| Term | Definition |
|---|
| List 5 things that can be determined by a star's light and how each is measured | 1) Temperature – Wein Displacement Law 2) Size – Eclipsing Binary 3) Companion – Periodic Doppler Shift 4) Spin – Doppler shift is broad 5) Magnetic Field – Zeeman Effect |
| Zeeman Effect | The splitting of a spectral lines in a magnetic fieldStefan-Boltzman Law ; E=σT |
| Give the Wein Displacement Law and the Stefan-Boltzman Law and what they mean | F=CT – The Frequency of the light emitted by a star is related to its temperature. |
| How many forces are needed to have stars and planets? How are they related? | 1) Strong – A short range powerful force. 2) Electric – Long range repulsive medium power. 3) Gravity – Long Range, adds, low power. |
| Black Body | An object which emits as much energy as it absorbs. |
| Why is the Sun a Black Body? | Energy is created by fusion in the core. It must then travel to the surface. Since the Sun's output is constant it must be a Black Body. |
| Using Conservation laws, show Neutrinos must exist | (ask prof) |
| Hadron | A particle that 'sees' the Strong Force (A set of rules) |
| Conservation Laws | Some aspect that is always true in any interaction. (Draw Diagram) |
| Lepton | A non-Hadron associated with the weak force. |
| Draw the binding energy curve and explain | When atoms add or subtract Hadrons their predicted mass will be more, or less, than the measured mass (Draw Diagram) |
| Discuss the Cl » Argon Experiment | You take a tank of Chlorine whose binding energy in relation to Argon is exactly equal to the energy produced for solar Neutrinos. Argon was observed but only about 1/3 of the predicted rate. |
| Discuss the 1987A Nova and its connection to Neutrinos | A nova should produce many Neutrinos. When the 1987A Nova happened, several events occurred, all at the same time and from the same direction. |
| Discuss how Protons and Neutrons 'see' each other | There should be an exchange particle (Pion) that has a predicted mass and must have ' +, -, 0 (Zero) ' charge states, and is exchanged by the rules of the Strong Force. |
| List the three types of radiation and what is usually associated with each type | Alpha – Stripped He (Helium) nucleus fission. Beta – High speed electron neutron delay. Gamma – High energy photon level shift in the nucleus. |
| Discuss the single electron experiment and draw a diagram | If we do not detect which slit an electron uses we get a wave pattern. If we detect the slit The electron uses we get a particle pattern. (Draw Diagram) |
| Discuss the concept of Schrodinger's Cat | It is the observer that 'forces' a system in one of several possible states by doing an experiment. |
| For the non-relativistic case find the wavelength of an electron. Why is this accepted? | Energy "Particle" – E = ½MC² : Energy "Wave" – E = hf : Velocity – C = fλ : Wavelength – 2h/mc : Accepted because we can build electron microscopes. |
| Draw the HR diagram. | (Draw Diagram) |
| Absolute Magnitude | How bright a star is when 10 Parsecs distant. |
| Parsec | The distance to a star that has a Parallax of 1 second of Arc. |
| Light Year | The distance light travels in one year.Apparent Magnitude ; How bright a star appears. |
| Discuss Discrete Spectra | Since electrons are wave/particle, their 'wavelengths' must fit the requirement λ=2∏R as such only a few Radii are possible. Thus only specific energies are emitted. |
| List the major methods of determining Stellar Distances with the needs and range of each method | 1) Parallax – Trigonometry, but limited to ~100 Parsecs. Spectral Parallax to ~10,000 Parsecs. 3) Cepheid Variables to ~ 1,000,000 Parsecs, must see light. Hubble Red Shift measures Doppler shift to ~ 15 billion Parsecs. |
| Draw a Diagram and Discuss Parallax. (Not spectral parallax) | Using our orbit as a baseline we build a triangle which gives us the distance (D) to the star. (Draw Diagram) |
| Parallax | The apparent shift of position due to distance. |
| Discuss Spectral Parallax | A) Using spectra we determine the 'class' of a star. B) Using the HR diagram we determine the Absolute Magnitude. C) We compare Absolute Magnitude to the Apparent Magnitudes which gives us a distance. |
| Draw an HR diagram. Pick any star and determine what its apparent magnitude would be @ 1,000 Parsecs. | (Draw Diagram) |
| Draw a diagram and discuss an Eclipsing Binary | From Kepler's Laws we find the Velocity of the star. This gives us the size of the star. Thus we are able to define Red Giants and White Dwarfs. |
| List the layer of the Sun and what is found in each layer. | Photosphere – Essentially the surface of the sun, 'finds Granules' : Chromospheres – The atmosphere of the sun. 'finds Fraunhofer Lines' : Corona – Upper region of the sun. 'finds Lorentz Law' |
| Granule | A convection cell of the sun (think Grits) |
| Fraunhofer Lines | The absorption lines in the spectra of the sun. |
| Discuss the impact of the low sunspot numbers on the earth | Since the Lorentz Force Law states 'F = qv x B (note a right arrow above each variable) ' If there are few sunspots, the energy arriving at the earth is less. |
| Draw and discuss the Butterfly diagram | Every 11 years the sun goes from a minimum to a maximum, this gives the ' Butterfly Diagram '. |
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