaces explode, triggering a bright nova.

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