What is Sun? tell it's shape. what is made up of? it's temperature.
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The Sun is the star at the center of the Solar System. It is a nearly perfect sphere of hotplasma,[14][15] with internal convective motion that generates a magnetic field via a dynamo process.[16] It is by far the most important source of energy for life on Earth. Its diameter is about 1.39 million kilometers, i.e. 109 times that of Earth, and its mass is about 330,000 times that of Earth, accounting for about 99.86% of the total mass of the Solar System.[17] About three quarters of the Sun's mass consists of hydrogen (~73%); the rest is mostly helium (~25%), with much smaller quantities of heavier elements, includingoxygen, carbon, neon, and iron.[18]
The Sun
Sun with sunspots and limb darkening as seen invisible light with solar filter.
Observation dataMean distance
from Earth1 au ≈ 1.496×108 km
8 min 19 s at light speedVisual brightness (V)−26.74[1]Absolute magnitude4.83[1]Spectral classificationG2V[2]MetallicityZ = 0.0122[3]Angular size31.6–32.7 minutes of arc[4]AdjectivesSolarOrbital characteristicsMean distance
from Milky Way core≈ 2.7×1017 km
27,200 light-yearsGalactic period(2.25–2.50)×108 yrVelocity≈ 220 km/s (orbit around the center of the Milky Way)
≈ 20 km/s (relative to average velocity of other stars in stellar neighborhood)
≈ 370 km/s[5] (relative to the cosmic microwave background)Physical characteristicsEquatorial radius695,700 km,[6]
696,392 km[7]
109 × Earth[8]Equatorial circumference4.379×106 km[8]
109 × Earth[8]Flattening9×10−6Surface area6.09×1012 km2[8]
12,000 × Earth[8]Volume1.41×1018 km3[8]
1,300,000 × EarthMass1.9885×1030 kg[1]
333,000 × Earth[1]Average density1.408 g/cm3[1][8][9]
0.255 × Earth[1][8]Center density (modeled)162.2 g/cm3[1]
12.4 × EarthEquatorial surface gravity274 m/s2[1]
28 × Earth[8]Moment of inertia factor0.070[1] (estimate)Escape velocity
(from the surface)617.7 km/s[8]
55 × Earth[8]TemperatureCenter (modeled):1.57×107 K[1]
Photosphere (effective):5,772 K[1]
Corona: ≈ 5×106 KLuminosity (Lsol)3.828×1026 W[1]
≈ 3.75×1028 lm
≈ 98 lm/W efficacyMean radiance (Isol)2.009×107 W·m−2·sr−1Age≈ 4.6 billion years[10][11]Rotation characteristicsObliquity7.25°[1]
(to the ecliptic)
67.23°
(to the galactic plane)Right ascension
of North pole[12]286.13°
19 h 4 min 30 sDeclination
of North pole+63.87°
63° 52' NorthSidereal rotation period
(at equator)25.05 d[1](at 16° latitude)25.38 d[1]
25 d 9 h 7 min 12 s[12](at poles)34.4 d[1]Rotation velocity
(at equator)7.189×103 km/h[8]Photospheric composition (by mass)Hydrogen73.46%[13]Helium24.85%Oxygen0.77%Carbon0.29%Iron0.16%Neon0.12%Nitrogen0.09%Silicon0.07%Magnesium0.05%Sulfur0.04%
The Sun is a G-type main-sequence star (G2V) based on its spectral class. As such, it is informally and not completely accurately referred to as a yellow dwarf (its light is closer to white than yellow). It formed approximately 4.6 billion[a][10][19] years ago from the gravitational collapse of matter within a region of a large molecular cloud. Most of this matter gathered in the center, whereas the rest flattened into an orbiting disk that became the Solar System. The central mass became so hot and dense that it eventually initiated nuclear fusion in its core. It is thought that almost all stars form by this process.
The Sun is roughly middle-aged; it has not changed dramatically for more than four billion[a] years, and will remain fairly stable for more than another five billion years. It currently fuses about 600 million tons ofhydrogen into helium every second, converting 4 million tons of matter into energy every second as a result. This energy, which can take between 10,000 and 170,000 years to escape from its core, is the source of the Sun's light and heat. In about 5 billion years, whenhydrogen fusion in its core has diminished to the point at which the Sun is no longer inhydrostatic equilibrium, the core of the Sun will experience a marked increase in density and temperature while its outer layers expand to eventually become a red giant. It is calculated that the Sun will become sufficiently large to engulf the current orbits of Mercury and Venus, and render Earthuninhabitable. After this, it will shed its outer layers and become a dense type of cooling star known as a white dwarf, which no longer produces energy by fusion, but still glows and gives off heat from its previous fusion.
The enormous effect of the Sun on Earth has been recognized since prehistoric times, and the Sun has been regarded by some culturesas a deity. The synodic rotation of Earth and its orbit around the Sun are the basis of solar calendars, one of which is the predominantcalendar in use today.
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The Sun
Sun with sunspots and limb darkening as seen invisible light with solar filter.
Observation dataMean distance
from Earth1 au ≈ 1.496×108 km
8 min 19 s at light speedVisual brightness (V)−26.74[1]Absolute magnitude4.83[1]Spectral classificationG2V[2]MetallicityZ = 0.0122[3]Angular size31.6–32.7 minutes of arc[4]AdjectivesSolarOrbital characteristicsMean distance
from Milky Way core≈ 2.7×1017 km
27,200 light-yearsGalactic period(2.25–2.50)×108 yrVelocity≈ 220 km/s (orbit around the center of the Milky Way)
≈ 20 km/s (relative to average velocity of other stars in stellar neighborhood)
≈ 370 km/s[5] (relative to the cosmic microwave background)Physical characteristicsEquatorial radius695,700 km,[6]
696,392 km[7]
109 × Earth[8]Equatorial circumference4.379×106 km[8]
109 × Earth[8]Flattening9×10−6Surface area6.09×1012 km2[8]
12,000 × Earth[8]Volume1.41×1018 km3[8]
1,300,000 × EarthMass1.9885×1030 kg[1]
333,000 × Earth[1]Average density1.408 g/cm3[1][8][9]
0.255 × Earth[1][8]Center density (modeled)162.2 g/cm3[1]
12.4 × EarthEquatorial surface gravity274 m/s2[1]
28 × Earth[8]Moment of inertia factor0.070[1] (estimate)Escape velocity
(from the surface)617.7 km/s[8]
55 × Earth[8]TemperatureCenter (modeled):1.57×107 K[1]
Photosphere (effective):5,772 K[1]
Corona: ≈ 5×106 KLuminosity (Lsol)3.828×1026 W[1]
≈ 3.75×1028 lm
≈ 98 lm/W efficacyMean radiance (Isol)2.009×107 W·m−2·sr−1Age≈ 4.6 billion years[10][11]Rotation characteristicsObliquity7.25°[1]
(to the ecliptic)
67.23°
(to the galactic plane)Right ascension
of North pole[12]286.13°
19 h 4 min 30 sDeclination
of North pole+63.87°
63° 52' NorthSidereal rotation period
(at equator)25.05 d[1](at 16° latitude)25.38 d[1]
25 d 9 h 7 min 12 s[12](at poles)34.4 d[1]Rotation velocity
(at equator)7.189×103 km/h[8]Photospheric composition (by mass)Hydrogen73.46%[13]Helium24.85%Oxygen0.77%Carbon0.29%Iron0.16%Neon0.12%Nitrogen0.09%Silicon0.07%Magnesium0.05%Sulfur0.04%
The Sun is a G-type main-sequence star (G2V) based on its spectral class. As such, it is informally and not completely accurately referred to as a yellow dwarf (its light is closer to white than yellow). It formed approximately 4.6 billion[a][10][19] years ago from the gravitational collapse of matter within a region of a large molecular cloud. Most of this matter gathered in the center, whereas the rest flattened into an orbiting disk that became the Solar System. The central mass became so hot and dense that it eventually initiated nuclear fusion in its core. It is thought that almost all stars form by this process.
The Sun is roughly middle-aged; it has not changed dramatically for more than four billion[a] years, and will remain fairly stable for more than another five billion years. It currently fuses about 600 million tons ofhydrogen into helium every second, converting 4 million tons of matter into energy every second as a result. This energy, which can take between 10,000 and 170,000 years to escape from its core, is the source of the Sun's light and heat. In about 5 billion years, whenhydrogen fusion in its core has diminished to the point at which the Sun is no longer inhydrostatic equilibrium, the core of the Sun will experience a marked increase in density and temperature while its outer layers expand to eventually become a red giant. It is calculated that the Sun will become sufficiently large to engulf the current orbits of Mercury and Venus, and render Earthuninhabitable. After this, it will shed its outer layers and become a dense type of cooling star known as a white dwarf, which no longer produces energy by fusion, but still glows and gives off heat from its previous fusion.
The enormous effect of the Sun on Earth has been recognized since prehistoric times, and the Sun has been regarded by some culturesas a deity. The synodic rotation of Earth and its orbit around the Sun are the basis of solar calendars, one of which is the predominantcalendar in use today.
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jannatkhan52130:
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the sun is a star in the solar system in the milky way galaxy. the sun is the biggest star in the solar system. the sun is made up
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