ch. 28 the sun. 28.1 the structure of the sun 3 parts 1.core 2.inner zones radiative zone convective...
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The Core
• Entirely composed of Gas• Nuclear Fusion Reactor
H + H He + energy
• Energy is released as heat and light
E = mc2
Energy = (mass)(speed of light)2
The Inner Zones
• Radiative Zone: Energy is moving from atom to atom in the form of waves (radiation)
• Convective Zone: Energy is transferred through the movement of unevenly heated gases (convection)
The Sun’s Atmosphere
• Photosphere: Inner most layer• Chromosphere: gasses that appear to glow
red• Corona: The outermost layer– Solar Wind: Charged atomic particles that stream
out into space
• Solar Flares: outward eruption of electrically charged particles.
• Auroras: When electrically charged particles of a solar wind reach earth.
28.3 Formation of the Solar System
1. About 4-5 billion years ago, a Solar Nebula contracted due to an outside force.
2. The Sun began to form at the center of the contacting nebula – 99% of the matter in the nebula became the sun
3. Left over matter aggregated to form the planets
• Temperature and Distance from the Sun affected the planetary composition. – Proto-planets closest to the sun contain large
amounts of heavier elements, such as iron– Proto-planets further away consist of gasses and
lighter elements
Formation of Earth• Early Earth was very hot compared to Earth
today. – Heat from collisions with plantesimals– Increasing mass of the outer core, increased inner
pressure and temperature– Radioactive materials were very abundant
Separation into 3 layers
• Dense materials, such as iron, flowed into the center
• Less dense materials were forced to the outer layers
Earth’s “second atmosphere” came from Earth itself.
The volcanoes released:- steam (H2O)- carbon dioxide (CO2)- ammonia (NH3)
Eventually photosynthetic organisms converted the carbon dioxide gas found in the oceans into
oxygen. This formed our current atmosphere
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