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L5PresentationFive

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Published on October 19, 2007

Author: Lindon

Source: authorstream.com

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John T. McGraw, Professor Laurel Ladwig, Planetarium Manager:  Astronomy 101 Section 020 Lecture 5 The Nature of Light John T. McGraw, Professor Laurel Ladwig, Planetarium Manager Determining the Speed of Light:  Determining the Speed of Light Galileo tried unsuccessfully to determine the speed of light using an assistant with a lantern on a distant hilltop Researchers later (much later!) used rapidly spinning mirrors to accomplish this difficult task. Light travels through empty space at a speed of 300,000 km/s:  Light travels through empty space at a speed of 300,000 km/s In 1676, Danish astronomer Olaus Rømer discovered that the exact time of eclipses of Jupiter’s moons depended on the distance of Jupiter to Earth This happens because it takes varying times for light to travel the varying distance between Earth and Jupiter Light is electromagnetic radiation and is characterized by its wavelength ():  Light is electromagnetic radiation and is characterized by its wavelength () The Nature of Light:  The Nature of Light In the 1860s, the Scottish mathematician, physicist and coffee brewer James Clerk Maxwell succeeded in describing all the basic properties of electricity and magnetism in four equations This mathematical achievement demonstrated that electric and magnetic forces are really two aspects of the same phenomenon, which we now call electromagnetism Slide6:  Because of its electric and magnetic properties, light is also called electromagnetic radiation Visible light falls in the 400 to 700 nm range Stars, galaxies and other objects emit light in all wavelengths Three Temperature Scales:  Three Temperature Scales An opaque object emits electromagnetic radiation according to its temperature:  An opaque object emits electromagnetic radiation according to its temperature Visible light from stars:  Visible light from stars The wavelength at which a hot object (a metal rod or a star) emits the most electromagnetic radiation is inversely proportional to the temperature of the object. Light has properties of both waves and particles:  Light has properties of both waves and particles Newton thought light was in the form of little packets of energy called photons and subsequent experiments with blackbody radiation indicate it has particle-like properties Young’s Double-Slit Experiment indicated light behaved as a wave Light has a dual personality; it behaves as a stream of particle like photons, but each photon has wavelike properties Each chemical element produces its own unique set of spectral lines:  Each chemical element produces its own unique set of spectral lines How light is radiated:  How light is radiated Slide16:  “Fingerprinting” the elements Slide17:  Iron in our sun An atom consists of a small, dense nucleus surrounded by electrons:  An atom consists of a small, dense nucleus surrounded by electrons An atom has a small dense nucleus composed of protons and neutrons Rutherford’s experiments with alpha particles shot at gold foil helped determine the structure Slide21:  A schematic atom Slide22:  The number of protons in an atom’s nucleus is the atomic number for that particular element The same element may have different numbers of neutrons in its nucleus These three slightly different kinds of elements are called isotopes, (or “baseball players” if you are from Albuquerque) Spectral lines are produced when an electron jumps from one energy level to another within an atom:  Spectral lines are produced when an electron jumps from one energy level to another within an atom The nucleus of an atom is surrounded by electrons that occupy only certain orbits or energy level. When an electron jumps from one energy level to another, it emits or absorbs a photon of appropriate energy (and hence of a specific wavelength). The spectral lines of a particular element correspond to the various electron transitions between energy levels in atoms of that element. Balmer Lines in a Stellar Spectrum:  Balmer Lines in a Stellar Spectrum The wavelength of a spectral line is affected by the relative motion between the source and the observer:  The wavelength of a spectral line is affected by the relative motion between the source and the observer Doppler Shifts:  Doppler Shifts Red Shift: The object is moving away from the observer Blue Shift: The object is moving towards the observer Dl/lo = v/c Dl = wavelength shift lo = wavelength if source is not moving v = velocity of source c = speed of light

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