The Sun: Our Star - PowerPoint PPT Presentation

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The Sun: Our Star. Hydrostatic Equilibrium. Structure of the Sun. More About the Sun. Helioseismology. Vibrations on the surface depend on the density and temperatures in the interior of the Sun. Nuclear Reactions. Overcoming Electrostatic Repulsion. Nuclear Fusion: Energy for Sun.

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The Sun: Our Star

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Presentation Transcript

The sun our star

The Sun: Our Star

Hydrostatic equilibrium

Hydrostatic Equilibrium

Structure of the sun

Structure of the Sun

More about the sun

More About the Sun



  • Vibrations on the surface depend on the density and temperatures in the interior of the Sun

Nuclear reactions

Nuclear Reactions

Overcoming electrostatic repulsion

Overcoming Electrostatic Repulsion

Nuclear fusion energy for sun

Nuclear Fusion: Energy for Sun

Fusion in the core of the sun

Fusion in the Core of the Sun

Energy from fusion

Energy from Fusion

  • Proton mass = 1.6726 ´ 10-27 kg

  • Four protons = 6.690 ´ 10-27 kg

  • One helium-4 nucleus = 6.643 ´ 10-27 kg

  • Two positrons = 0.0018´ 10-27 kg

  • Neutrino mass even smaller

  • Mass converted per reaction: E = mc24.5 ´ 10-29 kg E = 4 ´ 10-12 Joules

  • Less than a percent (0.7%) of mass

Core pressure balance

Core Pressure Balance

Testing the solar model

Testing the Solar Model

Neutrinos from the sun

Neutrinos from the Sun

Radiation zone

Radiation Zone:

  • Photons “random walk” through many layers of the Sun

Convection zone

Convection Zone

  • The gas in the convection layers “bubble” like boiling water

  • Photons of light are aided in their journey to the outer layers of the Sun





Granulation and sunspots

Granulation and Sunspots

  • The brighter features are hotter due to the laws of thermal radiation

  • What does this imply about the Sunspot?

  • Granules are evidence of convection below the photosphere

Chromosphere and corona

Chromosphere and Corona

Magnetic fields and charged particles

Magnetic Fields and Charged Particles

Sunspots and magnetic fields

Sunspots and Magnetic Fields

  • Sunspots are cold spots on the photosphere

  • Sunspots are“storms” of magnetic field

  • Prominencesand flares are connected tosunspots



Solar flare

Solar Flare

The active sun x ray image

The Active Sun: X-ray Image

Sunspot cycle

Sunspot Cycle

  • Number of sunspotspeaks every 11 years

  • Location of sunspotsshifts during cycle

  • Solar cycle is really22 years: magnetic field is reversed in the E-W direction

Babcock model

Babcock Model

Solar activity affects earth

Solar Activity Affects Earth

Solar activity affects earth1

Solar Activity Affects Earth

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