Sunsun Power

By · Sunday, April 19th, 2009

Sunsun Power

The sun is called Sol de America and that is where the term comes from the solar system. This is a typical main sequence star and is the largest object and most massive of our solar system. The Sun contains 99.8 percent of all matter in the solar system with Jupiter occupying most of the rest. The Sun is a population the one hand, GV2 class star and is sometimes referred to as a typical star that is true in many respects. However, the Sun is actually larger than most the other stars in the same class as the sun.

The Sun is composed of 74 percent hydrogen, 25 percent helium and traces of other elements. The temperature nucleus of the Suns, which is seen within 20 percent, is approximately 15.6 million degrees Kelvin, the pressure is 250 billion atmospheres and the density of mass is over 150 times that of water. Under such extreme conditions nuclear fusion occurs in which hydrogen atoms are combined with that of the helium atoms. This reaction releasing massive amounts amounts of energy as gamma rays and is responsible for the Suns of 386 billion billion megawatts of power. During During his journey out to the surface of these gamma rays are repeatedly absorbed and re-emitted at lower temperature and lower. At the time that the energy reaches the surface has been reduced to visible light and is done mostly through the latter part of the way convection than radiation.

The convective zone is the outer layer of the Suns to 70 percent of the radius of the Suns. It is an area where thermal convection takes place in a large thermal columns. These columns are heated by thermal nuclear fusion taking place in the heart of the Suns and the Suns rise to surface where they release their energy into space in the form of sunlight and dust. As the columns of discharge of its thermal energy to cool and sink down inside the Suns, which overheated and back to the surface again in a great cycle. The top of these large thermal columns can be seen on the surface of the Sun in the form of what is called solar granulation and supergranulation.

The surface layer of the Sun that we see is called the photosphere and has a temperature of about 5800 degrees Kelvin. Above the photosphere are five layers that make up the atmosphere of the Suns. They are the lowest temperature, the chromosphere, transition region, the crown and the heliosphere. The temperature of the region extends from the photosphere up to 2000 kilometers and has a temperature of about 4000 degrees Kelvin. This is cold enough for these molecules such as water and carbon monoxide exist and can be detected by their absorption spectra.

The chromosphere extends from the top the minimum temperature to another region of 2000 kilometers and is named for the Greek word chrome color. The chromosphere can be seen as a flash of color on the right in the beginning and end of a total solar eclipse of the sun. Interestingly, the temperature of the chromosphere increases gradually with altitude at temperatures of up to 100,000 degrees Kelvin at the top.

Above the chromosphere is a transition region where the temperature rises quickly to about a million degrees Kelvin. This temperature rise is caused by what is known as a phase transition of the element helium in the region of transition. The transition region has no well-defined height and is in constant motion. The transition zone is not easy to see from Earth, but can be observed by space-based instruments operating in the region far ultraviolet spectrum.

After the chromosphere is the corona which is much higher than the previous layers of the Suns atmosphere and extends far into space. The corona is characterized by solar prominences, which are huge clouds of super hot glowing gas that has erupted from the upper chromosphere. The crown may clearly seen during total eclipses of the sun and is very spectacular to see. The crown is composed of charged particles that become what we call the solar wind, and radiating outward from the sun at 450 miles per second and are responsible for the Aurora Borealis.

Beyond the crown is the heliosphere, which is also known as the magnetosphere. The heliosphere is immensely strong and extends far beyond the orbit of the dwarf planet Pluto. The solar wind travels outward along the heliosphere until it collides with helicopter platforms about 50 astronomical units from the sun.

When viewed with appropriate filters, we can see sunspots on the surface of the sun. These points have a lower temperature than the surrounding area and therefore appear dark. Sunspots are areas where intense magnetic power convection heat from the sun's interior is inhibited. Sunspots are usually couples with opposite magnetic polarity and are responsible for the eruptions solar. The number of sunspots varies over an eleven-year solar cycle.

The Sun has been active for about four and a half billion years and has used up about half of the hydrogen fuel it started with. The sun will burn for another five billion years after which they begin to helium the strength to go under the nuclear fusion into heavier elements. This will cause the Sun swells in size to the point of consumption of the Earth and as it becomes what is called a red giant. Billion years after becoming a red giant sun, eventually will collapse into a white dwarf. Incredibly, then it could take up to a trillion years to cool.

Burl T Collins is the owner of The Dragons Crystal Ball Astrology Tarot and Horoscope Pavillion

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