In this presentation you are going to know about solar energy utilization and storage methods

1. Welcome To All

2. YOUKO
Presented By
R. Vigneswar
Guided By : Mr. N. Sreekanth (associative professor)
Global College Of Engineering And Technology, Kadapa
THEFEATURE SOURCE OF ENERGY
Seminar
On

3. Contents:
Abstract
About Sun
Energy From The Sun
Energy That Falls On The Earth
Energy That Is Usable
Collection Of Energy
Applications Of Collected Energy
Storage Of Energy Collected
Conclusion

4. Abstract:
In this presentation I’m going to tell you about the solar
energy usage and applications of solar energy, and storage
methods. How much of energy is realizing from the sun in
which how much of energy is falling on the earth and how
much of energy is utilizing by us.

5. About The Sun

6. About Sun:
The Sun is the star at the center of the Solar System.
It is by far the most important source of energy for life on Earth.
 The Sun is a nearly perfect spherical ball of hot plasma, with internal
convective motion that generates a magnetic field via a dynamo process.
 The diameter of the Sun is about 109 times that of Earth, and it has a mass
about 330,000 times that of Earth, accounting for about 99.86% of the
total mass of the Solar System.
 Chemically, about three quarters of the Sun's mass consists of hydrogen,
whereas the rest is mostly helium, and much smaller quantities of heavier
elements, including oxygen, carbon, neon and iron.

7. Name and etymology:
 Sunne Old English
 The Sun is viewed as a goddess in Germanic paganism, Sol/Sunna.
 Sanskrit Surya
 The Latin name for the Sun, Sol, is widely known but is not common in
general English language use
Scholars theorize that the Sun, as a Germanic goddess, may represent
an extension of an earlier ProtoIndoEuropean Sun deity due to Indo-
European linguistic connections between Old Norse Sol

8. Characteristics:
 The Sun is a G-type main sequence star that comprises about 99.86% of
the mass of the Solar System.
 The Sun is a Population I, or heavy element rich, star.
 The mean distance of the Sun to Earth is approximately 1 astronomical
unit (about 150,000,000 km; 93,000,000 mi), though the distance varies
as Earth moves from perihelion in January to aphelion in July.
 At this average distance, light travels from the Sun to Earth in about 8
minutes and 19 seconds.
The Sun's radius can be measured from its center to the edge of the
photosphere, the apparent visible surface of the Sun.

9. Structure

10. Core:
 The core of the Sun extends from the center to about 20–25% 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 15.7 million kelvin (K)
 The core is the only region in the Sun that
produces an appreciable amount of thermal
energy through fusion; 99% of the power is
generated within 24% of the Sun's radius, and
by 30% of the radius, fusion has stopped nearly
entirely. The rest of the Sun is heated by this
energy that is transferred outwards,
respectively, through the radiative and
convection zones.

11. Radiative zone:
From the core out to about 0.7 solar
radii, thermal radiation is the primary
means of energy transfer.
However the temperature drops from
approximately 7 to 2 million kelvin
with increasing distance from the
core.
The density drops a hundredfold (from 20 g/cm3 to only 0.2 g/cm3) from
0.25 solar radii to the top of the radiative zone.
Energy is transferred by radiation—ions of hydrogen and helium emit
photons, which travel only a brief distance before being reabsorbed by other
ions.

12. Tachocline:
The radiative zone and the convective zone are
separated by a transition layer, the Tachocline.
This is a region where the sharp regime change
between the uniform rotation of the radiative zone
and the differential rotation of the convection zone
results in a large shear—a condition where
successive horizontal layers slide past one another.
Presently, it is hypothesized (see Solar dynamo) that a magnetic dynamo
within this layer generates the Sun's magnetic field.

13. Convective zone:
In the Sun's outer layer, from its surface to approximately 200,000 km
below (70% of the solar radius from the center), the temperature is lower
than in the radiative zone and heavier atoms are not fully ionized.
As a result, radiative heat transport is less effective. The density of the
plasma is low enough to allow convective currents to develop.

14. Photosphere:
 The visible surface of the Sun, the
photosphere, is the layer below
which the Sun becomes opaque to
visible light.
 The change in opacity is due to
the decreasing amount of H− ions,
which absorb visible light easily.

15. Energy from the Sun:
 The Earth receives 174 peta-watts
(PW) of incoming solar radiation
(insolation) at the upper atmosphere.
 Approximately 30% is reflected back
to space while the rest is absorbed by
clouds, oceans and land masses.
 Sunlight absorbed by the oceans and
land masses keeps the surface at an
average temperature of 14°C.

16. Contd………….

17. APPLICATIONS OF SOLAR TECHNOLOGY

18. Solar Light

19. Architecture and urban planning

20. Agriculture and horticulture

21. Transport and
reconnaissance

22. Solar Thermal

23. Water heating

24. Heating, cooling and ventilation

25. Water treatment

26. Process heat

27. Cooking

29. Concentrated solar power

30. Photovoltaic

32. Energy storage methods

33. Thermal mass systems can store solar energy in the form of heat at
domestically useful temperatures for daily or inter seasonal durations.
Phase change materials such as paraffin wax and Glauber's salt are another
thermal storage media.

34. Conclusion

35. Beginning with the surge in coal use which accompanied the Industrial
Revolution, energy consumption has steadily transitioned from wood and
biomass to fossil fuels.
However development of solar technologies stagnated in the early 20th
century in the face of the increasing availability, economy, and utility of coal
and petroleum.

36. We have proved ... that after our stores of oil and coal are
exhausted the human race can
Receive unlimited power from the rays of the sun.