CHAPTER ONE

1.0 INTRODUTION

The ionosphere is subjected to diurnal, solar cycle, and spatial variation(eg Rishbeth and Garriottm 1969, ivanor_kholodny and mikhailor, 1986, Brekkem 1997,kazamura et al, 2002, yu et al, 2004).It is zell established that the formation of the ionosphere is primarily due to the upper atmosphere by solar x-ray and extreme ultraviolet (EUV) radiations of wavelengths less than 1026A(Adler et al, 1997), which are known to have different period variations, especially the well-known solar cycle variations. Observations indicates that parameters of the Earth’s ionosphere, such as the critical frequency (FOF2), the peak electron content (TEC) are strongly controlled by solar activity in a rather complicated way.

   Solar proxies have been used to represented solar emissions in the absence to continued long-term records of solar EUV fluxes, since the variations of solar EUV radiations are the primary cause for changes in the ionosphere.

Sunspot number and solar 10.7cm radio noise, F107, are commonly used as proxies for solar activity (eg Bilitza 2000). By examining the relationship between a monthly median F107 (or Nmf2) and a smoothed sunspot numbers or F107. However, at high values of the sunspot numbers or F107, median FoF2 (or NmF2) tends to saturate. It is controversial whether the ionospheric saturation effect is a true manifestation of solar activity  effect, and what cause tat the ionospheric saturation effect is due to the nonlinearity of solar EUV with F107

The sun is a star. It is rather ordinary star-not particularly big or small, not particularly young or old. It is the source of heat which sustains life on Earth, and controls our climate and weather. It is the closest star to Earth and the most closely studied from it we have learned a great deal about the physical processes which determine the structure and evolution of stars in general

Only the  sun’s outer layers, collectively referred to as the  solar atmosphere’, can be observed directly. There are distinct regions to the solar atmosphere, the photosphere, the chromosphere and the corona. These three regions have substantially different properties from each other, with regions of gradual transition between them.

           THE PHOTOSPHERE 

The sum has basically the same chemical elements as found on Earth. However, the sum is so hot that all of these elements exist in the gaseous state. There is not really a “surface” to the sun. Think of it this way; the sun is a bunch of gas which gets denser and denser as you move from space toward the core. Think of what a thick cloud looks like when you look down on it from an airplane. It looks solid, but it isn’t.

The sun’s atmosphere changes from being transparent to being opaque over a distance to only a few hundred kilometers. This is remarkable given the size of the sun, and represents such a huge change that we often think of it as a true boundary. When we speak of the size of the sun, we usually mean the size of the region surrounded by the photosphere. The photosphere is slightly different from one place on the sun to another, but in general it has a pressure about a few hundredths of the sea-level pressure on Earth, a density of about a ten-thousandth of the Earth’s sea-level atmospheric density, and a temperature in the range 4500-6000 Kelvin

The gases which extend away from the photosphere make up the chromosphere. These gases are transparent to most visible radiation. The chromosphere is about 2500km thick. The density of the gases decreases as you move away from the photosphere into the chromosphere, but the temperature increases. From the bottom to the top  of the chromosphere, the average temperature goes from 4500 to 10,000kelvin.

Needless to say, this rise was not anticipated by scientists when they first measured it. Throughout the rest of the sun, temperature decreases as you move further away from the core.

 THE CORONA

The chromosphere merges into the outermost region of the sun’s atmosphere, the corona. The corona extends for millions of miles into space above the photosphere. Usually, we cannot see the corona because of the brightness of the photosphere.

However, during a total solar eclipse, the corona shines beautifully against the dark sky. The corona has a density of about 0.0000000001 times that of the Earth’s sea level atmosphere. It is very hot-millions of Kelvin. Because of this high temperature, the bulk of the radiation from the corona is emitted at ultraviolet and x-ray wavelengths. Magnetic fields on the sun seem to play an important part in heating the gas to such a high temperature. However, the exact way that this happens is not well understood. The image you see to the left was taken during a solar eclipse in 1980: light from the photosphere is blocked out by the moon (the dark disk)

1.1                     BACKGROUND OF STUDY

THE SOLAR WIND

The solar wind is nothing more than a stream of charged particles flowing outward from the sun with an average velocity of about 400km|sec. it is a natural consequence of the sun being so hot-the corona gas has too much energy to be gravitationally bound to the sun..............................................................................................................

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