© 2010 Pearson Education, Inc. Chapter 14 Our Star.

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Presentation transcript:

© 2010 Pearson Education, Inc. Chapter 14 Our Star

© 2010 Pearson Education, Inc. Why does the Sun Shine?

© 2010 Pearson Education, Inc. Is it on FIRE?

© 2010 Pearson Education, Inc. Is it on FIRE? Luminosity ~ 10,000 years Chemical energy content

© 2010 Pearson Education, Inc. Is it on FIRE? …NO! Luminosity ~ 10,000 years Chemical energy content

© 2010 Pearson Education, Inc. Is it CONTRACTING? Insert TCP 6e Chapter 14 opener

© 2010 Pearson Education, Inc. Is it CONTRACTING? Luminosity Gravitational potential energy ~ 25 million years

© 2010 Pearson Education, Inc. Is it CONTRACTING?...NO! Luminosity Gravitational potential energy ~ 25 million years

© 2010 Pearson Education, Inc. Why does the Sun shine?

© 2010 Pearson Education, Inc. Weight of upper layers compresses lower layers. Insert TCP 6e Figure 14.1

© 2010 Pearson Education, Inc. Gravitational equilibrium: There is a balance between the outward fusion pressure and the inward pressure, due to gravity.

© 2010 Pearson Education, Inc. What is the Sun’s structure? Insert TCP 6e Figure 14.3

© 2010 Pearson Education, Inc. Solar wind: A flow of charged particles from the surface of the Sun

© 2010 Pearson Education, Inc. Corona: Outermost layer of solar atmosphere and seen only during a total solar eclipse. ~1 million K

© 2010 Pearson Education, Inc. Chromosphere: Middle layer of solar atmosphere and seen only during a total solar eclipse. ~ 10 4 –10 5 K

© 2010 Pearson Education, Inc. Photosphere: Visible surface of Sun ~ 6000 K

© 2010 Pearson Education, Inc. Convection Zone: Energy transported upward by rising hot gas

© 2010 Pearson Education, Inc. Radiation Zone: Energy transported upward by photons

© 2010 Pearson Education, Inc. Core: Energy generated by nuclear fusion ~ 15 million K

© 2010 Pearson Education, Inc. Clicker Question What is the surface we see? A.corona B.photosphere C.chromosphere D.solar wind

© 2010 Pearson Education, Inc. Clicker Question What is the surface we see? A.corona B. photosphere C.chromosphere D.solar wind

© 2010 Pearson Education, Inc. Clicker Question What layer is the hottest? A.corona B.photosphere C.chromosphere

© 2010 Pearson Education, Inc. Clicker Question What layer is the hottest? A. corona B.photosphere C.chromosphere

© 2010 Pearson Education, Inc. Clicker Question What layer is the coolest? A.corona B.photosphere C.chromosphere

© 2010 Pearson Education, Inc. Clicker Question What layer is the coolest? A.corona B. photosphere C.chromosphere

© 2010 Pearson Education, Inc. How does nuclear fusion occur in the Sun?

© 2010 Pearson Education, Inc. Fission Big nucleus splits into smaller pieces. (Example: nuclear power plants) Fusion Small nuclei stick together to make a bigger one. (Example: the Sun, stars)

© 2010 Pearson Education, Inc. High temperatures enable nuclear fusion to happen in the core.

© 2010 Pearson Education, Inc. The Sun releases energy by fusing four hydrogen nuclei into one helium nucleus.

© 2010 Pearson Education, Inc. The proton–proton chain is how hydrogen fuses into helium in Sun.

© 2010 Pearson Education, Inc. IN 4 protons OUT 4 He nucleus 2 gamma rays 2 positrons 2 neutrinos Total mass is 0.7% lower.

© 2010 Pearson Education, Inc. Proton-Proton Chain in Gory Detail Step 1: 1 H H 1 --> 2 H 1 + e H 1 is a hydrogen nucleus - subscript is the number of protons in nucleus, superscript is the number of protons + neutrons in the nucleus. Hydrogen nucleus has 1 proton, 0 neutrons. 2 H 1 is a deuterium nucleus (hydrogen isotope) with 1 proton and 1 neutron in nucleus. e + is a positron or antiparticle of the e -. When e + and e - meet, e + + e - __ > 2   two gamma rays are produced  is a neutrino and helps to carry away energy. Step 2: 1 H H 1 --> 3 He 2 +  3 He 2 is a helium isotope,  is a gamma ray. Step 3: 3 He He 2 --> 4 He H H 1 4 He 2 is ordinary or ‘balloon’ helium.

© 2010 Pearson Education, Inc. Clicker Question What is e + ? A.electron B.positron C.Neutron D.proton E.neutrino

© 2010 Pearson Education, Inc. Clicker Question What is e + ? A.electron B.positron C.Neutron D.proton E.neutrino

© 2010 Pearson Education, Inc. Clicker Question What is 2 H 1 ? A.gamma ray B.helium nucleus C.deuterium nucleus D.ordinary hydrogen nucleus

© 2010 Pearson Education, Inc. Clicker Question What is 2 H 1 ? A.gamma ray B.helium nucleus C.deuterium nucleus D.ordinary hydrogen nucleus

© 2010 Pearson Education, Inc. Clicker Question What is ? A.gamma ray B.positron C.Neutron D.proton E.neutrino

© 2010 Pearson Education, Inc. Clicker Question What is ? A.gamma ray B.positron C.Neutron D.proton E.neutrino

© 2010 Pearson Education, Inc. Clicker Question What is  ? A.gamma ray B.positron C.Neutron D.proton E.neutrino

© 2010 Pearson Education, Inc. Clicker Question What is  ? A.gamma ray B.positron C.Neutron D.proton E.neutrino