History of The Sun

History of The Sun

• 1. History of The Sun History of The Sun
• 2. History of The Sun The sun is situated in the very centre of the solar system, the largest universe to date. It accounts for about 99.8 per cent of the mass of the solar system, and roughly one million times the world wide, roughly a million times the Earth. History of The Sun
• 3. History of The Sun It is thought that the visible part of the sun can be equal to 10,000 degrees Fahrenheit (5.500 degrees Celsius degrees) and the core temperature is equal to nuclear reactions. It is estimated to reach 27 million F (15 million C). According to NASA, the sun needs to be matched with the energy produced by 100 billion tonnes of dynamite per second. History of The Sun
• 4. Formation & Evolution It is estimated that the sun appeared or was born 4.6 billion years ago. Many scientists think that the sun and the rest of the solar system are made up of a giant, rotating gas cloud known as the sun cloud. Most of the clouds in the atmosphere were drawn into the center of the sun. The sun can produce and explode enough fuel for billions of years. Formation & Evolution
• 5. Internal Structure and Atmosphere Internal Structure and Atmosphere The sun and its surrounding atmosphere are divided into compartments, layers, and zones. The solar core radiation zone consists of the transport and spraying zone. Beyond that, the solar wind comes out of the corona with its own gas output.
• 6. Internal Structure and Atmosphere It is estimated that the core of the sun can be reached from the full inner centre to the top of one-third of the surface. Although the core constitutes only 6 per cent of the molar volume, it is almost 7 times the lead density and almost a quarter of the solar mass. The radiation zone, which then forms 40 percent of the solar volume and 24 percent of its mass, extending from the core to the 40 per cent of the road to the sun's surface. The light from the core begins to disintegrate and disintegrate as soon as it enters this region so that a single photon can take millions of years to pass. Internal Structure and Atmosphere
• 7. Internal Structure and Atmosphere The convection zone extends to the sun's surface and tries to reach half of the sun, and when doing so, it occupies 33% of the sun's surroundings, but only a little more than 2 percent of its mass. Gas "convection cells" dominate this region. It is estimated that two main types of solar convection cells, a granulation cell of approximately 300 miles (500 kilometers) wide and about 10,000 miles (15,000 km) of supergranulation cells. Internal Structure and Atmosphere
• 8. Internal Structure and Atmosphere The sphere of light is the basis of the atmosphere created by the sun itself and emits light and ray bursts coming into the world. Although most of the light comes from the lowest third, it is about 150 miles (250 km) thick. Temperatures in the photosphere are between 6,000 F (4,135 C) and 5,460 F (2,125 C). Then there is the chromosphere at a temperature of about 15,500 F (9,725 C) and a temperature of about 300 miles (500 km) and a height of 3,000 miles (5000 km). According to these data, it is still unclear whether to send warm beam waves to the world from such a distant distance. Internal Structure and Atmosphere
• 9. Internal Structure and Atmosphere After that, the transition zone of several hundred to several thousand kilometres thick is heated by the corona on its top and keeps most of its light as ultraviolet rays. Internal Structure and Atmosphere
• 10. Internal Structure and Atmosphere At the top, there is a super hot corona consisting of structures such as loops and ionized gas streams. The corona is generally between 900,000 F (500,000 C) and 10.8 million F (6 million C) and can reach tens of millions of degrees when a sunburst occurs. The substance in the corona is blown up like solar wind. Internal Structure and Atmosphere
• 11. Magnetic Field Magnetic Field
• 12. Magnetic Field The force of the magnetic field of the sun is typically twice as much as that of the Earth. However, in small areas, it becomes more intense than normal and becomes 3,000 times more powerful. These flexes and bending in the magnetic field develop because the sun rotates faster in the equator than in the higher latitudes, and the sun's interior rotates faster than the surface. Magnetic Field
• 13. Magnetic Field Magnetic Field These distortions create a variety of features ranging from sunspots to flares and spectacular explosions are known as coronal mass castings. Flares are the most severe eruptions in the solar system, but coronal mass excretions are less severe, but a single ejection with an extraordinary amount of substances can throw roughly 20 billion tonnes (18 billion metric tons) of material into space.
• 14. Thank You Thank You