the sun unit 6: astronomy. first…we have to discuss light information about universe light...
TRANSCRIPT
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The SunThe Sun
Unit 6: AstronomyUnit 6: Astronomy
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First…we have to discuss light
First…we have to discuss light Information about universe
Light emitted from stars and other bodies in space
Electromagnetic spectrum = arrangement of waves according to their wavelengths and frequencies We see visible part of spectrum
Information about universe Light emitted from stars and other
bodies in space Electromagnetic spectrum =
arrangement of waves according to their wavelengths and frequencies We see visible part of spectrum
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Visible LightVisible Light
A range of waves with various wavelengths
Passed through a prism Violet bent more
than blue Blue bent more
than green Etc.
A range of waves with various wavelengths
Passed through a prism Violet bent more
than blue Blue bent more
than green Etc.
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SpectroscopySpectroscopy
Study of the properties of light that depend on wavelength
absorption spectrum = visible light is passed through a cool gas under low pressure
Study of the properties of light that depend on wavelength
absorption spectrum = visible light is passed through a cool gas under low pressure
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Absorption SpectrumAbsorption Spectrum
Each element or compound in gaseous form produces unique set of spectral lines
Studying a star Lines indicate
which elements --> star’s chemical composition
Each element or compound in gaseous form produces unique set of spectral lines
Studying a star Lines indicate
which elements --> star’s chemical composition
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Remember the Doppler Effect?
Remember the Doppler Effect?
Light from a source moving away from you appears redder Waves are lengthened
Moving toward you appears bluer Waves are shortened
Determine whether a star or other body in space is moving away from or toward Earth Measured from the dark
lines in spectra and comparing them with a standard spectrum
Light from a source moving away from you appears redder Waves are lengthened
Moving toward you appears bluer Waves are shortened
Determine whether a star or other body in space is moving away from or toward Earth Measured from the dark
lines in spectra and comparing them with a standard spectrum
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Intro to the SunIntro to the Sun
“Average” star Earth’s primary
source of energy Only star whose
surface we can study Diameter = 109
Earths Mass = 332,000
times of Earth
“Average” star Earth’s primary
source of energy Only star whose
surface we can study Diameter = 109
Earths Mass = 332,000
times of Earth
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Our Sun is a StarOur Sun is a Star
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Structure of the SunStructure of the Sun
Sun is made of gas No clear
boundaries between layers
4 parts Solar interior Photosphere Chromosphere corona
Sun is made of gas No clear
boundaries between layers
4 parts Solar interior Photosphere Chromosphere corona
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PhotospherePhotosphere
Visible surface Radiates most of the
sunlight we see Layer of gas Grainy texture -->
granules Composition = 90%
hydrogen, almost 10% helium Dark lines of
absorption spectrum
Visible surface Radiates most of the
sunlight we see Layer of gas Grainy texture -->
granules Composition = 90%
hydrogen, almost 10% helium Dark lines of
absorption spectrum
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ChromosphereChromosphere
Above the photosphere
Thin layer of hot gases
Can see during a total solar eclipse (red rim) Light from
photosphere is blocked out
Above the photosphere
Thin layer of hot gases
Can see during a total solar eclipse (red rim) Light from
photosphere is blocked out
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CoronaCorona
Outermost portion of the solar atmosphere
Weak Envelope of gases
--> extend a million kilometers from sun
Outermost portion of the solar atmosphere
Weak Envelope of gases
--> extend a million kilometers from sun
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CoronaCorona
Solar wind = streams of protons and electrons ejected at high speed from the corona Travel through solar
system and are lost to space
Alters appearance of bodies in the solar system
Earth’s magnetic field doesn’t allow them to reach our surface --> do affect our atmosphere
Solar wind = streams of protons and electrons ejected at high speed from the corona Travel through solar
system and are lost to space
Alters appearance of bodies in the solar system
Earth’s magnetic field doesn’t allow them to reach our surface --> do affect our atmosphere
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Solar WindSolar Wind
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SunspotsSunspots Dark spots on the surface
of the sun Temperature is less than the
surrounding solar surface Number of sunspots
observable vary in an 11-year cycle Increases to maximum (100)
--> then decrease to minimum
Motion of sunspots --> sun rotates about once a month Not all parts rotate at the
same speed (gaseous)
Dark spots on the surface of the sun Temperature is less than the
surrounding solar surface Number of sunspots
observable vary in an 11-year cycle Increases to maximum (100)
--> then decrease to minimum
Motion of sunspots --> sun rotates about once a month Not all parts rotate at the
same speed (gaseous)
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SunspotsSunspots
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The Solar CycleThe Solar Cycle
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ProminencesProminences
Concentration of gases often appearing as arches extending beyond corona Sometimes can
erupt matter escapes Sun’s atmosphere
Concentration of gases often appearing as arches extending beyond corona Sometimes can
erupt matter escapes Sun’s atmosphere
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Solar FlaresSolar Flares Sudden eruption
Above sunspot cluster Release lots of energy
(UV, radio, X-ray) Atomic particles released
--> reach Earth day later (affect long-distance radio communications)
Auroras = bright display of light caused by solar radiation interacting with the upper atmosphere at the poles Following strong solar
flare
Sudden eruption Above sunspot cluster Release lots of energy
(UV, radio, X-ray) Atomic particles released
--> reach Earth day later (affect long-distance radio communications)
Auroras = bright display of light caused by solar radiation interacting with the upper atmosphere at the poles Following strong solar
flare
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How Solar Activity Affects the Earth
How Solar Activity Affects the Earth
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Solar InteriorSolar Interior
Source of energy = nuclear fusion Combining of the nuclei of lighter
elements to form a heavier element Energy released because some
matter is converted to energy
Source of energy = nuclear fusion Combining of the nuclei of lighter
elements to form a heavier element Energy released because some
matter is converted to energy
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Introduction to Nuclear Energy
Introduction to Nuclear Energy
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Process of nuclear fusionProcess of nuclear fusion
Converts four hydrogen nuclei into the nucleus of a helium atom Lots of energy released! 4 hydrogens = 4.032 amu; 1 helium
= 4.003 amu Missing mass! (.029 amu)
Animation
Converts four hydrogen nuclei into the nucleus of a helium atom Lots of energy released! 4 hydrogens = 4.032 amu; 1 helium
= 4.003 amu Missing mass! (.029 amu)
Animation
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Process of nuclear fusionProcess of nuclear fusion
E = mc2
c = speed of light Speed of light is very high (300,000
km/sec) --> amount of energy released from small mass is very high One pinhead of hydrogen to helium >
burning thousands of tons of coal
E = mc2
c = speed of light Speed of light is very high (300,000
km/sec) --> amount of energy released from small mass is very high One pinhead of hydrogen to helium >
burning thousands of tons of coal
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Nuclear Fusion in the SunNuclear Fusion in the Sun
Small percentage of hydrogen is converted to energy Helium forms the solar core --> grows
Small percentage of hydrogen is converted to energy Helium forms the solar core --> grows
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Future of the SunFuture of the Sun
Will the sun run out of hydrogen fuel? Last another 100 billion years
Sun will grow Engulf Earth
Sun can exist in its stable state for 10 billion years Already 4.5 billion years old
Will the sun run out of hydrogen fuel? Last another 100 billion years
Sun will grow Engulf Earth
Sun can exist in its stable state for 10 billion years Already 4.5 billion years old