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Presentation on the topic: “Internal structure of the Sun” Completed by a student of class 11 “a” GBOU secondary school 1924 Governors AntonSlide 2
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The Sun is the only star in the Solar System around which other objects of this system revolve: planets and their satellites, dwarf planets and their satellites, asteroids, meteoroids, comets and cosmic dust.
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Structure of the Sun: -Solar core. -Zone of radiative transfer. -Convective zone of the Sun.
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Solar core. The central part of the Sun with a radius of approximately 150,000 kilometers, in which thermonuclear reactions occur, is called the solar core. The density of the substance in the core is approximately 150,000 kg/m³ (150 times higher than the density of water and ~6.6 times higher than the density of the densest metal on Earth - osmium), and the temperature in the center of the core is more than 14 million degrees.
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Radiative transfer zone. Above the core, at distances of about 0.2-0.7 solar radii from its center, there is a radiative transfer zone in which there are no macroscopic movements; energy is transferred using photon re-emission.
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Convective zone of the Sun. Closer to the surface of the Sun, vortex mixing of the plasma occurs, and the transfer of energy to the surface is accomplished primarily by the movements of the substance itself. This method of energy transfer is called convection, and the subsurface layer of the Sun, approximately 200,000 km thick, where it occurs is called the convective zone. According to modern data, its role in the physics of solar processes is exceptionally great, since it is in it that various movements of solar matter and magnetic fields originate.
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Photosphere of the Sun. The photosphere (the layer that emits light) forms the visible surface of the Sun, from which the size of the Sun, the distance from the surface of the Sun, etc. are determined. The temperature in the photosphere reaches an average of 5800 K. Here, the average gas density is less than 1/1000 of the density of the earth's air.
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Chromosphere of the Sun. The chromosphere is the outer shell of the Sun, about 10,000 km thick, surrounding the photosphere. The origin of the name of this part of the solar atmosphere is associated with its reddish color. The upper boundary of the chromosphere does not have a distinct smooth surface; hot emissions called spicules constantly occur from it. The temperature of the chromosphere increases with altitude from 4000 to 15,000 degrees.
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Solar core The central part of the Sun with a radius of approximately kilometers, in which thermonuclear reactions occur, is called the solar core. The density of the substance in the core is approximately kg/m³.
Chromosphere of the Sun The chromosphere of the Sun (colored sphere) is a dense layer (km) of the solar atmosphere, which is located directly behind the photosphere. The chromosphere is quite problematic to observe due to its close location to the photosphere. It is best seen when the Moon covers the photosphere, i.e. during solar eclipses.
Solar prominences Solar prominences are huge emissions of hydrogen that resemble long luminous filaments. The prominences rise to enormous distances, reaching the diameter of the Sun (1.4 million km), move at a speed of about 300 km/sec, and the temperature reaches degrees.
Solar core. The central part of the Sun with a radius of approximately kilometers, in which thermonuclear reactions occur, is called the solar core. The density of the material in the core is approximately kg/m³ (150 times the density of water and ~6.6 times the density of the densest metal on Earth, osmium), and the temperature in the center of the core is more than 14 million degrees.
Convective zone of the Sun. Closer to the surface of the Sun, vortex mixing of the plasma occurs, and the transfer of energy to the surface is accomplished primarily by the movements of the substance itself. This method of energy transfer is called convection, and the subsurface layer of the Sun, approximately km thick, where it occurs is the convective zone. According to modern data, its role in the physics of solar processes is exceptionally great, since it is in it that various movements of solar matter and magnetic fields originate.
Photosphere of the Sun. The photosphere (the layer that emits light) forms the visible surface of the Sun, from which the size of the Sun, the distance from the surface of the Sun, etc. are determined. The temperature in the photosphere reaches an average of 5800 K. Here, the average gas density is less than 1/1000 of the density of the earth's air.
Chromosphere of the Sun. The chromosphere is the outer shell of the Sun, about km thick, surrounding the photosphere. The origin of the name of this part of the solar atmosphere is associated with its reddish color. The upper boundary of the chromosphere does not have a distinct smooth surface; hot emissions called spicules constantly occur from it. The temperature of the chromosphere increases with altitude from 4000 to degrees.
Crown of the Sun. The corona is the last outer shell of the Sun. Despite its very high temperature, from up to degrees, it is visible to the naked eye only during a total solar eclipse.
“Stars and Constellations” - Ptolemy. On a cloudless and moonless night, far from populated areas, about 3,000 stars can be distinguished. Calf. Ancient astronomers divided the starry sky into constellations. It is easy to determine the northern direction from the Ursa Major bucket. Starry sky. Whale. Images of constellations from the ancient atlas of Hevelius.
“The Evolution of Stars” - Stars are huge balls of helium and hydrogen, as well as other gases. Stars are the main element of the galaxy. Supernova explosion. A graph of the evolution of a typical star. Two young black dwarfs in the constellation Taurus. Crab Nebula. As the density of the cloud increases, it becomes opaque to radiation.
“Starry Sky” - Letters of the Greek alphabet. Ursa Major Bucket. Winter triangle. Johann Bayer. A section of the celestial sphere. Starry sky. North hemisphere. Celestial sphere. Stars. Ancient astronomers. Constellation Ursa Major. The stars were the main landmarks. Bright stars. Constellation images. Bright stars.
“Structure of stars” - Masse. Age. For different stars, the maximum radiation occurs at different wavelengths. Color and temperature of stars. White - blue. Luminosity of stars. Yellow - white. Stars come in a variety of colors. Class. Stars. Arcturus has a yellow-orange hue, Carrot. Vega. Rigel. One. Radii of stars. Antares. The building.
"Black holes" - Small consequences of the appearance of black holes. When a star explodes, a supernova occurs. Astronomer Karl Schwarzschild, in the last years of his life, calculated the gravitational field around a mass of zero volume. Black holes are the end result of the activity of stars whose mass is five or more times greater than that of the Sun.
“Distances to the stars” - Distances to the stars. Using spectral lines, you can estimate the luminosity of a star and then find its distance. Telescope studies show that no two stars are alike. The distance to stars can be estimated using the spectral parallax method. Stars differ from each other in color and shine.
There are a total of 17 presentations in the topic
Presentation on the topic: “Internal structure of the sun” Completed by a student of class 11 “a” GBOU secondary school 1924 Governors Anton
Internal structure of the Sun.
The Sun is the only star in the Solar System around which other objects of this system revolve: planets and their satellites, dwarf planets and their satellites, asteroids, meteoroids, comets and cosmic dust.
Structure of the Sun: -Solar core. -Zone of radiative transfer. - Convective zone of the Sun.
Solar core. The central part of the Sun with a radius of approximately 150,000 kilometers, in which thermonuclear reactions occur, is called the solar core. The density of the substance in the core is approximately 150,000 kg/m³ (150 times higher than the density of water and ~6.6 times higher than the density of the densest metal on Earth - osmium), and the temperature in the center of the core is more than 14 million degrees.
Radiative transfer zone. Above the core, at distances of about 0.2-0.7 solar radii from its center, there is a radiative transfer zone in which there are no macroscopic movements; energy is transferred using photon re-emission.
Convective zone of the Sun. Closer to the surface of the Sun, vortex mixing of the plasma occurs, and the transfer of energy to the surface is accomplished primarily by the movements of the substance itself. This method of energy transfer is called convection, and the subsurface layer of the Sun, approximately 200,000 km thick, where it occurs is called the convective zone. According to modern data, its role in the physics of solar processes is exceptionally great, since it is in it that various movements of solar matter and magnetic fields originate.
Atmosphere of the Sun: -Photosphere. -Chromosphere. -Crown. -Sunny wind.
Photosphere of the Sun. The photosphere (the layer that emits light) forms the visible surface of the Sun, from which the size of the Sun, the distance from the surface of the Sun, etc. are determined. The temperature in the photosphere reaches an average of 5800 K. Here, the average gas density is less than 1/1000 of the density of the earth's air.
Chromosphere of the Sun. The chromosphere is the outer shell of the Sun, about 10,000 km thick, surrounding the photosphere. The origin of the name of this part of the solar atmosphere is associated with its reddish color. The upper boundary of the chromosphere does not have a distinct smooth surface; hot emissions called spicules constantly occur from it. The temperature of the chromosphere increases with altitude from 4000 to 15,000 degrees.
Crown of the Sun. The corona is the last outer shell of the Sun. Despite its very high temperature, ranging from 600,000 to 5,000,000 degrees, it is only visible to the naked eye during a total solar eclipse.
Sunny wind. Many natural phenomena on Earth are associated with disturbances in the solar wind, including geomagnetic storms and auroras.
