Components of the sun
Layers of the sun
Layers of the sun
Layers of the sun
The Sun as an Energy Resource
Technology Fundamentals
Technology Fundamentals
Solar Spectrum
Maybe it's the amazingly warm week we are having here in northern New England, but it's hard not to think about the sun these days. Even as we soak up its warmth, we also hear of fearsome solar storms flinging billions of tons of plasma into space, some of it toward us.
These coronal mass ejections tend to peak around the so-called solar maximum, a time of increased solar activity with a period of approximately 11 years. We are entering one.
Our typically naïve picture of the sun as a placid ball of fire in the sky has nothing to do with the real thing.
Close-up images reveal an inferno of intense heat (some 11,000 degrees Fahrenheit at the surface), bubbling with incessant activity and intense magnetic fields.
Solar storms are a reminder that we shouldn't take the sun for granted, assuming it will always be doing its job quietly, even if this has been the case for billions of years.
The sun radiates 4 X 1026 watts, that is, 4 followed by 26 zeros watts, equivalent to 100 billion 1-megaton nuclear bombs. Compare this to your living room light bulb, at 60 Watts. All this power comes from nuclear reactions happening at the solar core, fusing hydrogen into helium at a furious rate. The sun, now in its middle age, is in its main sequence phase, which, fortunately for us, is fairly stable. No one should start having nightmares that we will be fried tomorrow.
At its present age, the sun has converted only about 5 percent of its total mass into helium. As this amount increases, so will the Sun's luminosity, that is, its total power output. In 1.1 billion years, the luminosity will be 10 percent larger than today, and in 3.4 billion years, 40 percent larger. This extra power will have serious consequences for Earth's climate. First it will create a "moist greenhouse" effect, then a true "runaway greenhouse" effect. In the end, we won't be able to take the heat.
Given that life was impossible for the first billion or so years of Earth's 4.5 billion-year existence due to a steady bombardment from comets and asteroids — it follows that life can only exist within a window of the sun's lifetime, roughly 5 billion of its 10 billion years.
The Sun as an Energy Resource
Technology Fundamentals
The sun is the source of the life on our planet Earth and, directly or indirectly, is the fuel for most renewable systems. Photovoltaic and solar thermal systems, as well as solar thermal power stations, convert solar irradiation directly into useable energy. Continuing our Fundamentals series, Volker Quaschning gives an overview of the solar energy resource.
The sun is made up of about 80% hydrogen, 20% helium and only 0.1% other elements. Its radiant power comes from nuclear fusion processes, during which the sun loses 4.3 million tonnes of mass each second. This mass is converted into radiant energy. Each square metre of the sun’s surface emits a radiant power of 63.1 MW, which means that just a fifth of a square kilometre of the sun’s surface emits an amount of energy equal to the global primary energy demand on earth. Fortunately, only a small part of this energy reaches the earth’s surface. Solar irradiance decreases with the square of the distance to the sun. Since the distance of the earth to the sun changes during the year, solar irradiance outside the earth’s atmosphere also varies between 1325 W/m² and 1420 W/m². The annual mean solar irradiance is known as the solar constant and is 1367±2 W/m². On Mars, which is further from the sun than Earth, solar irradiance is below 600 W/m² – a factor to be considered when designing PV-powered satellites for the Mars orbit. Only a surface that is perpendicular to the incoming sun’s rays receives this level of irradiance. Outside the atmosphere, and therefore not subject to its influence, solar irradiance has only a direct component – all solar radiation is virtually parallel. This irradiance is also called direct normal or beam irradiance Ebeam. Under these conditions, a surface that is oriented parallel to the sun’s rays receives no irradiance. (The specific direct solar irradiance Edir that reaches an inclined surface is lower depending on the cosine of the angle of incidence q: Edir = Ebeam·cos q.)
Irradiance, Irradiation and Illuminance
Various different terms are used when dealing with solar radiation. However, these terms are often used incorrectly, even by some solar specialists. The total specific radiant power, or radiant flux, per area that reaches a Spectrum AM 0 (extraterrestrial) Spectrum AM 1.5 (terrestrial) receiver surface is called irradiance. Irradiance is measured in W/m² and has the symbol E. When integrating the irradiance over a certain time period it becomes solar irradiation. Irradiation is measured in either J/m² or Wh/m², and represented by the symbol H. For daylighting purposes, only the visible part of the sunlight is considered. The analogous quantity to the irradiance for visible light is the illuminance. This uses the unit lm/m² (lumen/m²) or lx (lux).
Solar Spectrum
It is the surface temperature of the sun that mainly characterizes the solar spectrum. This spectrum defines the corresponding spectral irradiance for all wavelengths of sunlight. Visible light, with wavelengths between 0.4 µm and 0.75 µm, has a 46% share of the spectrum, infrared light 47%, and ultraviolet light only 7% (see Figure 1). The earth’s atmosphere reduces the irradiance that reaches the earth’s surface. Ozone, water vapour and carbon dioxide absorb radiation with certain wavelengths as it passes through the atmosphere. The significant reduction in mainly the ultraviolet and infrared parts of the spectrum is a result of this absorption.
FIGURE 1. Extraterrestrial and terrestrial spectrum of sunlight
Direct and Diffuse Irradiance
Other atmospheric particles reflect or scatter sunlight. Only a part of the extraterrestrial beam irradiance reaches the earth’s surface directly (see Figure 2). The scattered part of the irradiance has no direction. Only direct irradiance can be used for concentrating solar systems, but non-concentrating systems can also use the scattered, or diffuse irradiance. The so-called global irradiance Eg on a horizontal surface on earth consists of the direct Edir and diffuse irradiance Edif. On a tilted plane, there is another irradiance component Eref, which is that component reflected from the ground. The average ground reflection is about 20% of the global irradiance. Hence, the irradiance Etilt on the tilted plane consists of three components, Etilt = Edir + Edif + Eref.
A surface perpendicular to the incoming direct sunlight usually gets the highest possible irradiance. Normally, it is below 1000 W/m²; higher values are only possible in particular situations, such as if snow or clouds reflect sunlight onto the receiver surface.
FIGURE 2. Sunlight passing through the atmosphere
Air Mass
If the sun is perpendicular to the earth’s surface, sunlight only has to pass through the air mass (AM) of the atmosphere once. Therefore, this state is called AM 1. In all other cases, the route of the solar radiation through the atmosphere is longer. This way depends on the sun’s height. AM 2 indicates that the path of the sunlight through the atmosphere is twice AM 1. This is the case if the sun is 30° above the horizon (gS = 30°). In general, the definition of the air mass is AM = 1/sin(gS).
Figure 3 shows the variation of the air mass during the year for Berlin and Cairo at solar noon – that is, the time during a day with the highest sun elevation, which depends on longitude, latitude and date. It is obvious that in Cairo the air mass is always lower than in Berlin.
FIGURE 3. Position of the sun and AM values at solar noon for various days in Berlin, Germany and Cairo, Egypt
Position of the Sun
The optimum tilt angle for solar systems depends on the position of the sun. Two angles define this position:
1. Sun height, height angle, solar altitude angle or elevation gS
This is the angle between a line that points from the site towards the centre of the sun, and the horizon (see Figure 4). The zenith angle is the opposite angle to the sun height (90° – gS). At a sun height of 90°, the sun is at the zenith and the zenith angle is therefore zero.
2. Sun azimuth aS
The sun azimuth aS is the angle, measured clockwise, between geographical North and the point on the horizon directly below the sun (at the end of a line running from the centre of the sun to the horizon).
(Another definition is sometimes used, whereby the definition of the sun height remains the same but the sun azimuth is counted as zero when the sun is in the South and measured anticlockwise.Sometimes the symbols of azimuth and sun height are also interchanged.)
The calculation of the position of the sun is rather complicated. It is mainly influenced by the earth’s orbit around the sun and the rotation of the earth. If the sun’s height is very low, the visible position of the sun varies from the real position due to refraction of sunlight in the atmosphere. However, some algorithms have been developed to calculate the position of the sun with accuracies better than 0.1°. (A free on-line tool to estimate the position of the sun with three different algorithms can be found at
FIGURE 4. Definition of the angles for the description of the position of the sun
Optimal Solar System Orientation
Figure 5 visualizes the sun angles, azimuth and tilt angle to define the position of a tilted surface. The angle of incidence q depends on all these angles. As mentioned above, the maximum irradiance can usually be obtained by a surface that is perpendicular to the sun. Since the position of the sun changes during the day and year, only a two-axis tracked surface gets the maximum irradiation. The annual irradiation can be more than 30% higher than on a non-tracked surface, while for a one-axis tracked surface the irradiation gain will be in the range of 20%. Near the equator, the optimal orientation of a non-tracked surface is nearly horizontal. In the Northern Hemisphere, it should be tilted towards the south, and in the southern hemisphere, towards the north. The optimal tilt angle increases with higher latitudes, and is higher in winter than in summer.
FIGURE 5. Angles to define the position of the sun and the orientation of a tilted plane
Irradiance Measurements
Outside the atmosphere, the annual solar irradiation is about 12,000 kWh/m² (8760 h at 1367 W/m²). At every site on the earth, half of the year is night, with no sunshine. The atmosphere reduces the irradiance at least by 25%. Clouds and dust cause a further reduction. The best sites on earth, in extreme desert areas, receive an annual solar irradiation which can be more than 2500 kWh/m². On the other hand, there are cloudy sites at high latitudes with an annual irradiation far below 1000 kWh/m². On-site measurements are the only way to estimate the solar potential for solar systems. Different types of sensors exist to measure the solar irradiance.
A pyranometer measures the global irradiance. Different designs offer different levels of accuracy (see photographs). Low-cost pyranometers use silicon sensors with a small photovoltaic cell that generates an electrical current that is nearly proportional to the solar irradiance. However, these sensors measure only part of the solar spectrum – they cannot sense infrared light. The annual accuracy of these sensors is limited because the spectrum changes with the air mass. In the ideal case error margins be of the order of 5%.
More precise pyranometers use a black receiver plate that is mounted below a double glass dome. This plate heats up depending on the incoming irradiance. A thermocouple converts the heat difference between the plate and its surroundings into a voltage signal that is proportional to the irradiance. These sensors can obtain annual error margins of less than 3%.
To measure the direct normal or beam irradiance, the sensor is mounted inside the end of an absorber tube (this tube keeps the diffuse irradiance away). This so-called pyrheliometer has to be mounted on a two-axis tracker that follows the sun very accurately. If a shading ball, or shading ring, permanently shades a pyranometer, it measures the diffuse irradiance since direct irradiance is kept away.
However, careful maintenance of all sensors is necessary in order to obtain high levels of accuracy. Dust on the sensors, inaccurate trackers or dirt can reduce the measurement quality significantly. In the worst case, measurements can be totally useless!
Sensors for solar irradiance measurements
Pyranometer with thermal sensor for global irradiance measurements (left top)
Two-axis tracked pyrheliometer for direct normal irradiance measurements (left bottom)
Pyranometer with shading ball for diffuse irradiance measurements (right)
Satellite Measurements
Meteorological satellites can also provide irradiance data. Half-hourly meteorological images are compared with clear sky pictures. The result is a cloud index for the whole satellite image. Finally, models that consider the position of the sun, water vapour and aerosols provide the reduction of the extraterrestrial irradiance on the way through the atmosphere. The annual accuracy of satellite measurements compared with ground measurements is not bad, and can exceed 5%.
Solar Irradiance Data Sources
Since the variation of annual irradiations from year to year can be well over 20%, a measurement period should cover at least 7–10 years. Carrying out a measurement campaign over such a long time period is unlikely to be possible before planning and installing a solar system, so irradiance data can be taken from existing databases. Local irradiance maps or atlases offer information on annual or monthly irradiance. In many cases, local weather services can provide very detailed data. However, this data is rarely available free. The Meteonorm software (www.meteotest.ch) includes the largest commercially available database of irradiance data with some thousands of sites around the world. Some internet databases offer free irradiance data, while the US National Renewable Energy Laboratory provides 239 free hourly data sets of the US (rredc.nrel.gov/solar). The World Radiation Data Centre (wrdc-mgo.nrel.gov) and NASA surface meteorology resource website (eosweb.larc.nasa.gov/sse) offer additional global irradiance data. Finally, the European projects S@tel-light (www.satellight.com) and SoDa (www.soda-is.com) provide exhaustive data for Europe.
With irradiance data that describe the availability of the fuel for solar systems the planning and prediction of the energy yield of solar systems is possible. These aspects will be discussed in later articles in this series.
Components of the sun
Consists of the sun like the rest of the stars of hydrogen as an essential component represents 92% and during the process of energy production turn hydrogen into helium atom, which represents 7.8% of the components of the sun and the rest other elements such as oxygen, which represents 0.06% of carbon, sulfur and nitrogen.
Layers of the sun
Consists sun of several layers, center of the sun is the nucleus, consisting of compressed gas - equivalent to the pressure inside the center 340 billion times atmospheric pressure at sea level in the ground - in the case of the condition is called plasma (other cases of solid, liquid, gas) - The plasma state is simply situation where the molecule material has been subjected to heat and pressure alarming and begins electron to escape from the nucleus then the plasma state - and this place (the kernel) is the source of energy production that takes its way towards the outside, and pass through the layers of the Sun, for which the particles of light (photon) energy and seep into the upper classes, and in the fact that the process of downloading the photon energy and rushes out takes about a million years and there and through that process Chih energy boiling graduated.
Consists sun of several layers, center of the sun is the nucleus, consisting of compressed gas - equivalent to the pressure inside the center 340 billion times atmospheric pressure at sea level in the ground - in the case of the condition is called plasma (other cases of solid, liquid, gas) - The plasma state is simply situation where the molecule material has been subjected to heat and pressure alarming and begins electron to escape from the nucleus then the plasma state - and this place (the kernel) is the source of energy production that takes its way towards the outside, and pass through the layers of the Sun, for which the particles of light (photon) energy and seep into the upper classes, and in the fact that the process of downloading the photon energy and rushes out takes about a million years and there and through that process Chih energy boiling graduated.
Layers of the sun
Consists sun of several layers, center of the sun is the nucleus, consisting of compressed gas - equivalent to the pressure inside the center 340 billion times atmospheric pressure at sea level in the ground - in the case of the condition is called plasma (other cases of solid, liquid, gas) - The plasma state is simply situation where the molecule material has been subjected to heat and pressure alarming and begins electron to escape from the nucleus then the plasma state - and this place (the kernel) is the source of energy production that takes its way towards the outside, and pass through the layers of the Sun, for which the particles of light (photon) energy and seep into the upper classes, and in the fact that the process of downloading the photon energy and rushes out takes about a million years and there and through that process Chih energy boiling graduated.
The photosphere
They lower layer of the atmosphere of the sun and a thickness of approximately 500 km, and from which the solar radiation, which lies in the visible light and temperature of about 5000 degrees Celsius.
The chromosphere
Thickness extends to a few thousand kilometers and its constituent gases less dense and more transparent than the photosphere and radiations weak in visible light but powerful in X-rays and ultraviolet and Alradojh, temperature up to about 100,000 Kelvin.
Area aura Koruna
They lower layer of the atmosphere of the sun and a thickness of approximately 500 km, and from which the solar radiation, which lies in the visible light and temperature of about 5000 degrees Celsius.
The chromosphere
Thickness extends to a few thousand kilometers and its constituent gases less dense and more transparent than the photosphere and radiations weak in visible light but powerful in X-rays and ultraviolet and Alradojh, temperature up to about 100,000 Kelvin.
Area aura Koruna
They outer layer of the atmosphere of the sun and extends millions of kilometers, with less density and transparency Ghazadtha chromosphere and radiations weak in visible light, but strong in UV and UV ray and Alradojh, and temperature up to millions of degrees centigrade
Solar flares
A phenomenon repeated constantly during the activity cycle is repeated every 11 years, and occurs when more than magnetic energy and liberated suddenly Vinbos white light severe flare as a result, has been observed first time in September 1859 by the British astronomer Richard Carrington when he watched sunspots observed the emergence of white light Baher suddenly appeared, and the explosion of solar-called gas electrically charged quickly three million miles per hour toward the ground, although some penetrate the magnetosphere., and affects one layer of the atmosphere is a layer (the ionosphere); these high-energy particles disrupt case ionic in the ionosphere which works to save the Earth's magnetic field which affects the radio communications on the ground, especially as they rely on electromagnetic waves.
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