THE SUN
Hi there and welcome in today’s article we will be looking at some of the fun facts about our sun. The Sun, like all stars, is an enormous ball of extremely hot, largely ionized gas, shining under its power. And we do mean enormous. The Sun is the star at the center of the Solar System. It is a nearly perfect ball of hot plasma, heated to incandescence by nuclear fusion reactions in its core, radiating the energy mainly as visible light, ultraviolet light, and infrared radiation. It is by far the most important source of energy for life on Earth. The Sun is the only star in our solar system. It is the center of our solar system, and its gravity holds the solar system together. Everything in our solar system revolves around it – the planets, asteroids, comets, and tiny bits of space debris.
The Sun does not have a solid surface or continents like Earth, nor does it have a solid core. However, it does have a lot of structure and can be discussed as a series of layers, not unlike an onion. In this section, we describe the huge changes that occur in the Sun’s extensive interior and atmosphere, and the dynamic and violent eruptions that occur daily in its outer layers. The Sun could fit 109 Earths side-by-side across its diameter, and it has enough volume (takes up enough space) to hold about 1.3 million Earths.
Here we will look at some of the fun facts about the sun;
The sun is made up of mostly hydrogen and helium
The sun is huge but tiny
The sun is middle-aged
The sun has layers
The sun is heating up and will kill all life on earth
Different parts of the sun rotate at different speeds
The outer atmosphere is hotter than the surface
I know some are confused about some of the facts written above but don’t worry I will clear up those confusions in this article. so let's get right into it.
THE COMPOSITION OF THE SUN
Just like most other stars, the sun is made up mostly of hydrogen, followed by helium. Nearly all the remaining matter consists of seven other elements — oxygen, carbon, neon, nitrogen, magnesium, iron, and silicon. For every 1 million atoms of hydrogen in the sun, there are 98,000 helium, 850 oxygen, 360 carbon, 120 neon, 110 Rogen, 40 magnesium, 35 iron, and 35 silicon. Still, hydrogen is the lightest of all elements, so it only accounts for roughly 72% of the sun's mass, while helium makes up about 26%.
The sun's magnetic field is typically only about twice as strong as Earth's magnetic field. However, it becomes highly concentrated in small areas, reaching up to 3,000 times stronger than usual. These kinks and twists in the magnetic field develop because the sun spins more rapidly at the equator than at higher latitudes and because the inner parts of the sun rotate more quickly than the surface.
The Sun is classified as a G2 V star, with G2 standing for the second hottest of the yellow G class—with a face temperature of about 5,800 kelvins (K)—and the V representing a mathen sequence, or dwarf, star, the typical star for this temperature class. (G stars are so called because of the prominence of a band of atomic and molecular spectral lines that the German physicist Joseph von Fraunhofer designated G.) The Sun exists in the outer part of the Milky Way Galaxy and was formed from material rial that had been processed inside a supernova. The Sun is not, as is often said, a small star. Although it falls midway between the biggest and smallest stars of its type, there are so many dwarf stars that the Sun falls in the top 5 percent of stars in the neighborhood that immediately surrounds it.
The radius of the Sun, R☉, is 109 times that of Earth, but its distance from Earth is 215 R☉, so it subtends an angle of only 1/2° in the sky, roughly the same as that of the Moon. By comparison, Proxima Centauri, the next closest star to Earth, is 250,000 times farther away, and its relative apparent brightness is reduced by the square of that ratio or 62 billion times. The temperature of the Sun’s surface is so high that no solid or liquid can exist there; the constituent materials are predominantly gaseous atoms, with a very small number of molecules. As a result, there is no fixed surface. The surface viewed from Earth, called the photosphere, is the layer from which most of the radiation reaches us; the radiation from below is absorbed and reradiated, and the emission from overlying layers drops sharply, by about a factor of six every 200 kilometers (124 miles). The Sun is so far from Earth that this slightly fuzzy surface cannot be resolved, and so the limb (the visible edge) appears sharp. The orbits of the planets and other elements of the solar system, including asteroids, Kuiper belt, Oort cloud, comet
THE SUN IS HUGE BUT TINY
The mass of the Sun, M☉, is 743 times the total mass of all the planets in the solar system and 330,000 times that of Earth. All the interesting planetary and interplanetary gravitational phenomena are negligible effects in comparison to the force exerted by the Sun. Under the force of gravity, the great mass of the Sun presses inward, and to keep the star from collapsing, the central pressure outward must be great enough to support its weight. The density at the Sun’s core is about 100 times that of water (roughly six times that at the center of Earth), but the temperature is at least 15,000,000 K, so the central pressure is at least 10,000 times greater than that at the center of Earth, which is 3,500 kilobars. The nuclei of atoms are completely stripped of their electrons, and at this high temperature, they collide to produce the nuclear reactions that are responsible for generating the energy vital to life on Earth. The mass of the Sun, M☉, is 743 times the total mass of all the planets in the solar system and 330,000 times that of Earth. All the interesting planetary and interplanetary gravitational phenomena are negligible effects in comparison to the force exerted by the Sun. Under the force of gravity, the great mass of the Sun presses inward, and to keep the star from collapsing, the central pressure outward must be great enough to support its weight. The density at the Sun’s core is about 100 times that of water (roughly six times that at the center of Earth), but the temperature is at least 15,000,000 K, so the central pressure is at least 10,000 times greater than that at the center of Earth, which is 3,500 kilobars. The nuclei of atoms are completely stripped of their electrons, and at this high temperature, they collide to produce the nuclear reactions that are responsible for generating the energy vital to life on Earth. The sun's circumference is about 2,715,396 miles (4,370,006 km) It may be the biggest thing in this neighborhood, but the sun is just average compared to other stars. Betelgeuse, a red giant, is about 700 times bigger than the sun and about 14,000 times brighter "We have found stars that are 100 times bigger in diameter than our sun. Truly those stars are enormous, "We have also seen stars that are just a tenth the size of our sun." This is what is meant by the sun being huge but tiny.
THE SUN HAS LAYER
There are 7 layers of the sun but we will not be looking at all 7 of them we will only be discussing four very important layers.
Photosphere - The photosphere is the deepest layer of the Sun that we can observe directly. It reaches from the surface visible at the center of the solar disk to about 250 miles (400 km) above that. The temperature in the photosphere varies between about 6500 K at the bottom and 4000 K at the top (11,000 and 6700 degrees F, 6200 and 3700 degrees C). Most of the photosphere is covered by granulation.
Chromosphere - The chromosphere is a layer in the Sun between about 250 miles (400 km) and 1300 miles (2100 km) above the solar surface (the photosphere). The temperature in the chromosphere varies between about 4000 K at the bottom (the so-called temperature minimum) and 8000 K at the top (6700 and 14,000 degrees F, 3700 and 7700 degrees C), so in this layer (and higher layers) it gets hotter if you go further away from the Sun, unlike in the lower layers, where it gets hotter if you go closer to the center of the Sun.
Transition Region - The transition region is a very narrow (60 miles / 100 km) layer between the chromosphere and the corona where the temperature rises abruptly from about 8000 to about 500,000 K (14,000 to 900,000 degrees F, 7700 to 500,000 degrees C).
Corona - The corona is the outermost layer of the Sun, starting at about 1300 miles (2100 km) above the solar surface (the photosphere). The temperature in corona is 500,000 K (900,000 degrees F, 500,000 degrees C) or more, up to a few million K. The corona cannot be seen with the naked eye except during a total solar eclipse, or with the use of a coronagraph. The corona does not have an upper limit.
DIFFERENT PARTS OF THE SUN ROTATE AT DIFFERENT SPEEDS
Our gaseous sun is divided into different zones and layers, with each of our host star's regions moving at varying speeds. On average, the sun rotates on its axis once every 27 days. However, its equator spins the fastest and takes about 24 days to rotate, while the poles take more than 30 days. The inner parts of the sun also spin faster than the outer layers, according to NASA. Back in 1612, Galileo Galilei noticed something odd: sunspots moved across the sun's disk over time, confirming the sun's rotation, according to Stanford University's Solar Center. Even today, researchers can monitor the sun's movements and rate of rotation by observing its sunspot activity.
Sunspots occur when the sun's plasma interacts with its magnetic field and can lead to solar flares and other types of solar storms.
You'd expect sunspots to be hot, but they're cold areas on the sun's surface, though "cold" is a relative term. Sunspots average around 5,000 to 7,500 degrees Fahrenheit (2,760 to 4150 degrees Celsius), in contrast to the areas surrounding them, which average around 9,900 degrees F (5,480 C).
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