1 / 27

The Sun as a Star

The Sun as a Star. The “Surface” of the Sun and Its Structure. Outer Layers – 3 distinct region Photosphere Chromosphere Corona. Photosphere -- light sphere. The surface in “visible” light T ~ 6500 - 4000 K Depth 100’s kms. Granulation – cellular pattern due to convection.

leila-maldonado
Download Presentation

The Sun as a Star

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. The Sun as a Star The “Surface” of the Sun and Its Structure Outer Layers – 3 distinct region Photosphere Chromosphere Corona

  2. Photosphere -- light sphere The surface in “visible” light T ~ 6500 - 4000 K Depth 100’s kms Granulation – cellular pattern due to convection

  3. Chromosphere – color sphere, seen at solar eclipse T ~ 6000 - 100,000 K, 2000 km thick Hot, low density gas, also granular appearance – supergranulation

  4. The Corona or Halo T ~ 1-2 x 106 K , extends millions kms Very hot, low density gas Source of energy to heat chromosphere and corona ?? Coronal holes -- in X ray images Flux of charged particles – solar wind - from the holes, governed by magnetic fields Heating via magnetic waves and mechanical flux from convective layers deep in interior

  5. Sunspots and the Solar Activity Cycle Appear dark – lower temp. ~ 4500 K vs 6000 K Strong magnetic fields ~ several thousand Gauss – normal Sun – few Gauss Opposite polarity between sides of a large spot group Magnetic disturbance or storm

  6. The 11 yr sunspot cycle -- magnetic cycle every 22 yrs.

  7. Maunder Minimum and the “ little ice age” the Thames 1677 -- frozen

  8. Solar Activity – Prominences associated with large spot groups

  9. Solar Flares -- most violent form of solar activity A sudden brightening, above large spot group, between regions of opposite polarity Outburst of charged particles (cosmic rays), increase in high energy radiation

  10. The Carrington Event or solar super storm 1859 most powerful solar storm and solar flare recorded Coronal mass ejection – directly toward Earth aurora seen around world as far south as Caribbean so bright it woke people , telegraph systems failed all over Europe and N. America, telegraph machines threw sparks and some telegraph poles caught fire.

  11. Sunspots, prominences, flares all associated with magnetic fields All increase and reach maximum with 11 yr solar activity cycle

  12. lack of spots, aurora, < 50 spots 1672-1699 Normal in 30 yrs 30,000 – 40,000 Galileo1614 ~ 100 spots observed Hevelius 1652-1685, Picard 1653-1685 (LaHire 1718), Flamsteed 1676-1699 LaHire and Durham noted surge in activity 1715

  13. the Maunder minimum and the “little ice age” 1645 -- 1715 global cooling 0.2o C N. Europe ~ 1 - 2o C

  14. Dalton minimum 1800 – 1830 year without a summer 1816 but in 1815 Tambora volcano – middle of Dalton minimum

  15. Sunspots and short term climate change? the Solar irradiance – energy flux watts/m2 at upper atmosphere 0.1 – 0.2% variation in flux Earth’s surface temperature vary by 0.1 – 0.2o C During little ice age global cooling 0.2o C

  16. Sunspot Cycle 24 Cycle 23 minimum 2008.0 but then a lack of spots solar irradiance at 2008 minimum – lower 0.1% global magnetic field at minimum weaker solar wind weakening Is the Sun Missing Its Spots? NY Times 7/21/2009

  17. The impact on global warming ? Or – our perception of it slight increase in solar output ~1900 - 1950

  18. Zero degree reference is 30yr average ~ 1950 - 80

  19. Most recent sunspot curve

  20. The Solar Interior and the energy source of the Sun and Stars Gravitational (contraction/collapse) Nuclear Fission --- radioactive elements Nuclear Fusion --- ??? p+ + p+ -> ? How? the Coulomb barrier

  21. Nuclear Fusion and Nucleosynthesis in the Stars The proton-proton chain or hydrogen fusion, requires 107o K 1. p+ + p+ np+ + e+ + neutrino np+ = deuteron (deuterium) 2. d+ + p+  n2p+ + gamma ray n2p+ = 3He 3. 3He+ + 3He+ 4He+ + 2 p+ Net Result -- 4H  1He

  22. Alternative -- CNO cycle in more massive stars > 2 Msun The CNO cycle converts hydrogen to helium The mass-12 isotope of C captures a proton and emits a gamma-ray producing the mass-13 isotope of N. N-13 is unstable and beta decays to the mass-13 isotope of C with a half-life of approximately 10 minutes. The mass-13 isotope of C captures a proton and emits a gamma-ray to become the mass-14 isotope of N. The mass-14 isotope of N captures another proton and emits a gamma-ray to become the mass-15 isotope of O. The mass-15 isotope of O undergoes a beta decay to become the mass-15 isotope of N. The mass-15 isotope of N captures a proton and emits an alpha-particle (that is, a nucleus of helium) to close the cycle and return to C-12.

  23. Beyond Hydrogen Fusion He Fusion to Carbon, Oxygen3He4 C12 C12 + He4  O16 requires 108o K C, O fusion to heavier elements up to Fe (iron) requires 5 x 108o K C12 + C12  Mg24 ,O16 + He4  Ca20

  24. The Solar Interior Hydrostatic Equilibrium (Pressure) gas pressure out = gravity in Thermal Equilibrium (Temperature) Energy (heat) in = Energy out => Energy production rate = luminosity of the star

  25. Transfer of energy Radiative (inner) and convection (outer) Random walk of photons

More Related