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Die Stars und ihre Geschichten finden Sie immer topaktuell auf vcd-vl.be! Alle Stars, die besten Schnappschüsse und Fehltritte: vcd-vl.be Stars aktuell: Die neusten Promi News, Interviews mit Stars und Geschichten zu deinem Lieblings-VIP findest du in unseren vcd-vl.be Star News. Ein Star oder auch, alternativ oder ist eine prominente Persönlichkeit mit überragenden Leistungen auf einem bestimmten Gebiet und einer herausgehobenen medialen Präsenz. News zu Stars und VIPs: Ob Hollywood-Schauspieler, TV-Liebling, C-Promi oder Supermodel - auf vcd-vl.be verpassen Sie keine News zu ihrem Star. Welche neuen süßen Bilder gibt es aus den Familien der Stars? Was hat der Lieblingsschauspieler im Interview gesagt? Wer über News, Partys und das Leben.

Stars

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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. New Liskeard , Ontario , Kanada. Opava , Tjeckien. Stockholm , Sverige.

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On the other hand, the most massive stars, known as hypergiants, may be or more times more massive than the Sun, and have surface temperatures of more than 30, K.

Hypergiants emit hundreds of thousands of times more energy than the Sun, but have lifetimes of only a few million years.

Although extreme stars such as these are believed to have been common in the early Universe, today they are extremely rare - the entire Milky Way galaxy contains only a handful of hypergiants.

In general, the larger a star, the shorter its life, although all but the most massive stars live for billions of years. When a star has fused all the hydrogen in its core, nuclear reactions cease.

Deprived of the energy production needed to support it, the core begins to collapse into itself and becomes much hotter. Hydrogen is still available outside the core, so hydrogen fusion continues in a shell surrounding the core.

The increasingly hot core also pushes the outer layers of the star outward, causing them to expand and cool, transforming the star into a red giant.

If the star is sufficiently massive, the collapsing core may become hot enough to support more exotic nuclear reactions that consume helium and produce a variety of heavier elements up to iron.

However, such reactions offer only a temporary reprieve. Gradually, the star's internal nuclear fires become increasingly unstable - sometimes burning furiously, other times dying down.

These variations cause the star to pulsate and throw off its outer layers, enshrouding itself in a cocoon of gas and dust.

What happens next depends on the size of the core. Universe Learn About This Image. Stars Stars are the most widely recognized astronomical objects, and represent the most fundamental building blocks of galaxies.

Star Formation Stars are born within the clouds of dust and scattered throughout most galaxies. Black Holes. The Big Bang. Helpful Links Organization and Staff.

Astrophysics Fleet Mission Chart. Spacecraft Paper Models. Related Content Mysteries of the Sun. Death of Stars video.

Life Cycles of Stars. More About Stars. Stellar Evolution. Recommended Articles. Remembering Riccardo Giacconi, X-Ray December 11, Finding the Invisible.

March 10, Hubble Captures the Galaxy's July 03, July 10, Ask a Question. Average Stars Become White Dwarfs For average stars like the Sun, the process of ejecting its outer layers continues until the stellar core is exposed.

This dead, but still ferociously hot stellar cinder is called a White Dwarf.

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Average Stars Become White Dwarfs For average stars like the Sun, the process of ejecting its outer layers continues until the stellar core is exposed.

This dead, but still ferociously hot stellar cinder is called a White Dwarf. White dwarfs, which are roughly the size of our Earth despite containing the mass of a star, once puzzled astronomers - why didn't they collapse further?

What force supported the mass of the core? Quantum mechanics provided the explanation. Pressure from fast moving electrons keeps these stars from collapsing.

The more massive the core, the denser the white dwarf that is formed. Thus, the smaller a white dwarf is in diameter, the larger it is in mass!

These paradoxical stars are very common - our own Sun will be a white dwarf billions of years from now.

White dwarfs are intrinsically very faint because they are so small and, lacking a source of energy production, they fade into oblivion as they gradually cool down.

This fate awaits only those stars with a mass up to about 1. Above that mass, electron pressure cannot support the core against further collapse.

Such stars suffer a different fate as described below. White Dwarfs May Become Novae If a white dwarf forms in a binary or multiple star system, it may experience a more eventful demise as a nova.

Nova is Latin for "new" - novae were once thought to be new stars. Today, we understand that they are in fact, very old stars - white dwarfs.

If a white dwarf is close enough to a companion star, its gravity may drag matter - mostly hydrogen - from the outer layers of that star onto itself, building up its surface layer.

When enough hydrogen has accumulated on the surface, a burst of nuclear fusion occurs, causing the white dwarf to brighten substantially and expel the remaining material.

Within a few days, the glow subsides and the cycle starts again. Sometimes, particularly massive white dwarfs those near the 1. Supernovae Leave Behind Neutron Stars or Black Holes Main sequence stars over eight solar masses are destined to die in a titanic explosion called a supernova.

A supernova is not merely a bigger nova. In a nova, only the star's surface explodes. In a supernova, the star's core collapses and then explodes.

In massive stars, a complex series of nuclear reactions leads to the production of iron in the core. Having achieved iron, the star has wrung all the energy it can out of nuclear fusion - fusion reactions that form elements heavier than iron actually consume energy rather than produce it.

The star no longer has any way to support its own mass, and the iron core collapses. In just a matter of seconds the core shrinks from roughly miles across to just a dozen, and the temperature spikes billion degrees or more.

The outer layers of the star initially begin to collapse along with the core, but rebound with the enormous release of energy and are thrown violently outward.

Supernovae release an almost unimaginable amount of energy. For a period of days to weeks, a supernova may outshine an entire galaxy.

Likewise, all the naturally occurring elements and a rich array of subatomic particles are produced in these explosions. On average, a supernova explosion occurs about once every hundred years in the typical galaxy.

About 25 to 50 supernovae are discovered each year in other galaxies, but most are too far away to be seen without a telescope.

Neutron Stars If the collapsing stellar core at the center of a supernova contains between about 1. Neutron stars are incredibly dense - similar to the density of an atomic nucleus.

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.

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