DOC PREVIEW
UW ASTR 101 - The Sun

This preview shows page 1-2 out of 5 pages.

Save
View full document
View full document
Premium Document
Do you want full access? Go Premium and unlock all 5 pages.
Access to all documents
Download any document
Ad free experience
View full document
Premium Document
Do you want full access? Go Premium and unlock all 5 pages.
Access to all documents
Download any document
Ad free experience
Premium Document
Do you want full access? Go Premium and unlock all 5 pages.
Access to all documents
Download any document
Ad free experience

Unformatted text preview:

11The SunThe SunOur star - inside and out2EarEarth having a really, really bad day.th having a really, really bad day.3Explain the proton-proton cycle in easy-to-understand language.State how radiation is transported through eachregion of the Sun’s interiorExplain how the Sun maintains a constantbalance in its interior (solar thermostat)Learning Goals:Learning Goals:24LIGHT!LIGHT!5•1H + 1H --> 2H + e+ + neutrino•2H + 1H --> 3He + gamma ray•3He + 3He --> 4He + 1H + 1HCoreCoreνγMustoccurtwiceExplain the proton-proton cycle in easy-to-understand language.Proton-Proton Cycle0.007 of original mass is converted to energye-2 γ6Protons must collide at high velocities:Temperature must be > 10,000,000 KelvinPlasma must be extremely dense.++I hate you,proton. You areso repulsive.You reek! Stayaway, youpositive jerk.Explain the proton-proton cycle in easy-to-understand language.37 Explain the proton-proton cycle ineasy-to-understand language.a. Two helium-3 nuclei collide andfuse to form the more commonform of the element: helium-4.b. At the instant the nuclei fuse andcreate a deuterium nucleus, apositron and a neutrino arecreated.c. Two protons (H nuclei) meet underthe extreme conditions present inthe core of the Sun.d. Positron + electron = annihilation;masses convert to energy in formof 2 gamma ray photons.e. Two extra protons are released,available for further nuclearreactions.f. In about 6 seconds a 3rd protonfuses with deuterium nucleus toform He-3 + gamma ray.8PASS YOUR SHEETS TO THEPASS YOUR SHEETS TO THECENTER AISLECENTER AISLEDEMONSTRATION OF THERANDOM WALK WILL TAKEPLACE WHILE YOU AREHANDING IN YOUR SHEETS.http://en.wikipedia.org/wiki/Random_walk9Random WalkState how radiation is transported through each region of the Sun’s interiorRadiative Radiative ZoneZone410CONVECTION MOVIEState how radiation is transported through each region of the Sun’s interiorGranulationConvection ZoneConvection Zone1112State how radiation is transported through each region of the Sun’sinterior513Another way of thinking about this:Another way of thinking about this:TheThe Solar Thermostat Solar ThermostatExplain how the Sun maintains a constant balance in its interior (solar thermostat)Hydrostatic (gravitational) equilibrium in the Sunmaintains a constant balance between inward-pushing gravity and outward-pressing pressure.14Number of particles in core is decreasing.Number of particles in core is decreasing.NET RESULTNET RESULTIN: 6 H OUT: 1 He + 2 HIN: 6 H OUT: 1 He + 2 HExplain how the Sun maintains a constant balance in its interior (solar thermostat)15Explain how the Sun maintains a constant balance in its interior(solar


View Full Document

UW ASTR 101 - The Sun

Documents in this Course
Galaxy

Galaxy

12 pages

Load more
Download The Sun
Our administrator received your request to download this document. We will send you the file to your email shortly.
Loading Unlocking...
Login

Join to view The Sun and access 3M+ class-specific study document.

or
We will never post anything without your permission.
Don't have an account?
Sign Up

Join to view The Sun 2 2 and access 3M+ class-specific study document.

or

By creating an account you agree to our Privacy Policy and Terms Of Use

Already a member?