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| There are electrons, protons, and neutrons |
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| the motion of a star across the sky |
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| The luminosity of a star is... |
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| the amount of energy it radiates each second into space |
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| The more distant an object... |
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| a photon. Sometimes it acts as a wave sometimes as a particle. |
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| Speed in terms of waves is |
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| the rate at which the peaks move |
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| is the number of peaks per second that passes the observer |
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| frequency is(in the equation) |
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| a vibrating electric field |
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| a wave in electric and manetic fields is... |
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| Electromagnetic radiation is... |
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| the speed at which the particles move |
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| a hot solid, liquid, or opague gas emits light at all wavelengths, producing a continuos spectrum |
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| Black body radiation is... |
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| the ideal case for radiation |
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| The energy emitted by a black body |
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| increases rapidly with temperature |
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| have the same number of protons and electrons |
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| are missing one or more electrons |
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| collisions with other atoms |
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| Atoms are more likely to be ionized in |
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| Hot gases because atoms move more rapidly when the temperature is high. Atoms are moving more rapidly, collisions are stronger. Ionization is more likely stronger collisions. So ionization is more likely at higher temperatures. |
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| Energy of an electron is... |
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(a constant) x (wave frequency)
the equation is E=hv |
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| When an electron jumps from a higher to a lower energy level, |
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| a photon appears and carries away the difference |
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| in black body radiation λ max = |
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| can be measured from their spectral type, from their color, and from the wavelength of the peak in their continuous spectra. |
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| is something that absorbs all the light falling on it. |
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| when a blackbody object is heated... |
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| it emits light very efficiently without any gaps or breaks in the brightness |
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| a hot, rarefied gas emits light at discrete wavelengths, creating an emission line spectrum. |
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| if light with a continuous spectrum pass through a cool, low density gas, the gas removes light at discrete frequencies, producing an absorption line spectrum. |
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| Temperature for spectral type O |
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| Temperature for spectral type B |
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| Temperature for spectral type A |
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| Temperature for spectral type F |
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| Temperature for spectral type G |
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| Temperature for spectral type K |
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| Temperature for spectral type M |
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| for the doppler effect v/c |
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| objects radial velocity/speed of light = |
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| change of wavelength/ rest wavelenth |
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| Hertsprung-Russel Diagram |
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| Each dot represents a single star |
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| In the HR(Hertzsprung Russel) Diagram why do we put the low on the right and the high on the left? |
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| Because of luminosity. The position of the dot is set by the stars luminosity and temperature. We do this for lots of stars. Every time we get this we put a dot on the diagram. The dots fall into clumps. The most important one is the one that goes from the upper left to the lower right. |
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| White dwarf sequence include about _ of all stars |
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| Red Giants are _ of all stars |
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| are extremely rare and can have a luminosity of 10^6 times greater than the sun. |
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| electrons are normally found in there lowest level because they spontaneously jump to lower levels. But they do take time to jump, so they can sometimes be found in a higher level than normal. |
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