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26.1 The Sun’s Size, Heat, and Structure
26.2 Observing the Solar System: A History
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The Sun and the Solar System
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The sun is enormous compared to Earth. Its surface
temperature is about 5500°C; its interior is even
hotter.
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The sun’s energy is the result of the conversion of
hydrogen to helium in nuclear fusion. The mass that
does not convert to helium is not lost, but becomes
energy.
26.1 The Sun’s Size, Heat, and Structure
2626 The Sun and the Solar System
4 Hydrogen nuclei (protons)
1 Helium nucleus
energy
2 protons 2 neutrons
Fusion of Hydrogen to Helium
+
fusion
plasma
photosphere
chromosphere
corona
sunspot
solar wind
aurora
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The photosphere, chromosphere, and corona are
layers of the sun’s atmosphere.
26.1 The Sun’s Size, Heat, and Structure
2626 The Sun and the Solar System
Granules, solar
prominences, sunspots, and solar flares appear on
the sun’s surface.
Corona (1,000,000°C)
Core (15,600,000°C)
Chromosphere (20,000°C)
Photosphere (6,000°C)
Radiative zone (8,000,000°C)
Convection zone (1,500,000°C)
Solar prominence
Sunspots (3,500°C)
fusion
plasma
photosphere
chromosphere
corona
sunspot
solar wind
aurora
SECTION OUTLINESECTION OUTLINE
CHAPTER HOMECHAPTER
VOCABULARY
The photosphere, chromosphere, and corona are
layers of the sun’s atmosphere.
26.1 The Sun’s Size, Heat, and Structure
2626 The Sun and the Solar System
Granules, solar
prominences, sunspots, and solar flares appear on
the sun’s surface.
The solar wind is a stream of charged particles from
the sun’s corona. Some solar events, such as solar
flares or coronal holes, cause changes in the solar
wind that can affect Earth.
fusion
plasma
photosphere
chromosphere
corona
sunspot
solar wind
aurora
SECTION OUTLINESECTION OUTLINE
CHAPTER HOME
Ptolemy proposed a geocentric, or earth-centered,
solar system to explain planetary motion.
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Nicolaus Copernicus proposed a heliocentric system,
in which the planets orbit the sun. This model
explained the retrograde motion of planets better
than the geocentric model.
26.2 Observing the Solar System: A History
2626 The Sun and the Solar System
Retrograde motion of Mars
East West
Sept.
Aug. July
June
Dec.Jan.Feb.March
AprilMay
geocentric
heliocentric
gravitation
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VOCABULARY26.2 Observing the Solar System: A History
2626 The Sun and the Solar System
Johannes Kepler used Tycho Brahe’s data to develop three laws that explained the motions of the planets.
June 15th
July 15th
January 15th
December 15th
(30 days) (30 days)
Sun
Equal areas
Earth’s orbit
KEPLER’S EQUAL AREA LAW states that a line connecting Earth to the sun will pass over equal areas of space in equal times. Because Earth’s orbit is elliptical, Earth moves faster when it is nearer to the sun.
geocentric
heliocentric
gravitation
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VOCABULARY26.2 Observing the Solar System: A History
2626 The Sun and the Solar System
Johannes Kepler used Tycho Brahe’s data to develop three laws that explained the motions of the planets.
Isaac Newton developed the universal law of
gravitation, which helped explain the motions of
planets in the solar system.
geocentric
heliocentric
gravitation
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2626 The Sun and the Solar System
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