Introduction
According to
Stellar Classification, the Sun is a G2V star and is informally designated as a
yellow dwarf. G2 indicates its surface temperature of 5778K and V indicates
that the Sun, like most stars, is a main-sequence star which generates energy
by nuclear fusion of hydrogen nuclei to helium. In
its core, the Sun fuses 620 million metric tonnes of hydrogen each second.
Internal Layers
Surface of the Sun
Invisible
lines of magnetic force that twist around the Sun’s globe are the cause of many
extraordinary features. Huge arches of fire, called Prominences, can be held up
above the Sun by magnetism. Flares, sudden, massive explosions of energy, burst
forth when the magnetic field shifts. Where the magnetic field lines erupt
through the photosphere, there are dark, cooler areas known as sunspots. Beyond
the chronosphere lies the corona, the Sun’s hot, shimmering outer atmosphere.
This is visible from the Earth only during Total solar Eclipses.
Fate of the Sun
T
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he Sun is an
ordinary star. To us on Earth, it is of crucial importance since no life could
exist without it, but it is simply one of billions of stars in the Milky Way
Galaxy, itself one of billions of galaxies in the universe. For a star, the Sun
is below average size- some astronomers classify it as a “yellow dwarf”. Yet it
is massive when compared to the planets. The Sun contains more than 99% of all matter
in the Solar System. Its diameter of 1,392,684 kilometres is more than 100 times that of
Earth.
According to
Stellar Classification, the Sun is a G2V star and is informally designated as a
yellow dwarf. G2 indicates its surface temperature of 5778K and V indicates
that the Sun, like most stars, is a main-sequence star which generates energy
by nuclear fusion of hydrogen nuclei to helium. In
its core, the Sun fuses 620 million metric tonnes of hydrogen each second.
The mean distance of the Sun from the Earth is approximately
149.6 million kilometers (1 AU), though the distance varies as the Earth moves from perihelion in January to aphelion in July.
Internal Layers
At
the centre of the Sun is the core, a region of incredible pressure (200 billion
times that on the Earth’s surface) and intense heat- about 15 million degrees
Celsius. This is the Sun’s nuclear furnace, where the energy that keeps it
shining is released. Energy from the fusion reaction flows out from the
radiative zone to the connective zone. Here, in a continuous cycle, hot gas
bubbles up to the surface before sinking down to be reheated again.
The
picture below shows all the layers of the Sun.
An illustration of the structure of the Sun:
1. Core
2. Radiative zone
3. Convective zone
4. Photosphere
5. Chromosphere
6. Corona
7. Sunspot
8. Granules
9. Prominence
1. Core
2. Radiative zone
3. Convective zone
4. Photosphere
5. Chromosphere
6. Corona
7. Sunspot
8. Granules
9. Prominence
Surface of the Sun
The
Sun’s outer shell, the Photosphere, is only about 500km thick and, at 5500
degrees, much “cooler” than at the core. It is in a state of constant motion,
like water in a boiling kettle. Hundreds of thousands of flaming gas jets,
called spicules, leap up to 10,000km into the Sun’s atmosphere, known as the
Chromosphere.
Invisible
lines of magnetic force that twist around the Sun’s globe are the cause of many
extraordinary features. Huge arches of fire, called Prominences, can be held up
above the Sun by magnetism. Flares, sudden, massive explosions of energy, burst
forth when the magnetic field shifts. Where the magnetic field lines erupt
through the photosphere, there are dark, cooler areas known as sunspots. Beyond
the chronosphere lies the corona, the Sun’s hot, shimmering outer atmosphere.
This is visible from the Earth only during Total solar Eclipses.Fate of the Sun
About
7 billion years from now, the hydrogen that the Sun uses as furl to create
energy will start to run out. Eventually the Sun will balloon into a Red Giant,
engulfing Mercury and perhaps Venus too. This is what Earth’s landscape may
look like when this happens. Its oceans and atmosphere have gone and its rocky
surface is melting in temperatures of 1500 degrees Celsius.
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| A White Dwarf |




