The PPT Contains the detailed information regarding the energy derived from sun. Also it include structure of sun.

1. SOLAR ENERGY
By
Dr. Sonal G. Chonde
Department of Environmental
Science, Shivaji University,
Kolhapur.

2. ENERGY GIVEN BY SUN

3. The Sun is the star at the center of the solar system. It has a
diameter of about 1,392,000 km, about 109 times that of
earth and its mass (about 2 × 1030 kilograms, 330,000 times
that of Earth) accounts for about 99.86% of the total mass of
the Solar System.
Figure : sun observe
by SUMER instrument

4.  Physical characteristics
 Mean diameter 1.392×106 km
109 × Earth
 Equatorial radius 6.955×105 km
109 × Earth
 Equatorial circumference 4.379×106 km
109 × Earth
 Surface area 6.0877×1012 km2
11,990 × Earth
 Volume 1.412×1018 km3
1,300,000 × Earth
 Mass 1.9891×1030 kg
333,000 × Earth
 Average Density 1.408×103 kg/m3

5.  Hydrogen 73.46%
 HELIUM 24.85%
 OXYGEN 0.77%
 CARBON 0.29%
 IRON .16%
 SULFER 0.12%
 NEON 0.12%
 NITROGEN 0.09%
 SILICON 0.07%
 MAGNESIUM 0.05%

6.  As the Sun consists of a plasma and is not solid, it rotates
faster at its equator than at its poles. This behavior is known
as differential rotation, and is caused by convection in the
Sun and the movement of mass, due to steep temperature
gradient from the core outwards.

 The period of this actual rotation is approximately 25.6 days
at the equator and 33.5 days at the poles.
 The Sun does not have a definite boundary as rocky planets
do, and in its outer parts the density of its gases drops
exponentially with increasing distance from its center.
 The solar interior is not directly observable, and the Sun itself
is opaque to electromagnetic radiation.

9. The core of the Sun is considered to extend from the
center to about 0.2 to 0.25 of the solar radius.
It has a density of up to 150 g/cm3
(about 150 times the density of water) and
a temperature of close to 13.6 million Kelvin(K).
By contrast, the Sun's surface temperature is approximately
5,800 K.
The core is the only region in the Sun that produces an
appreciable amount of thermal energy through fusion

12. From about 0.25 to about 0.7 solar radii, solar material is hot and
dense enough that thermal radiation is sufficient to transfer the intense heat
of the core outward.This zone is free of thermal convection while the
material gets cooler from 7 to about 2 million Kelvin with increasing
altitude, this temperature gradients less than the value of the adiabatic
lapse rate and hence cannot drive convection.
Energy is transferred by radiation ion of hydrogen and helium emit
photons , which travel only a brief distance before being reabsorbed by
other ions.

13.  An the Sun's outer layer, from its surface down to approximately
200,000 km (or 70% of the solar radius), the solar plasma is not dense
enough or hot enough to transfer the thermal energy of the interior outward
through radiation; in other words it is opaque enough.
 As a result, thermal convection occurs as thermal columns carry hot
material to the surface (photosphere) of the Sun. Once the material cools
off at the surface, it plunges downward to the base of the convection zone,
to receive more heat from the top of the radiative zone.
 At the visible surface of the Sun, the temperature has dropped to 5,700 K
and the density to only 0.2 g/m3 (about 1/6,000th the density of air at sea
level)
 The thermal columns in the convection zone form an imprint on the surface
of the Sun as the solar granulation and super granulation The turbulent
convection of this outer part of the solar interior causes a "small-scale"
dynamo that produces magnetic north and south poles all over the surface
of the Sun

14.  The Sun's photosphere has a temperature between 4500 and 6000 Kelvin
(with an effective temperature of 5800 Kelvin)
 and a density of about 2 × 10−4 Kg m3 other stars may have hotter or
cooler photospheres.
 The Sun's photosphere is composed of convection cell called granules —
cells of gas each approximately 1000 kilometers in diameter with hot
rising gas in the center and cooler gas falling in the narrow spaces between
them. Each granule has a lifespan of only about eight minutes, resulting in
a continually shifting "boiling" pattern.
 Grouping the typical granules are super granules up to 30,000 kilometers in
diameter with lifespan of up to 24 hours. These details are too fine to see
on other stars.

15.  The chromospheres (literally, "color sphere") is a thin layer of the Sun's
atmosphere just above the photosphere , roughly 2,000 kilometers deep.
 The chromospheres is more visually transparent than the photosphere. The name
comes from the fact that it has a reddish color, as the visual spectrum of the
chromospheres is dominated by the deep red H-alpha spectral line of hydrogen.
The coloration may be seen directly with the naked eye only during a total solar
eclipse , where the chromospheres is briefly visible as a flash of color just as the
visible edge of the photosphere disappears behind the Moon .
 the temperature of the chromospheres is hotter than that of the photosphere. The
photosphere is closer to the center of the sun and its temperature is around 4000 K
to 6400 K but the chromospheres is about 4500 K to as high as 20,000 K
 Figure :The Sun observed through a
telescope with an H-alpha filter

16.  A corona is a type of plasma “atmosphere" of the Sun or other celestial body,
extending millions of kilometers into space, most easily seen during a total Solar
eclipse, but also observable in a Chronograph. The Latin root of the word corona
means crown.
 The high temperature of the corona gives it unusual spectral features.
 Light from the corona comes from three primary sources, which are called by
different names although all of them share the same volume of space. The K-corona
(K for kontinuierlich, "continuous" in German) is created by sunlight scattering off
free electron The F-corona (F for Fraunhofer) is created by sunlight bouncing off
dust particles
 The E-corona (E for emission) is due to spectral emission lines produced by ions
that are present in the coronal plasma
 Figure : During a total solar eclipse ,
 the solar corona can be seen with
 the naked eye.

17. Sunspots are temporary phenomena on the photosphere of the Sun that
appear visibly as dark spots compared to surrounding regions. they are
caused by intense magnetic activity, temperatures of sunspot are roughly
3,000–4,500 K the contrast with the surrounding material at about 5,780 K
leaves them clearly visible as dark spots, as the intensity of a heated black
body . They may also travel at relative speeds ("proper motions") of a few
hundred m/s when they first emerge onto the solar photosphere.

18. Granules on the photosphere of the sun are caused by convection current
of plasma within the Sun's convective zone. The grainy appearance of the
solar photosphere is produced by the tops of these convective cells and is
called granulation. The rising part of the granules is located in the center
where the plasma is hotter. The outer edge of the granules is darker due to
the cooler descending plasma. A typical granule has a diameter on the order
of 1,000 kilometers and lasts 8 to 20 minutes before dissipating. Below the
photosphere is a layer of “super granules" up to 30,000 kilometers in
diameter with lifespan of up to 24 hours.

19. A prominence is a large, bright feature extending outward from the Sun's surface,
often in a loop shape. Prominences are anchored to the Sun's surface in the
photosphere, and extend outwards into the Sun's corona. While the corona consists
of extremely hot ionized gases, known as plasma, which do not emit much visible
light, prominences contain much cooler plasma, similar in composition to that of
the chromospheres. A typical prominence extends over many thousands of
kilometers. roughly half the radius of the Sun or 28 times the diameter of the Earth.
Flocculi (plural of flocculus) is another term for these filaments, and dark Flocculi
typically describes the appearance of solar prominences when viewed against the
solar disk in certain wavelengths.
Solar prominences.

20. The solar wind is a stream of charged particle ejected from the upper atmosphere
of the Sun. It mostly consists of electrons and protons with energies usually
between 10 and 100 keV. The stream of particles varies in temperature and speed
over time. These particles can escape the Sun's gravity because of their high kinetic
energy and the high temperature of the corona The solar wind creates the
heliosphere a vast bubble in the interstellar medium that surrounds the solar system.
The solar wind is divided into two components, respectively termed the slow solar
wind and the fast solar wind. The wind is considered responsible for the tails of
comets, along with the Sun's radiation. Earth itself is largely protected from the
solar wind by its magnetic field ,which deflects most of the charged particles,
however some of the charged particles are
trapped in the Van Allen radiation belt.

21. Birth:
Gravitational Collapse of
Interstellar Cloud
"Hayashi Contraction" of
Protostar
Life:
Stability on Main-
Sequence
Long life - energy from
nuclear reactions in the
core
(E = mc2)
Death:
Lack of fuel, instability,
variability expansion (red
giant, then white dwarf)
Life Cycle of the Sun

22.  Solar spectrum:
The solar radiation distribution constituting UV-VIS-IR
radiation.
solar wide spectrum of wavelengths
 The maximum span of solar spectrum: The region of
spectrum where a high energy radiation is falling on earth
(1.4-1.8 eV)

23. BLUE
GREEN
YELLOW
ORANGE
RED
VIOLET
Increasing λ
Cosmic
and
γ-rays
X-rays
(UV)
Vacuum
ultraviolet
(UV)
Near
ultraviolet
Visible
(NIR)
Near
infrared
(IR)
Infrared
Radio
Microwave
0.1 nm 200 nm 400 nm 800 nm 2 μm 50 μm
1019Hz 1015Hz 1013Hz
Increasing Frequency (ν)

24. The surface receives about 47% of the total solar energy that
reaches the Earth. Only this amount is usable.

25. http://en.wikipedia.org/wiki/File:Breakdown_of_the_incoming_solar_energy.svg

28. Complete the Reaction
1H
4Be
1
H
8O
4Be
2He
2He
1H
2He
2He
2He
6C
1H element
atomic
number
(protons)
6C

29.  Nuclear Fusion is the energy-producing process taking place in the
core of the Sun and stars
 The core temperature of the Sun is about 15 million °C. At these
temperatures hydrogen nuclei fuse to give Helium and Energy. The
energy sustains life on Earth via sunlight

30. 1kg Hydrogen
.993 kg Helium

31. Neutron induced in U235
Fission is Exothermic
The sum of the masses of
the resulting nuclei is less
than the original mass
(about 0.1% less)
The “missing mass” is converted
to energy according to E=mc2

32. Review
Nuclear fission:
A large nucleus splits into several
small nuclei when impacted by a
neutron, and energy is released in
this process
Nuclear fusion:
Several small nuclei fuse
together and release
energy.

33. It is an artificial constructed pond.
It consist of different layers of water
Temperature as well as salt concentration goes
on increasing as we move from top to bottom
of solar pond.
1) Surface convective Zone
2) Non- Convective Zone
3) Lower convective Zone

47.  1) Latent Heat Storage Device :-
 Storage of Thermal energy by Phage Changing Material
(PCM) such a material which changes phase when it store
energy content. E.g.. Hydrated salts
 2) Sensible Heat Storage Device :-
 Storage of Thermal energy by absorbing it. E.g.. Solar pond