YOUKO

Welcome To All

YOUKO

Presented By

R. Vigneswar

Guided By : Mr. N. Sreekanth (associative professor)

Global College Of Engineering And Technology, Kadapa

THE FEATURE SOURCE OF ENERGY

Seminar

On

Contents:Abstract About SunEnergy From The SunEnergy That Falls On The

EarthEnergy That Is Usable Collection Of EnergyApplications Of Collected

EnergyStorage Of Energy

CollectedConclusion

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.

About The Sun

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.

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

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.

Structure

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.

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.

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.

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.

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.

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.

Contd………….

APPLICATIONS OF SOLAR

TECHNOLOGY

Solar Light

Architecture and urban planning

Agriculture and horticulture

Transport and reconnaissance

Solar Thermal

Water heating

Heating, cooling and ventilation

Water treatment

Process heat

Cooking

Electricity production

Concentrated solar power

Photovoltaic

Energy storage methods

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.

Conclusion

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.

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.