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| Electromagnetic Radiation |
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| Changing electric and magnetic fields that travel through space and transfer energy from one place to another. |
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| The distance between successive peaks or troughs of a wave. |
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| nm unit of distance equaling one-billionth of a meter 10-9 meter |
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| Limits of human vision in terms of wavelength |
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| Wavelenght where the human eye is most sensative |
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Day vision with good lighting conditions cones are used |
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tansition vision between light and dark lighting rods and cones are used |
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night vision dark lighting rods only used |
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atmospheric conditions-how steady the air is provides detail to vision |
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| how clear the skies are at a given time provides the sight of fainter things in the sky |
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| a parabolic mirror in a telescope |
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how big the lense or mirror is in a telescope bigger is better |
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| Ability of a telescope to see more detail |
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Ability of a telescope to make something seem larger least important variable of a telescope |
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used to detect radio waves made up of a dish, antenna, amplifier, and computer |
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| taking multiple telescopes to make a much the much higher resolution a large telescope would have |
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| Black with bright emission lines |
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| Emits black body radiation and is composed of the complete specturm |
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| Contains entire spectrum with dark lines |
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| a line in a spectrum at a specific wavelenght produced by the absorption or emission of light by certain atoms |
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| is a model of the proton, nuetron and electon of a molecule |
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| An atom that has lost or gained one electron |
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| same element with a different number of nuetrons |
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| Two or more atoms bonded together |
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| when an atom goes to a higher energy level or when atoms collide or absorb a proton |
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| the binding energy state of an electron |
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| The lowest permitted energy level of an electron in an atom |
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| Two ways an atom can become excited |
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When Atoms collide When atoms absorb a photon |
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Allow the sight of faint light 120 million |
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Allow the sight of color RBG 6-7 million |
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| looking out of a corner of your eye to see more |
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| The higher the temperature the shorter the wavelength or peak intensity |
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| As the temperature goes up emitted energy goes up |
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| Frequency increases coming closer making the wavelength shorter and visa versa |
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| Temperature of the Sun's surface |
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| Relativly dark spots on the sun that contain intense magnetic fields |
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| To the sun heating and cooling of gases |
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| The fine structure of bright grains coveringt he suns surface |
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The birght visible surface of the sun 500 km deep |
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| Bright gases just above the photosphere of the sun |
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| Outer atmosphere of the sun |
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| Rapidly moving atomss and ions that escape from the solar corona and blow outward through the solar system |
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| Nuclear fusion in the sun |
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| Atomic nulei running into each other to make heavier elements |
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| A series of three nuclear reactions that builds a helium atom by adding together protons. The main energy source is the sun. |
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| the rotation of a body in wich different parts of the body have different periods of rotation, like the sun |
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| The apparent change in the position of a object due to a change in the location of the observer. This allows us to mesaure the distance of stars |
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| The true amount of energy given off by a star in a given amount of time |
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| the total amount of energy a star radiates in one second |
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| Pairs of stars that orbit around their common center of mass. Gravitationally bound |
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| When you can see two stars next to each other |
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| Spectroscopic Binary Star |
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| Binary stars that can only be proven so by a spectroscopic analysis |
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| Eclipsing Binary Variable Star |
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| A binary star system in which the stars eclipse each other |
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| Mass Luminosity Relationship |
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| The more massive a star is the more luminous it is |
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| Gas and dust found between stars |
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| A cloud of glowing gas excited by ultraviolet radiation from hot stars |
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| A nebula produced by starlight reflecting off dust particals in the interstellar medium |
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| A cloud of gas and dust seen silhoueeted against a brighter nebula |
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| The process in which dust scatters blue light out of starlight and makes the stars look redder |
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| Shockwave and three causes |
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| A sudden charge in pressure that travels as an intense sound wave |
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| A group of stars that formed together and orbit a common center of mass |
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| A group of stars not gravitationally bound into clusters |
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| A collapsing cloud of dust and gas destined to become a star |
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| Pressure temperature thermostat |
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| When a star produces too much energy and expands to cool the center then contracts again to warm |
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The transfer of heat by the movement of a fluid |
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Heat transfer in the form of energy being transferred from molecule to molecule within the object |
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The transfer of energy (heat) via electromagnectic radiation |
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Stars with larger masses die quicker Stars with smaller masses die slower |
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