Solar Energy

Solar Energy

This section covers the fundamentals of solar energy. From this we can determine how much energy is available over an area to be used for heat or electricity.

Motivation

To use the sun effectively as a source of energy, we have to know how it moves through the sky and what energy is available. From this knowledge we can place photovoltaic panels, building windows, or heat collectors correctly.

References

  • Renewable and Efficient, Gil Masters

Questions we will be able to answer

  • Where is the sun at any time?

  • How much radiation does it produce?

  • Where do I put solar panels or windows?

  • Will my solar devices be blocked by trees or homes?

  • Which direction should they face?

  • How much will they produce now? this month? this year?

Solar Fundamentals

This section covers the sun, the solar system, and the atmosphere in order to understand the radiation striking the earth.

The journey of a photon

  • Created in the core of the sun

  • Millions of years to bounce out to surface of sun

  • Zips to earth in about 8 minutes

  • Passes through the atmosphere

  • Strikes a solar panel and dislodges an electron in the PV panel

  • Electron is collected and delivered to the grid

Electromagnetic Spectrum

Blackbody Spectrum

Solar Spectrum

The Solar System

Radiation units

  • Power per unit area (watts per square meter) (W/m2^2)

  • Power = Power per unit area ×\times area

  • Energy = Power ×\times Time

Atmospheric depth

Atmospheric absorption

  • Air mass ratio

  • IB=AekmI_B = Ae^{-km}

  • IBI_B - insolation at earth's surface (W/m2^2)

  • AA - insolation in space (W/m2^2)

  • kk - optical depth (no units)

  • mm - air mass ratio (no units)

Air mass ratio

Air mass ratio

  • There are some standard air mass ratios we use

  • AM0 is "in space"

  • AM1 is for noon-day sun

  • AM1.5 is the standard test condition that resembles year round

    insolation

Earth sun distance

d=1.5×108(1+0.017sin(360(n93)365))kmd=1.5 \times 10^8 \left(1 + 0.017 sin\left(\frac{360(n-93)}{365}\right)\right)km

  • nn is the day of the year

  • Is this close to circular?

Theory vs Practice

  • I'll demonstrate mathematical expressions for solar radiation

  • In practice you will use tables or software applications that

    calculate these values

  • I want you to be able to go back in 10 years, pick up this book, and

    figure it out again.

Summary of Angles

  • Box 4.1 of REEPS

Solar Irradiation

  • Solar Constant

  • Peak sun hours

Radiation Basics

  • Power per unit area

  • Spectral intensity

Mass Glazing Ratio

Extraterrestrial solar radiation

  • Sunlight striking the top of the atmosphere

I0=SC(1+0.034cos(360n/365)))I_0 = SC \left( 1 + 0.034 \cos\left(360n/365)\right)\right)

Where

  • SC=1367W/m2SC = 1367 W/m^2

Software Implementation

You can see an example of these equations implemented in a software library at these locations

Solar Measurements

  • Pyranometers

Shading Measurements

Path Finder

Historical radiation data

Radiation measurements

  • We've seen how to calculate radiation

  • How do we measure it?

Measuring solar radiation

Typical meteorological year

  • Hourly solar and weather estimates for typical conditions

  • Based on historical data

Typical meteorological year

NREL TMY3

TMY Station Locations

NREL Station Map

TMY quantities

  • Global Horizontal Irradiance (GHI)

  • Direct Normal Irradiance (DNI)

  • Diffuse Horizontal Irradiance (DHI)

Components of solar radiation

  • Direct

  • Reflected

  • Diffuse

Direct, reflected, diffuse

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