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№1 слайд![The Sun and Solar constant](/documents_5/b1f6748d3457097a99cc35a22aa8cd4d/img0.jpg)
Содержание слайда: The Sun and Solar constant
Structure of the solar atmosphere
№2 слайд![Some particularities of the](/documents_5/b1f6748d3457097a99cc35a22aa8cd4d/img1.jpg)
Содержание слайда: Some particularities of the solar atmosphere
Solar atmosphere is non-homogeneous and very unstable.
Phenomena in the solar atmosphere
Flares (факелы)
Floccules-flocculi-flocculus (plasma blow out)
Flashes (вспышки)
chromospheres flashes occur corpuscular and electromagnetic emanation are very rapid to increase
flashes duration: few minutes to a few hours.
Corpuscle’s speed of about 1000 km/s.
The distance between the Sun and the Earth is about 150 000 000 km.
is the time needed for the corpuscular flux to reach the Earth and to cause magnetic storm or aurora.
№3 слайд![Two successive photos of a](/documents_5/b1f6748d3457097a99cc35a22aa8cd4d/img2.jpg)
Содержание слайда: Two successive photos of a solar flare phenomenon evolving on the sun. The solar disk was blocked in these photos for better visualization of the flare
A sunspot viewed close-up in ultraviolet light, taken by the TRACE spacecraft
№4 слайд![Solar spots Some relatively](/documents_5/b1f6748d3457097a99cc35a22aa8cd4d/img3.jpg)
Содержание слайда: Solar spots
Some relatively cold formations (4599 – 4600 K) of irregular shape appearing in the photosphere are known as SOLAR SPOTS.
They are observed in the latitudinal zone 5 – 35 degrees in the both sides from equator. Duration: from a few hours up to a few months.
The solar spots are regarded as indicator of SOLAR ACTIVITY (SA).
Wolfer Number (WN)
K is empirical coefficient, f indicates the total number of the spots,
g denotes number of the spot groups. The WN fluctuates with the period of 11 years (7 – 11). Minimal SA Maximal SA
№5 слайд![](/documents_5/b1f6748d3457097a99cc35a22aa8cd4d/img4.jpg)
№6 слайд![Total spectrum of the solar](/documents_5/b1f6748d3457097a99cc35a22aa8cd4d/img5.jpg)
Содержание слайда: Total spectrum of the solar radiation
Gamma rays Visible wavelengths (μ)
X-rays Violet 0,39 – 0,455
Ultraviolet (UV) Blue 0,455 – 0,485
Visible light Light blue 0,485 – 0,505
Infrared (IR) Green 0,505 – 0,575
Radio waves Yellow 0,575 – 0,585
Orange 0,585 – 0,620
Red 0,620 – 0,575
The energy emitted by the Sun is generated deep within the Sun. Like most of the stars the Sun is made up primary of hydrogen (71%) and helium (21%). The heavier elements occupy 2% only. Near the Sun centre temperature is about 16000000 K and the density is 150 times larger that of water. Under these conditions atoms of Hydrogen interact and form helium. This process generate energy in form of gamma radiation equal to hydrogen bombs per second.
№7 слайд![](/documents_5/b1f6748d3457097a99cc35a22aa8cd4d/img6.jpg)
№8 слайд![](/documents_5/b1f6748d3457097a99cc35a22aa8cd4d/img7.jpg)
№9 слайд![Notion of OPTICAL WINDOW](/documents_5/b1f6748d3457097a99cc35a22aa8cd4d/img8.jpg)
Содержание слайда: Notion of OPTICAL WINDOW
Emittance of the Sun is close to the emittance of the a. Bb with the temperature 5800 K, , and the most part of the SR energy falls on the wavelength range 0,29 – 2,4 μ.
It has happened that the Earth’s atmosphere is the most transparent just for the same wavelength range. That is why we call this range
OPTICAL WINDOW
№10 слайд![Solar constant The amount of](/documents_5/b1f6748d3457097a99cc35a22aa8cd4d/img9.jpg)
Содержание слайда: Solar constant
The amount of SR (radiation flux) coming to the upper boundary of the Earth atmosphere in a unit of time to a unit of area facing the rays, at average distance between the Sun and the Earth is called
SOLAR CONSTANT
According to satellite measurement
Some recent measurement recorded
This constant includes the energy of all wavelengths coming from the Sun. Therefore we call it Astronomic Solar Constant
For the upper part of the troposphere
(for the wavelength interval )
We call it Meteorological Solar Constant.
№11 слайд![Temperature of the Sun](/documents_5/b1f6748d3457097a99cc35a22aa8cd4d/img10.jpg)
Содержание слайда: Temperature of the Sun emitting surface
Average distance between the Sun and the Earth
And the radius of the sun is
Every of the sphere of the radius
in one second receives the energy
. The Whole sphere receives
all the energy emitted by the Sun
This temperature is also called effective (radiation) temperature of the Sun.
For practical purposes it adopted to be 6000 K
№12 слайд![](/documents_5/b1f6748d3457097a99cc35a22aa8cd4d/img11.jpg)
№13 слайд![](/documents_5/b1f6748d3457097a99cc35a22aa8cd4d/img12.jpg)
№14 слайд![Distribution of the Sun](/documents_5/b1f6748d3457097a99cc35a22aa8cd4d/img13.jpg)
Содержание слайда: Distribution of the Sun energy in various areas of the spectrum
UV ( ) – 9%
Visible Light ( ) – 47%
IR ( ) – 44%
99% of the energy falls to the area 0,1 – 4,0 μ.
Conclusion: The Sun emits Short wave radiation.
100% of the terrestrial radiation (Earth’s radiation) falls to the area 3 – 120 μ (maximal 10μ).
Conclusion: The Earth emits Long wave radiation.
№15 слайд![Solar radiation distribution](/documents_5/b1f6748d3457097a99cc35a22aa8cd4d/img14.jpg)
Содержание слайда: Solar radiation distribution over the globe
We’ll consider the distribution over the upper “boundary of the atmosphere”, where the astronomical factors only may be accounted for
Rotation of the Earth about the Sun.
The tilt to ecliptic of the earth spinning axis.
The Earth spinning.
At an arbitrary chosen moment of time the distance between the Sun and the Earth is not necessarily equal to the average one, i. e.
№16 слайд![Insolation The flux of solar](/documents_5/b1f6748d3457097a99cc35a22aa8cd4d/img15.jpg)
Содержание слайда: Insolation
The flux of solar radiation falling on a horizontal surface is called
INSOLATION
denotes altitude of the Sun above horizon (or just SUN ALTITUDE)
Here, φ is latitude, δ is declination of the Sun, П=86400 s is duration of the one spin of the earth, is hour angle, and t is time being counted from the noon.
Let us determine amount of SR Q arriving to one of a horizontal surface during a day time at the top of the atmosphere, i. e. diurnal insolation.
№17 слайд![](/documents_5/b1f6748d3457097a99cc35a22aa8cd4d/img16.jpg)
№18 слайд![](/documents_5/b1f6748d3457097a99cc35a22aa8cd4d/img17.jpg)
№19 слайд![](/documents_5/b1f6748d3457097a99cc35a22aa8cd4d/img18.jpg)
№20 слайд![](/documents_5/b1f6748d3457097a99cc35a22aa8cd4d/img19.jpg)
№21 слайд![](/documents_5/b1f6748d3457097a99cc35a22aa8cd4d/img20.jpg)