astronomy

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Created by:

meredith245  on November 30, 2010

Subjects:

geology

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astronomy

1905
current understanding of nature of light emerged
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1905 current understanding of nature of light emerged
einstein showed that light sometimes behaves as particles and sometimes as waves
wave model wavelengths of radiation vary
white light consists of several wavelengths corresponding to the colors of the rainbow
particle model exert a pressure called radiation pressure on matter
photons particles
particle model shorter wavelengths correspond to more energetic photons
light comes from movement of electrons in atoms
nucleus contains protons and neutrons
element atoms with the same number of protons
isotopes atoms with varying numbers of neutrons
ions atoms with varying numbers of electrons
spectral lines when electron jumps form one energy level to another
186,000 m/s speed of light
visible light only one small part of an array of energy
electromagnetic radiation gamma rays, x-rays, UV light, visible light, infrared light, radio waves
visible light only one type of electromagnetic radiation emitted by stars
each type of EM radiation travels at exactly the same speed (speed of light)
peak color (wavelength) shifts to shorter wavelengths as an object is heated
wavelength inversely proportional to temperature
sun emits all colors
sun most intensely emits blue-green part of spectrum
temperature learned by analyzing starlight
chemical composition learn by analyzing starlight
spectroscopy study of properties of light that depend on wavelength
spectrum light pattern produced by passing light through a prism which spreads out the various wavelengths
continuous spectrum produced by an incandescent solid, liquid, or high pressure gas
continuous spectrum uninterrupted band of color
dark-line (absorption) spectrum produced when light is passed through a comparatively cool, low pressure gas
dark-line (absorption) spectrum appears as a continuous spectrum but with dark lines running through it
bright-light (emission) spectrum produced by a hot (incandescent) gas under low pressure
bright-light (emission) spectrum appears as a series of bright lines of particular wavelengths depending on the gas that produced them
dark-line (absorption) spectrum most stars have
spectroscope instrument used to spread out the light
emission and absorption spectra allow astronomers to determine the elements present in a distant star
each chemical element produces its own unique set of spectral lines when it burns
brightness of spectral lines depend on conditions in spectrum's source
continuous spectrum produced by a hot,dense gas or object - is a complete rainbow of colors without any specific spectral lines
emission line spectrum produced by hot, rarefied gas - series of bright spectral lines against a dark background
absorption line spectrum produced by a cool gas in front of a continuous light - series of dark spectral lines among the colors of the rainbow
movement learned by analyzing starlight
doppler shift allows astronomers to measure radial velocity
spectral lines shift due to relative motion between the source and the observer
doppler effect apparent change in wavelength of radiation caused by the relative motions of the source and observer
doppler effect used to determine increasing distance (wavelength stretches)
doppler effect used to determine decreasing distance (wavelength compresses)
velocity larger doppler shifts indicate higher velocities
red shift distance between the observer and the sources is increasing
blue shift distance between the observer and the source is decreasing
radial velocity learned by analyzing starlight
different types of EM radiation require different types of telescopes
refracting telescope uses a lens to concentrate incoming light
reflecting telescope uses mirrors to concentrate incoming starlight
not all EM radiation can penetrate earth's atmosphere

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