salient aspects of structure of Sun and the various activities going on in
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Sun is a kind of star made from mainly two gases that are hydrogen and helium.It is very hot and only source of sunlight in earth.The reaction that take place in the earth between hydrogen and helium is called nuclear raction.
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HEY .
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Our sun is the closest star to Earth and the source of energy for all life here.The sun is essentially a huge burning ball of gas in the sky only 100 million or so miles from Earth. The majority of gas in the sun is hydrogen and helium, and it is so hot that all of these elements exist in the gaseous state. The gas is held together by gravity, which creates intense heat and pressure in the core. The sun has an interior consisting of the core, radiative zone, and convective zone. It has a visible surface called the photosphere, then the chromosphere, which usually isn't visible, and the very outer layer called the corona.
INNER LAYER
the sun has an inner core. This is where fusion occurs. The core is the very center of the sun where fusion occurs. The core has extremely high temperature and pressure. It is so hot here - 15 million degree Celsius - that nuclear fusion occurs. In the case of our sun, four hydrogen nuclei are fused into one helium nuclei while releasing a bunch of energy as photons. The sun produces so much energy.
The core is the hottest part of the sun and the only part of the sun that produces much energy. The sun cools off as you travel from the core to the outside, with the exception of the chromosphere.
The next layer of the sun is the radiative zone, the layer of the sun directly above the core. This zone, as you can probably guess, emits radiation, and the radiation from the core diffuses out from here. It may take photons millions of years to get out. The next layer as we work our way outward is the convective zone. In this layer, photons produced by fusion in the core make their way to the surface of the sun through convection.
The Solar Atmosphere
The visible solar atmosphere consists of three regions: the photosphere, the chromosphere, and the solar corona. Most of the visible (white) light comes from the photosphere, this is the part of the Sun we actually see. The chromosphere and corona also emit white light, and can be seen when the light from the photosphere is blocked out, as occurs in a solar eclipse. The sun emits electromagnetic radiation at many other wavelengths as well. Different types of radiation (such as radio, ultraviolet, X-rays, and gamma rays) originate from different parts of the sun.
The solar atmosphere is so hot that the gas is primarily in a plasma state: electrons are no longer bound to atomic nuclei, and the gas is made up of charged particles (mostly protons and electrons). In this charged state, the solar atmosphere is greatly influenced by the strong solar magnetic fields that thread through it. These magnetic fields, and the outer solar atmosphere (the corona) extend out into interplanetary space as part of the solar wind.
Solar Activity
The Sun is not a quiet place, but one that exhibits sudden releases of energy. One of the most frequently observed events are solar flares: sudden, localized, transient increases in brightness that occur in active regions near sunspots.
Another type of event, the coronal mass ejection, typically disrupt helmet streamers in the solar corona. As much as 1e13 (10,000,000,000,000) kilograms of material can be ejected into the solar wind. Coronal mass ejections propagate out in the solar wind, where they may encounter the Earth and influence geomagnetic activity.
The amount of solar activity on the Sun is not constant, and is closely related to the typical number of sunspots that are visible. The number of sunspots and the levels of solar activity vary with an 11 year period known as the solar cycle.
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Our sun is the closest star to Earth and the source of energy for all life here.The sun is essentially a huge burning ball of gas in the sky only 100 million or so miles from Earth. The majority of gas in the sun is hydrogen and helium, and it is so hot that all of these elements exist in the gaseous state. The gas is held together by gravity, which creates intense heat and pressure in the core. The sun has an interior consisting of the core, radiative zone, and convective zone. It has a visible surface called the photosphere, then the chromosphere, which usually isn't visible, and the very outer layer called the corona.
INNER LAYER
the sun has an inner core. This is where fusion occurs. The core is the very center of the sun where fusion occurs. The core has extremely high temperature and pressure. It is so hot here - 15 million degree Celsius - that nuclear fusion occurs. In the case of our sun, four hydrogen nuclei are fused into one helium nuclei while releasing a bunch of energy as photons. The sun produces so much energy.
The core is the hottest part of the sun and the only part of the sun that produces much energy. The sun cools off as you travel from the core to the outside, with the exception of the chromosphere.
The next layer of the sun is the radiative zone, the layer of the sun directly above the core. This zone, as you can probably guess, emits radiation, and the radiation from the core diffuses out from here. It may take photons millions of years to get out. The next layer as we work our way outward is the convective zone. In this layer, photons produced by fusion in the core make their way to the surface of the sun through convection.
The Solar Atmosphere
The visible solar atmosphere consists of three regions: the photosphere, the chromosphere, and the solar corona. Most of the visible (white) light comes from the photosphere, this is the part of the Sun we actually see. The chromosphere and corona also emit white light, and can be seen when the light from the photosphere is blocked out, as occurs in a solar eclipse. The sun emits electromagnetic radiation at many other wavelengths as well. Different types of radiation (such as radio, ultraviolet, X-rays, and gamma rays) originate from different parts of the sun.
The solar atmosphere is so hot that the gas is primarily in a plasma state: electrons are no longer bound to atomic nuclei, and the gas is made up of charged particles (mostly protons and electrons). In this charged state, the solar atmosphere is greatly influenced by the strong solar magnetic fields that thread through it. These magnetic fields, and the outer solar atmosphere (the corona) extend out into interplanetary space as part of the solar wind.
Solar Activity
The Sun is not a quiet place, but one that exhibits sudden releases of energy. One of the most frequently observed events are solar flares: sudden, localized, transient increases in brightness that occur in active regions near sunspots.
Another type of event, the coronal mass ejection, typically disrupt helmet streamers in the solar corona. As much as 1e13 (10,000,000,000,000) kilograms of material can be ejected into the solar wind. Coronal mass ejections propagate out in the solar wind, where they may encounter the Earth and influence geomagnetic activity.
The amount of solar activity on the Sun is not constant, and is closely related to the typical number of sunspots that are visible. The number of sunspots and the levels of solar activity vary with an 11 year period known as the solar cycle.
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