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Sunbursts and Solar Energy
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During its first 50 million years, the sun contracted to approximately its present size. Gravitational energy released by the collapsing gas heated the interior, and when the core was hot enough, the contraction ceased and the nuclear burnoing of hydrogen into helium began in the core. The sun has been in this stage of its life for about 4.5 billion years      The sun, by the gravitational effects of its mass, dominates the planetary system that includes the earth      By the radiation of its electromagnetic energy, the sun furnishes all of the energy supporting all life on earth, because all foods and all fuels are derived ultimately from plants using the energy of sunlight - photosynthesis.      Because of its proximity to the earth, and because it is such a typical star, the sun is a unique resource for the study of stellar phenomena      No other star can be studied in such detail. The star closest to the sun is located approximately 4.3 lightyears away

To observe features on the sun's surface of comparable size to those that can be seen routinely on the sun would require a telescope more than 18 miles in diameter      The total amount of energy emitted by the sun in the form of radiation is remarkably constant, varying by no more than a few tenths of 1 percent over several days      energy output is generated deep within the sun      Like most stars, the sun is made up primarily of hydrogen. Specifically, 71% hydrogen, 27% helium, and 2% other elements      Near the center of the sun the temperature is almost 29,000,000 degrees Fahrenheit and the density is 150 times that of water

Within the sun, the nuclei of individual hydrogen atoms interact, undergoing nuclear fusion      During nuclear fusion in the sun, two hydrogen nuclei combine to make one helium nucleus, and energy is released in the form of gamma radiation      The fusion energy from the sun is equivalent to that which would be released from the explosion of 100 billion one-megaton hydrogen bombs per second      The nuclear burning of hydrogen in the core of the sun extends out to about 25 percent of the sun's radius      To properly view the sun you would have to put a telescope into space, like the Hubble telescope orbiting the earth currently, to avoid distortions caused by the earth's atmosphere

During its first 50 million years, the sun contracted to approximately its present size. Gravitational energy released by the collapsing gas heated the interior, and when the core was hot enough, the contraction ceased and the nuclear burning of hydrogen into helium began in the core. The sun has been in this stage of its life for about 4.5 billion years      The sun, by the gravitational effects of its mass, dominates the planetary system that includes the earth      By the radiation of its electromagnetic energy, the sun furnishes all of the energy supporting all life on earth, because all foods and all fuels are derived ultimately from plants using the energy of sunlight, which is photosynthesis.      The fusion energy from the sun is equivalent to that which would be released from the explosion of 100 billion one-megaton hydrogen bombs per second      The total amount of energy emitted by the sun in the form of radiation is remarkably constant, varying by no more than a few tenths of 1 percent over several days

Like most stars, the sun is made up primarily of hydrogen. Specifically, 71% hydrogen, 27% helium, and 2% other elements      To observe features on the sun's surface of comparable size to those that can be seen routinely on the sun would require a telescope more than 18 miles in diameter      Within the sun, the nuclei of individual hydrogen atoms interact, undergoing nuclear fusion      Near the center of the sun the temperature is almost 29,000,000 degrees Fahrenheit and the density is 150 times that of water      During nuclear fusion in the sun, two hydrogen nuclei combine to make one helium nucleus, and energy is released in the form of gamma radiation

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