Facts About Sun

 

    Facts About Sun

DiD U Know!   SUN. It’s a great blessing of GOD. The star at the core of the Solar System is the Sun. Its center undergoes nuclear fusion events, transforming it into a nearly perfect ball of hot plasma that is incandescent. The Sun is the most significant source of energy for life on Earth, radiating this energy mostly as light, ultraviolet, and infrared radiation. In this article I am going to tell you some interesting facts about sun. So let’s start:

Size of Sun:

• The Sun's radius is around 109 times greater than that of the Earth at 695,000 kilometers (432,000 miles).
•  Its mass is approximately 330,000 times that of the Earth and accounts for 99.86% of the solar system's total mass.

Composition:

• The Sun's mass is made up of mostly hydrogen (73%) and helium (25%), with considerably lesser amounts of heavier elements such as oxygen, carbon, neon, and iron.
• The interstellar medium from which the Sun arose provided the Sun with much of its initial chemical makeup. Around 71.1% hydrogen, 27.4% helium, and 1.5% heavier elements would have made up its initial composition.

• Helium has risen from around 24% to about 60% of the core's composition as a result of fusion, and certain heavy elements including helium have gravitationally fallen from the photosphere into the Sun's core.
• 
  The Sun will eventually depart the main sequence and turn into a red giant as helium continues to slowly build up in its core over the course of the next 5 billion years.

Formation:

The collapse of a portion of a massive molecular cloud, primarily made up of hydrogen and helium, which likely gave birth to many other stars, led to the formation of the Sun some 4.6 billion years ago. Nucleocosmochronology and computer simulations of star evolution are used to determine its age. The outcome is in line with the 4.567 billion year radiometric age of the oldest Solar System material. The stable daughter nuclei of short-lived isotopes like iron-60, which can only originate in bursting, young stars, have been found in ancient meteorites. This suggests that the formation of the Sun must have been close to one or more supernovae.

Atmosphere:

• A temperature minimum zone of the Sun that reaches 500 km above the photosphere and has a temperature of around 4,100 K is considered to be its coldest layer. Simple molecules like water and carbon monoxide may exist in this region of the Sun because it is cold enough to support their presence. These molecules' absorption spectra can be used to identify them.
• In comparison to the Sun's surface, the chromosphere, transition area, and corona are significantly hotter. Although the cause is unclear, research shows that Alfvén waves may have sufficient energy to heat the corona.
• A layer about 2,000 km thick, which is characterized by a spectrum of emission and absorption lines, is present above the layer of lowest temperature. Because the chromosphere may be seen as a colourful flash at the start and finish of total solar eclipses, it gets its name from the Greek word chroma, which means color. The chromosphere's temperature rises steadily with height, peaking at around 20,000 K towards the top. Helium partly ionizes in the chromosphere's higher region.

• The temperature rapidly increases from roughly 20,000 K in the upper chromosphere to coronal temperatures that are closer to 1,000,000 K above the chromosphere in a narrow (about 200 km) transition area.
• The complete ionization of helium in the transition area, which considerably lessens radiative cooling of the plasma, facilitates the temperature increase. There is no clearly defined height at which the transition area occurs. Instead, it creates a nimbus-like structure surrounding chromospheric elements like spicules and filaments and moves chaotically all the time. Although the transition area is not clearly visible from Earth's surface, devices sensitive to the extreme ultraviolet section of the spectrum may easily see it from space.

Core:

• About 20–25% of the solar radius is where the core of the Sun begins. It has a temperature of over 15.7 million Kelvin and a density of up to 150 g/cm3 (around 150 times that of water) (K). The surface of the Sun, in comparison, is around 5800 K hot.
• Only the Sun's core generates a significant quantity of thermal energy through fusion; within 30% of the Sun's radius, fusion has all but ceased. 99% of the power is produced within this region.
• This energy heats the Sun's remaining material as it moves through a series of layers until arriving at the solar photosphere, where it radiates (as photons) or advects into space (massive particles).
• With a solar radius of 0.45, the radiative zone is the sun's thickest layer. Thermal radiation serves as the main energy transmission mechanism from the core to a distance of around 0.7 solar radii.  As you get farther from the core, the temperature lowers from around 7 million to 2 million Kelvin.
  
  
  

Unbelievable Facts:

• The sun is the nearest star to the Earth:

Inside the sun's enormous plasma ball, thermonuclear processes take occur. It is over 150 million kilometers away from us.

• Helium derives its name from the Sun:

The streaks of radiation from an unidentified element were seen when scientists initially sought to deduce the chemical makeup of our star from its spectrum. It was given the name Helios in honour of the Greek sun god since for a while it was thought to be present exclusively there. Later, this chemical was also discovered on Earth, but the term persisted.

• The mass of the Sun is 500 times bigger than that of all the planets in its solar system:

The mass of the solar system is made up 99.86% by the sun. This indicates that it is 500 times heavier than the combined weight of all the planets and asteroids. Even Jupiter's mass is merely a thousandth of the mass of our star.

• Magnetic storms may develop on Earth as a result of solar wind:

The solar wind is an ongoing acceleration of charged particles caused by the magnetic field of the Sun. Typically, its power is insufficient to do harm to Earthlings.

• The Earth is farther from the Sun in the summer than in the winter:

The orbit of the Earth around the Sun is elliptical. In other words, the distance to it changes over the year. The axis' inclination to the ecliptic, rather than this fact, is what determines when it is winter and summer. As a result, when summer arrives in the northern hemisphere, winter does likewise in the southern hemisphere.

• The sun produces more than just visible light:

The sun, like all stars, produces a variety of electromagnetic radiation. Our eyes can only discern a limited portion of colors, from 380 nm (purple) to 740 nm (red). You first reach the range of infrared radiation if you continue to increase the wavelength, and then you reach radio waves.

THANKS!