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ELECTROMAGNETIC SPECTRUM,[object Object],SPECTROSCOPY AND DOPPLER WAVE,[object Object]
Other light characteristics,[object Object],All radiant energy travels through the vacuum of space in a straight line at the rate of 300, 000 kilometers.,[object Object],1 day = 26 billion kilometers. ,[object Object]
Other light characteristics,[object Object],Photon,[object Object],A quantum of visible light. (Quantum – smallest quantity of energy),[object Object],A photon has neither mass nor electrical charge.,[object Object],A photon possesses energy and momentum.,[object Object],A photon can exert pressure on matter. (Radiation pressure),[object Object],Responsible for “pushing” material away from a comet to produce its tail.,[object Object]
Comet Hale-Bopp,[object Object]
SPECTROSCOPY,[object Object],Spectroscopy – study of the properties of light that depend on wavelength.,[object Object],Newton’s study on prism initiated this study.,[object Object],Also defined as the study of spectra, especially to determine the chemical composition of substances and the physical properties of molecules, ions and atoms.,[object Object]
SPECTROSCOPY,[object Object],Spectroscope,[object Object],Instrument for studying spectra; an instrument for dispersing light usually light in the visible range, into a spectrum in order to measure it.,[object Object]
SPECTROSCOPY,[object Object],Three types of spectrum:,[object Object],1. Continuous spectrum,[object Object],2. Dark-line spectrum ,[object Object],(Absorption spectrum),[object Object],3. Bright-line spectrum,[object Object],(Emission spectrum),[object Object]
SPECTROSCOPY,[object Object],1. Continuous spectrum,[object Object],Is produced by an incandescent solid, liquid or gas under high pressure.,[object Object],Consists of an uninterrupted band of color.,[object Object],E.g. Common light bulb,[object Object]
Spectrum,[object Object]
SPECTROSCOPY,[object Object],2. Dark-line spectrum (Absorption spectrum),[object Object],Is produced when “white” light is passed through a comparatively cool gas under low pressure.,[object Object],Gas absorbs selected wave length of light so the spectrum that is produced appears as a continuous spectrum, but with a series of dark lines.  ,[object Object]
Spectrum,[object Object]
SPECTROSCOPY,[object Object],3. Bright-line spectrum (Emission spectrum) ,[object Object],It is a series of bright lines of particular wavelengths, depending on the gas that produces them.,[object Object],These bright lines appear in the exact location as the dark lines that are produced by this gas in a dark-line spectrum (absorption).,[object Object]
Spectrum,[object Object]
SPECTROSCOPY,[object Object],Most stars have dark line spectra.,[object Object],Each element produces a unique set of spectral lines.,[object Object],Each spectrum acts as a “finger print” of a star and is used to identify the element present.,[object Object]
SPECTROSCOPY,[object Object],Spectrum of a star (sun) explained in an overly simplified manner: ,[object Object],Central region – high pressure and high temperature – continuous spectrum.,[object Object],Outer region – low pressure and low temperature – dark-line spectrum.,[object Object],Dark lines in the spectrum are absorbed light. ,[object Object]
SPECTROSCOPY,[object Object],The spectrum of the sun contains thousands of dark lines.,[object Object],Over 60 elements have been identified by matching those lines with those of elements known on Earth.,[object Object]
SPECTROSCOPY,[object Object],TWO FACTORS CONCERNING A RADIATING BODY,[object Object],1. If the temperature of a radiating surface is increased, the total amount of energy emitted is increased.,[object Object],*Stefan Boltzman Law,[object Object],The energy radiated by a body is directly proportional to the fourth power of its absolute temperature.,[object Object],E.g. Star – Temperature doubled – energy emitted times 2 raise to 4 (16 times more energy.),[object Object]
SPECTROSCOPY,[object Object],TWO FACTORS CONCERNING A RADIATING BODY,[object Object],2. As the temperature of an object increases, a larger proportion of its energy is radiated at shorter wavelengths.,[object Object],E.g. Heated Metal rod,[object Object],Red – longer wavelength – hot,[object Object],Blue – shorter wavelength – hotter,[object Object],Red stars – hot,[object Object],Blue stars - hotter,[object Object]
DOPPLER EFFECT,[object Object],Doppler effect,[object Object],Explained by Christian Doppler in 1842.,[object Object],change in frequency because of motion: a perceived change in the frequency of a wave as the distance between the source and the observer changes. ,[object Object]
DOPPLER EFFECT,[object Object],When a light source is moving away, its light appears redder than it actually is.,[object Object],The reason for it is that the wavelength is stretched.,[object Object],Objects approaching have their wavelength waves shifted toward blue (shorter wavelength).,[object Object]
Sodium lines,[object Object]
DOPPLER EFFECT,[object Object],Case analysis:,[object Object],If a source of light is approached you at a very high speed (near the speed of light),,[object Object],It would appear blue.,[object Object],If you move with a speed of light the color of a stationary light source will appear blue. ,[object Object]
DOPPLER EFFECT,[object Object],By using the Doppler effect,[object Object],It reveals weather Earth is approaching or receding from a star or another celestial body.,[object Object],The amount of shift allows to recalculate the rate at which the relative movement is occurring.,[object Object],Larger Doppler shifts indicate higher velocities.,[object Object],It is generally measured in from dark lines in the spectra of stars by comparing them with a standard spectrum produced in the laboratory.  ,[object Object]
END OF PRESENTATION,[object Object]

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