Sun and its unknown Rare facts in Solar System
Introduction
The solar system is a vast and complex cosmic arrangement that includes the Sun, planets, moons, asteroids, comets, and other celestial bodies held together by gravity. The Sun is the central star of the solar system, radiating energy and supporting life on Earth. Eight major planets orbit the Sun, each with its own distinct characteristics, ranging from rocky terrestrial worlds such as Mercury, Venus, Earth, and Mars to gas giants Jupiter, Saturn, Uranus, and Neptune.
There are also numerous moons orbiting these planets, some of which have diverse geology and the potential to support life. Asteroids, rocky pieces of the early solar system, and comets, icy bodies formed in the far reaches of the Kuiper Belt and Oort Cloud, populate the solar system beyond the planets.
Comprehending the dynamics, evolution, and composition of our solar system helps us understand our cosmic origins and guides scientific endeavors to investigate and possibly colonize worlds beyond our own.
The sun
Heat-producing gases make up the Sun. We refer to its glowing surface as the photosphere. The reddish-colored chromosphere sits above the photosphere, and the corona, which is visible during eclipses, is situated beyond it. The sun emits seven different colors in its visible light.
There are seven colors that make up the visible white light of the sun: violet, indigo, blue, green, yellow, orange, and red. The Fraunhofer lines are hundreds of dark lines superimposed on top of these. The primary component of the Sun, like all other stars, is hydrogen.
Every planet orbits the sun in a clockwise direction, starting from the west and moving eastward. Also, the majority of them revolve on their own axis, going from west to east. As a planet gets farther from the sun, its tenperatury decreases and its velocity increases.
At an average speed of roughly 285 km/s, the Sun and the surrounding stars orbit the galactic center in nearly circular patterns. It takes the Sun 224 million years to make one revolution around the galactic center at this speed. At the core of the Sun lies a massive nuclear furnace known as the cosmic yon, which is converting 600 million tonnes of hydrogen into helium every second. The temperature is roughly 1,50,00,000°C here.
It’s common to refer to the Sun, the central figure in the solar system of Earth, as an ordinary star. However, the sun’s mass and brightness exceed 80% of all the stars visible in the galaxy around Earth.
However, the majority of stars that are easily visible on a clear night are larger and more brilliant than the Sun.
The sun shines on Earth six million times more brightly than all the other stars combined, and it is 400,000 times brighter than the full moon. The heat and light that are produced by a sequence of thermonuclear reactions involving the atoms of the elements that make up the Sun enable life on Earth.
The Sun’s Structure One way to picture the globe of gas that makes up the Sun is as a collection of concentric shells that vary in thickness. Different processes happen within each shell.
The diagram illustrates how energy leaves the Sun’s core and makes its way to its surface through two substantial interior layers. The electromagnetic energy produced in the sun’s core is absorbed and reradiated by atoms in the radiation zone, which is where it travels towards the surface.
The process is slow, perhaps taking a million years, because the core’s X-rays and gamma rays collide with atoms on their indirect path through the radiation zone.
The convection zone is a turbulent layer made up of Row density gases that are stirred by convection, a method of heat transfer. At the bottom of the convection zone, gas atoms are heated by radiation from the radiation zone. As gases warm and lose density, they rise to the Sun’s surface. Gases emit energy into space from the surface in the form of visible light, ultraviolet right, and infrared radiation.
However, the majority of stars that are easily visible on a clear night are larger and more brilliant than the Sun. Because of its close proximity to Earth, the Sun appears incredibly big and bright. The sun shines on Earth six million times more brightly than all the other stars combined, and it is 400,000 times brighter than the full moon.
The heat and light that are produced by a sequence of thermonuclear reactions involving the atoms of the elements that make up the Sun enable life on Earth. The Sun’s structure is best described as a collection of concentric shells with differing densities. This globe of gas is what makes up the Sun. Different processes happen within each shell.
The diagram illustrates how energy leaves the Sun’s core and makes its way to its surface through two substantial interior layers. The electromagnetic energy produced in the sun’s core is absorbed and reradiated by atoms in the radiation zone, which is where it travels towards the surface. Because the X-rays and gamma rays from the core collide with atoms numerous times as they follow an indirect path through the radiation zone, the process is slow and could take a million years.
Convection is a mode of heat transfer that stirs up Row density gases, which form the turbulent layer known as the convection zone. Radiations from the radiation zone heat the gas atoms at the bottom of the convection zone. The gases rise to the surface of the Sun as they warm and lose density. From the surface, the gases release energy into space as visible light, ultraviolet light, and infrared radiation.
After losing some of their energy as radiation, the gas atoms in the convection zone lose volume, get denser, and descend back into the radiation zone. There, as they take in radiation from the sun’s core, they warm up once more. The heated gas atoms rise once more, transporting energy from the convection zone’s bottom to its top before radiating away at the surface and sinking once more.
The familiar pattern of a convection cell, which can be found in the Earth’s atmosphere, boiling water, and many other physical systems, is the movement of gas atoms in the solar convection zone. The sun’s surface and atmosphere are the parts that can be seen. The photosphere, also known as the surface of the sun, is a luminescent plasma with a temperature of 6000–K that is most likely 100 km thick.
We see most of the light that it emits. Relatively cool areas of the photosphere, known as sunspots when viewed from Earth, are present. The chromosphere, or “sphere of color,” is a transparent, 10,000 km-thick layer of plasma that makes up the layer of the Sun’s atmosphere directly above the photosphere.
It appears as a pinkish glow around the eclipsed Sun during an eclipse. Streamers and filaments of outward-moving, hot plasmas bent by the Sun’s magnetic field can be seen beyond the chromsphere. The corona, the outermost part of the Sun’s atmosphere, stretches several million kilometers before joining the solar wind, a vortex of protons and electrons traveling at high speeds. Comet tails and the Earth’s aurora borealis are both created by the solar wind.
Solar prominences, which are dense plasma clouds, are also found in the corona. The magnetic field of the sun pulls the plasma clouds into twisted and looping forms. If large prominences are oriented toward Earth, they can result in electric blackouts.
Sun’s Chemical Make-Up When sunlight is examined using a spectroscope, it is discovered to be a continuous spectrum made up of every color in a rainbow in the correct order, dotted with numerous dark lines. Gaseous matter in the Sun’s atmosphere is what creates the “absorption lines.”
It is thought that iron, nickel, and calcium make up the majority of the corona’s composition. They are all extremely attenuated and highly ionized, indicating temperatures in the range of a million degrees Fahrenheit.
Sunspots, which are regions of gas cooler than the surrounding gas, can occasionally be seen on the photosphere of the Sun. They are still hotter than the surface of many stars at 4,000°C. Sunspots are thought to form when magnetic force lines penetrate the Sun’s surface, blocking some of the heat from entering that area of the surface, according to astronomers.
The collapse of the magnetic field surrounding a sunspot results in an energy eruption called a solar flare. Since the discovery of sodium, which was the first metal to be discovered by scientists, the Sun has been found to contain over 60 different naturally occurring terrestrial elements, all of which are gaseous due to the Sun’s extreme heat.
Hydrogen accounts for 71 per cent of the Sun’s mass, helium 26.5 per cent and all the other known elements, 2.5 per cent.
Death of the Sun: The Sun, like all stars, will spend the majority of its life in a stable state of size and light output, powered by nuclear reactions at its core that convert hydrogen into helium in a process similar to that of a hydrogen bomb. However, during the last 10% of its life, the Sun will go through a series of death throes that will fundamentally alter it.
In the first stage, it will run out of hydrogen in its core and begin to burn helium. It will then expand into a red giant, roasting and engulfing planets as far away as Mars. Finally, it will become so swollen and distended that it will lose more than half of its mass in space, which will take approximately 50,000 years.
What remains will be a white dwarf, a small star that gradually releases energy from its outer layer and cools. It will then turn into an invisible black dwarf. Any planet that remains in orbit around the dead Sun will freeze in the extreme cold of space.