Term
Kirchhoff's Laws of Radiation
Law 1: Continuous Spectrum |
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Definition
| radiate at all wavelengths and thus produce a continuous spectrum. |
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Term
Kirchhoffs Laws of Radiation
Law 2: Emission Spectrum |
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Definition
| a low-density gas excited to emit light will do so at specific wavelengths |
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Term
Kirchhoff's Laws of Radiation
Law 3: Absorption Spectrum |
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Definition
| if light with continuous spectrum passes through a cool, low-density gas which absorbs them, it will produce an absorption spectrum. |
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Term
| The only thing that radiates a continuous spectrum (white light) |
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Definition
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| The one thing you need to know about a black body |
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Definition
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Definition
| motion of an object causes the wavelength to change; motion toward the observer shifts the color blue, and vice versa for red. |
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Term
| Temperature sequence classifications for stars |
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Definition
| OBAFGKM, 0-9, 0 being the hottest and so forth. |
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Definition
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| Hertzprung-Russel (H-R) Diagram |
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Definition
| star's luminosity versus the Temperature/spectral type; stars are found in specific regions of the diagram. 90% of stars fall on the Main Sequence line. |
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Definition
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Definition
| dying stars, high T/low L |
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Term
| few electrons make it to n=2 state |
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Definition
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Definition
| everything but hydrogen/helium...the others are easier to move electrons, since the outer ones are weakly bound. |
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Definition
| both stars seen in telescope, gravitational pull to each other. |
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Definition
| Doppler shift, only one star visible; SB1-one set of shifting lines...SB2=two |
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Definition
| Winking Star (demon Star) |
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Definition
| Interstellar Medium; mostly made of hydrogen (75%) and helium (25%) |
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Term
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Definition
| luminous clouds typically red in color, associated with O or B type stars. |
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Definition
| Opaque, made mostly of dust grains and complex molecules....also known as Molecular clouds. |
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Term
| Dark clouds are gravitationally stable when... |
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Definition
| outward gas pressure= inward gravitational force...they need something to initiate the cloud collapse, such as a shock wave |
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Definition
| supernova explosions, spiral arms in galaxies, collisions between clouds, between galaxies.... |
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Definition
| the beginning of the forming of a star, as it starts to collapse in on itself. |
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Definition
| small dark clouds in emission nebulae, possible sites of collapsing clouds. |
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Definition
| As cloud collapses, sun condenses in the middle, with a ring/disk of matter around it, creating planets. |
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Definition
| without H and He, formed in high T region of Solar nebula. |
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Definition
| low density, large in size, many moons and often ring systems; large atmospheres |
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Definition
| star forms in core, disk forms because of angular momentum. |
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Definition
| converting four H into one He, mass loss. |
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Definition
| heat transfer dominated by photons (heat from fire/sun |
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Definition
| energy transport dominated by gas motion (boiling pot of water) |
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Definition
| energy transport by contact (heat transferred along a metal spoon) |
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Definition
| region where photons escape the sun; Granules=convection cells, about the size of Texas. |
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Definition
| typical size of an atom; optical light= 4000A-7000A |
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Definition
| found temperature sequence in Anni Jump Cannon's spectral classification. |
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