Sun

   

The sun or the sun located in the center of the solar system, which surrounds the earth and other components of the solar system. Sun is the largest body of our solar system and its diameter is approximately 13 lakh 90 thousand kilometers which is almost 9 9 times higher than the Earth. This powerful reservoir of energy is mainly a huge circle of hydrogen and helium gases. Through the process of nuclear merger, the sun produces energy in its center. Only a small portion of the energy released from the sun reaches the Earth, of which 15 percent is reflected in the space, 30 percent water is used to make the steam, and many energy plants and plants absorb the sea. Its strong gravitational force keeps the earth and other planets moving around in different classes.

The average distance of the Earth from the Sun is approximately 14,96,00,000 kilometers, or 9, 29, 60,000 miles, and it takes 8.3 minutes for the sun to reach the Earth. From this same optical energy there is an important biochemical reaction called light-synthesis, which is the basis of life on Earth. It affects the climate and climate of the earth. Sun surface is formed from hydrogen, helium, iron, nickel, oxygen, silicon, sulfur, magnesium, carbon, neon, calcium, chromium elements. Of these, hydrogen is 74% of Sun's surface amount and Hilium is 24%.

Seeing this greasy gaseous object with a telescope, small spots appear on its surface. These are called solar stigma. These stigmas are seen moving from their places. With this, scientists have concluded that the Sun takes a rotation from the east to the west on 27 days in its axis. Just as the Earth and the other planets revolve around the Sun, so the sun revolves around the center of the galaxy. [[It takes 22 to 25 million years to revolve, it is also called an Niharika year. The orbital speed is 251 kilometers per second.

Attributes Play media This video takes images of the Solar Dynamics Observatory and applies additional procedures to increase the visibility of the structure. This event provides 24 hours of activity on September 25, 2011 in this video.

Sun is a G-type main sequence star that comprises approximately 99.86% of the total mass of the solar system. With the approximate flattening of about ninety million parts, it is nearly circular, it means its polar diameter is different from only 10 km from its equatorial diameter. As the Sun is made of plasma and not solid, it rotates more quickly on its equator than on its poles. This behavior is known as the internal rotation and is caused by the movement of the material due to the convection of the sun and the extreme temperature slope towards the outside of the core. It carries a large part of the angular momentum of the Sun's counter-clockwise, as seen from the North Pole of the ecliptic and thus the angular velocity is redistributed. The duration of this actual rotation is approximately 25.6 days on the equator and 33.5 days in the poles. However, due to our continuously changing position relative to the Earth, along with the Sun's orbiting, this star has a clear rotation on its equator for about 28 days. The centrifugal effect of rotation of this slow motion is 1.8 million times weak with the surface gravity of the sun's equator. Tidal effects of the planets are also weak and do not affect the size of the sun.

Sun is a population I or a star with heavy elements. This formation of the Sun may have been initiated by arched waves originating from one or more of the supernovas. In such a so-called Population II (heavy element-deprivation) stars, the abundance of these elements has been suggested by the high abundance of heavy elements in the solar system, such as gold and uranium. This element is most likely to be produced during a supernova, by conversion of heat-inducing neural reactions or by conversion through neutron absorption within a second-generation universe.

There is no fixed limit on the mass of the rocky planets of the sun. The density of gases in the outer parts of the sun drops rapidly along its growing distance from its center. Nonetheless, it has an well-defined internal structure that is described below. The radius of the Sun is measured from its center to the side of the halo. The outer halo of the Sun is the visible final layer. Layers of this above are quite cool or very thin in order to emit sufficient light to show naked eyes. During a complete solar eclipse, however, when the halo was hidden by the moon, the Corona of the sun can be easily seen around it.

The interior of the sun is not directly observable. The sun itself is opaque for electromagnetic radiation. However, just as earthquake science uses waves generated from earthquake to reveal the internal formation of the Earth, the rule of solar earthquake science uses pressure waves to make the inner structure of this star measurable and visible. . Computer modeling is also used as theoretical tool for exploring its deeper layers. Corner Main article: Solar core Sun formation

The Sun's core is thought to be extended from its center to about 20-25% of the solar radius. Its density is 150 g / cm (approximately 150 times the density of water) and the temperature is close to 15.7 million Kelvin. On the contrary, the temperature of the Sun's surface is approximately 5,800 Kelvin. Recent analyzes of SOHO mission data favor the sharp rotation rate of the core compared to the rest of the radiation area. In most of the sun's life, energy is produced by nuclear fusion through a phase series called p-p (proton-proton) series; This process converts hydrogen into helium. Only 0.8% of the sun's energy produced comes from the CNO cycle.

Core in the sun is the only area that produces a large amount of thermal energy through fusion; 99% of the energy is generated within 24% of the radius of the sun, and 30% of the radius has almost completely closed the fusion. The remainder of this star is scorched by the energy that is transferred from outside the core to the radius outside the core just to the vascular layers. The energy produced by the fusion in the core is then progressively progressed through many layers to the solar aura, before it sun rises or moves into space in the form of kinetic energy of particles.

The proton-proton series in the core is found every second 9.2 × 10 times. This reaction uses four free protons (hydrogen nuclei), it converts about 3.7 × 10 protons into alpha particles (helium nuclei) every second (of the Sun's total ~ 8.9 × 10 free protons), or approximately 6.2 × 10 kg per second. After helium fusion from hydrogen releases about 0.7% of the melt mass in the form of helium energy, the sun emits energy at a mass-energy conversion rate of 42.6 million metric tons per second, 384.6 yota watts (3.846 × 10 watts), or 9.192 × 10 TNT megaton per second. The amount is not destroyed in generating energy, but this amount has been transformed into equal energy and the transport was taken away to be emitted as the mass-energy equivalence concept has been described.

The power of the fusion in the core varies with the distance from the solar center. At the center of the Sun, it is approximately 276.5 watts / meter in the assessment of theoretical models, Life Cycle Main article: Formation and development of solar system and development of stars

Sun is almost halfway to its life in the most stable state. There has not been a dramatic change for several billion years, and it will remain unchanged for the next several years. However, the earlier and later star of a steady hydrogen-combustion period is very different. Life cycle of the sun Construction

The sun has formed around 4.57 billion years ago, which is mostly made of hydrogen and helium, and has created many other stars. This age has been assessed through the use of computer models of stellar evolution and through nucleocomoscopy. The result corresponds to the radiometric date of the oldest solar system, 4.567 billion years. Studies of ancient meteorites show signs of a stable nucleus of a short-lived isotope, such as iron-60, which is produced only in explosive, short-lived stars. This indicates that one or more supernovas must be found near the place where the Sun is formed. The shock wave from a nearby supernovae would have started composing the sun by compressing the gases within the molecular cloud and some areas would have been formed under the collapse of its own gravitational collapse. As soon as a fragment of the cloud started to rotate due to the protection of the collapsed angular momentum and he started getting hot with increasing pressure. Very large amount of money was concentrated in the center, while the rest turned outward and turned into a disc that made the planet and other solar system. Gravity and pressure within the core of the cloud produced excessive heat, so much gas was added around the disk, eventually activating nuclear fusion. Thus, the sun was born. Main sequence The sun's brightness, radius and the development of effective temperature compared to the current sun

Sun is about halfway through its main sequence stage, during which the nuclear fusion reaction turns hydrogen into helium. Every second, within the core of the Sun, more than four million tons of substances have been converted into energy and have formed neutrinos and solar radiation. At this rate, the Sun has so far converted as much as 100 Earth masses into energy. The sun will spend about 10 billion years in the form of a main sequence star. After core hydrogen closure

There is not enough mass for the explosion in the form of a supernova near the sun. Although it will enter a red demon stage. Sun is predicted to become a red demon in about 5.4 billion years. It is estimated that the Sun will probably be as big as swallowing the current orbits of the solar system with the Earth. The size of the current sun (currently in the main sequence) is in the future compared to its estimated size during its red demon phase

Before it becomes a red demon, the brightness of the sun will almost double and the earth will become more warmer than it is today. Once the core hydrogen is finished, the Sun's sub-stage phase will expand and will gradually double in size after half a billion years. After that, it will spread more quickly for more than half a billion years, until it is two hundred times bigger than the present day and ten thousand times more bright. This is the phase of the Red Demon branch, where the Sun has spent about one billion years and lost one third of its mass around.

The sun has only a few hundred thousand years left, but it is very interesting. First, the core helium flows fast in the glow and the sun shrinks back to about 10 times its size, with a little less temperature than today, with 50 times the sunlight. Solar space mission : Solar Observatory 13 Mar 2012 13:29, EST is a large geomagnetic storm outside the Sun Play media Ultraviolet imaging of stereo B is a moon transit captured in camera during detection

The first satellite designed for the inspection of the Sun was Pioneer 5, 6, 7, 8 and 9 of NASA. It was launched between 1959 and 1968. These orbes were the first detailed measurements of the solar wind and solar magnetic field while orbiting the Sun in equal orbital orbit of the Earth and the Sun. Pioneer 9 was specially operated for a long time and continued to transmit data by May 1983.

In the 1970s, two spacecraft Helios and Skylab Apollo Telescope Mount provided the important new data scientists of Solar Wind and Solar Corona. Helios 1 and 2 were US-Germany cooperation. It studied solar wind from the orbit moving towards spacecraft within the orbit of Mercury. In 1973 the SkyLab Space Station was launched by NASA. It included a solar observatory module called Apollo Telescope Mount, which was operated by astronauts living at the station. Skylab first solved the ultraviolet emission from the solar transit region and the solar corona. Searches included the first observation of coronal mass ajaxan, which is then called "coronal transistor" and then called coronal holes, is now widely known to be connected with solar wind.

The Solar Maximam Mission of 1980 was started by NASA. This spacecraft was created for the inspection of ultraviolet radiation from gamma rays, X-rays and solar flames during the time of high solar activity and solar glow. Just a few months after the launch, however, due to an electronics fault, the vehicle continued to be in taut condition and spent the next three years in this idle state. In 1984, Space Shuttle Challenger Mission STS-41C improved the satellite and repaired its electronics before leaving it again in the classroom. Before re-entering the Earth's atmosphere in June 1989, Solar Maximam Mission acquired thousands of images of solar corona after repair.

Yonkoh (solar mass) satellite of Japan, launched in 1991, observed solar flames on X-ray wavelength. Mission data allowed scientists to identify different types of flames, as well as shown that the corona was far more dynamic and active than areas with extreme activity, as was previously believed. Yonkoh observes a whole solar cycle, but in 2001, when an annular solar eclipse occurred, it went in a favorable state, due to which it damaged the connection with the Sun. It was destroyed during the atmospheric re-entry in 2005.

The most important solar mission till date has been Solar and Heliosporic Observatory. The mission, which started on December 2, 1995, was jointly created by the European Space Agency and NASA. Originally it was fixed for a two-year mission. The expansion of the mission till 2012 was approved in October 2009. It proved to be so useful that its follow-up mission Solar Dynamics Observatory (SDO) was launched in February, 2010. It was established between the Earth and the Sun on the Lagrangian point (on which the gravitational pull of both sides is equal). Soho has provided a continuous image of the sun on many wavelengths since its launch. In addition to direct solar observation, Soho has been able to discover a large number of comets, most of them are small sunken small comets which are consumed by passing through the sun. A solar eclipse emerging in August 2012, taken by NASA's Solar Activity Observatory

All these satellites have observed the Sun at the bottom of the ecliptic, so observations have been done in the expansion of its equatorial areas. The Ulysses Yan was launched in 1990 for the study of the polar regions of the Sun. It first traveled to Jupiter, before it was taken on the basis of Jupiter's gravitational force in a distant orbit above the ecliptic plane. Coincidentally, this was a good place to observe the collision of the Comet Schumacher-Levi 9 with Jupiter of 1994. Once the Ulysses was installed in its fixed orbit, it began to inspect the solar wind and magnetic field power of high solar latitudes and found that solar wind rising above 750 km / second on high latitudes was less slower than expected. It was also found that there was a large magnetic wave coming from high latitudes that had scattered galactic cosmic rays.

The elemental abundance of the chlorophyll is well known by spectroscopy studies, but the understanding of the inner structure of the sun is equally bad. Solar Air Sample Reflection Mission, Genesis, was created by astronomers to measure the structure of solar material directly. Genesis returned to Earth in 2004, but on the deployment of the Earth's atmosphere, it was accidentally damaged by the failure of the parachute while re-entering. Despite serious damage, some useful samples have been recovered from the sample return module of the space shuttle and are undergoing an analysis.

The Solar Terrestrial Relations Observatory (Stereo) mission was started in October 2006. Two of the same spacecraft were launched in classrooms in such a way that they (rotate) dragged them far forward and gradually dropped behind the earth. It is capable of stereoscopic mapping of the sun and solar phenomena, such as the coronal mass agax.

Indian Space Research Organization has set a launch of a 100 kg satellite named Aditya from 2015-16. Its main means of studying the mobility of Solar Corona will be a Coronagraph. Also see them

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