STARS
Published on Nov 19, 2015
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STARS
Photo by Instant Vantage
How do stars works
Stars are gigantic balls of plasma, which is ionized gas, is held together by gravity. Stars work because of thermonuclear fusion. In the very hot and dense core, hydrogen atoms fuse into helium atoms. The energy released by the fusion is conveyed to the surface and radiates into space. The counterbalance of gravity pulling inward and the pressure of nuclear reaction pushing outward keeps the sun stable until it starts to run out fuel, at which point it will expand.
Photo by bulliver
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What are stars made of
Plasma, gases
Hydrogen and helium
Photo by Pink Sherbet Photography
How do stars form
Stars are born within the clouds of dust and scattered throughout most galaxies. A familiar example of such as a dust cloud is the Orion Nebula, revealed in vivid detail in the adjacent image, which combines images at visible and infrared wavelengths measured by NASA's Hubble Space Telescope and Spitzer Space Telescope. Turbulence deep within these clouds gives rise to knots with sufficient mass that the gas and dust can begin to collapse under its own gravitational attraction. As the cloud collapses, the material at the center begins to heat up. Known as a protostar, it is this hot core at the heart of the collapsing cloud that will one day become a star. Three-dimensional computer models of star formation predict that the spinning clouds of collapsing gas and dust may break up into two or three blobs; this would explain why the majority the stars in the Milky Way are paired or in groups of multiple stars.
Photo by erick_vanbasten
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Photo by NASAblueshift
What's the the closest star
The sun
Photo by VinothChandar
How hot is the sun
At the core of the sun, gravitational attraction produces immense pressure and temperature, which can reach more than 27 million degrees F (15 million degrees C). Hydrogen atoms get compressed and fuse together, creating helium. This process is called nuclear fusion.
Nuclear fusion produces huge amounts of energy. The energy radiates outward to the sun's surface, atmosphere and beyond. From the core, energy moves to the radiative zone, where it bounces around for up to 1 million years before moving up to the convective zone, the upper layer of the sun's interior. The temperature here drops below 3.5 million degrees F (2 million degrees C). Large bubbles of hot plasma form a soup of ionized atoms and move upwards to the photosphere.
Photo by davedehetre
