The History of the Spectroscope
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Diffraction Grating Experiments Warning: Never Point Any Laser Into Your Own Or Other People’S Eyes
Diffraction grating experiments Warning: Never point any laser into your own or other people’s eyes. Materials and tools Diffraction glasses (diffraction grating 1000 lines/mm) Flashlight Laser pointers (red, green, blue) Other light sources (light bulbs, arc lamps, etc.) Rulers White paper for screen Binder clips Graphing paper or computer graphing tools Scientific calculator In these experiments you will use diffraction glasses to perform measurements of light diffraction. Diffraction is a phenomenon that is due to the wave-like nature of light. Predict 1. What do you think will happen when you shine white light through a prism and why? Draw a picture to show your predictions. When white light goes through a diffraction grating (diffraction glasses), different colors are bent a different angles, similar to how they are bent be a prism. 2. (a) What do you think will happen when you shine red laser light through the diffraction glasses? (b) What do you think will happen when you shine blue laser light through the diffraction glasses? (c) Draw a picture to show your predictions. Experiment setup 1. For a projection screen, use a white wall, or use binder clips to make a white screen out of paper. 2. Use binder clips to make your diffraction glasses stand up. 3. Secure a light source with tape as needed. 4. Insert a piece of colored plastic between the source and the diffraction grating as needed. Observation 1. Shine white light through the diffraction glasses and observe the pattern projected on a white screen. Adjust the angle between the beam of light and the glasses to get a symmetric pattern as in the figure above. -
Introduction
Introduction The following two papers of Planck represent only a very small part of the historical development of our knowledge about the spectral energy distribution of electromagnetic radiation. They are the result of a long series of investigations undertaken not only by Planck (in his work on irreversible processes since 1878, and—stimulated by Maxwell's theory as developed especially by H. Hertz—on the application of thermodynamics to electromagnetic processes, from about 1891) but also by many other scientists who contributed to these experimentally and theoretically in the 19th century or earlier. Planck did not work in a vacuum. On the theoretical side, his formulations were most directly preceded by the theoretical research of Wilhelm Wien, who not only introduced the entropy of (resonator-free) radiation in 1894, but also in 1893 and 1894 discovered several regularities governing the form of the black-body radiation function introduced in 1860 by Gustav Robert Kirchhoff; in 1896 Wien found, simultaneously and independently with Friedrich Paschen, what is now called Wien's distribution law. But Planck also drew on J. H. Poynting's theorem on energy flux, as well as on the law for total radiation obtained by Josef Stefan in 1879 from measure ments of earlier authors and derived theoretically in 1884 by L. Boltzmann. Indeed, Planck may have retained as "youthful memories" his intense preoccupation, in his 19th year, with John Tyndall's works on heat radiation. On the other hand the results, as they become evident in these two papers, are only the initial steps in the direction of the quantum theory to be developed later. -
Lab 4: DIFFRACTION GRATINGS and PRISMS (3 Lab Periods)
revised version Lab 4: DIFFRACTION GRATINGS AND PRISMS (3 Lab Periods) Objectives Calibrate a diffraction grating using a spectral line of known wavelength. With the calibrated grating, determine the wavelengths of several other spectral lines. De- termine the chromatic resolving power of the grating. Determine the dispersion curve (refractive index as a function of wavelength) of a glass prism. References Hecht, sections 3.5, 5.5, 10.2.8; tables 3.3 and 6.2 (A) Basic Equations We will discuss diffraction gratings in greater detail later in the course. In this laboratory, you will need to use only two basic grating equations, and you will not need the details of the later discussion. The first equation should be familiar to you from an introductory Physics course and describes the angular positions of the principal maxima of order m for light of wavelength λ. (4.1) where a is the separation between adjacent grooves in the grating. The other, which may not be as familiar, is the equation for the chromatic resolving power Rm in the diffraction order m when N grooves in the grating are illuminated. (4.2) where (Δλ)min is the smallest wavelength difference for which two spectral lines, one of wave- length λ and the other of wavelength λ + Δλ, will just be resolved. The absolute value insures that R will be a positive quantity for either sign of Δλ. If Δλ is small, as it will be in this experiment, it does not matter whether you use λ, λ + Δλ, or the average value in the numerator. -
WHITE LIGHT and COLORED LIGHT Grades K–5
WHITE LIGHT AND COLORED LIGHT grades K–5 Objective This activity offers two simple ways to demonstrate that white light is made of different colors of light mixed together. The first uses special glasses to reveal the colors that make up white light. The second involves spinning a colorful top to blend different colors into white. Together, these activities can be thought of as taking white light apart and putting it back together again. Introduction The Sun, the stars, and a light bulb are all sources of “white” light. But what is white light? What we see as white light is actually a combination of all visible colors of light mixed together. Astronomers spread starlight into a rainbow or spectrum to study the specific colors of light it contains. The colors hidden in white starlight can reveal what the star is made of and how hot it is. The tool astronomers use to spread light into a spectrum is called a spectroscope. But many things, such as glass prisms and water droplets, can also separate white light into a rainbow of colors. After it rains, there are often lots of water droplets in the air. White sunlight passing through these droplets is spread apart into its component colors, creating a rainbow. In this activity, you will view the rainbow of colors contained in white light by using a pair of “Rainbow Glasses” that separate white light into a spectrum. ! SAFETY NOTE These glasses do NOT protect your eyes from the Sun. NEVER LOOK AT THE SUN! Background Reading for Educators Light: Its Secrets Revealed, available at http://www.amnh.org/education/resources/rfl/pdf/du_x01_light.pdf Developed with the generous support of The Charles Hayden Foundation WHITE LIGHT AND COLORED LIGHT Materials Rainbow Glasses Possible white light sources: (paper glasses containing a Incandescent light bulb diffraction grating). -
Diffraction Grating and the Spectrum of Light
DIFFRACTION GRATING OBJECTIVE: To use the diffraction grating in the formation of spectra and in the measurement of wavelengths. THEORY: The operation of the grating is depicted in Fig. 1 on page 3. Lens 1 produces a parallel beam of light from the single slit source A to the diffraction grating. The grating itself consists of a large number of very narrow transparent slits equally spaced with a distance D between adjacent slits. The light rays numbered 1, 2, 3, etc. represent those rays which are diffracted at an angle by the grating. Lens 2 is used to focus these rays to a line image at B. Notice that ray 2 travels a distance x = D sin more than 1, ray 3 travels x more than 2, etc. When the extra distance traveled is one wavelength, two wavelengths, or N wavelengths, constructive interference occurs. Thus, bright images of a monochromatic (single color) source of wavelength will occur at position B at a diffraction angle if Sin(N) = N / D where N = 0, 1, 2, 3, ... (1) The images generally are brightest for N=0 (0 = 0), and become corresponding less bright for higher N. Since, for a given value of N, the angle at which constructive interference occurs depends on , a polychromatic light source will produce a SERIES of single color bright images. There will be an image for each wavelength radiated by the source. Each image will have a color corresponding to its wavelength, and each image will be formed at a different angle. In this manner a spectrum of the light source is formed by the grating. -
25-2 the Diffraction Grating
Answer to Essential Question 25.1 (a) The only points for which changing the wavelength has no impact on the interference of the waves are points for which the path-length difference is zero. Thus, the point in question must lie on the perpendicular bisector of the line joining the sources. (b) If we re-arrange Equation 25.3 to solve for the sine of the angle, we get . Thus, decreasing the wavelength decreases sin θ, so the pattern gets tighter. Decreasing d, the distance between the sources, has the opposite effect, with the pattern spreading out. We can understand the wavelength effect conceptually in that, when the wavelength decreases, we don’t have to go as far from the perpendicular bisector to locate points that are half a wavelength (or a full wavelength) farther from one source than the other. Figure 25.3 shows the effect of decreasing the wavelength, or of decreasing the distance between the sources. Figure 25.3: The top diagram shows the interference pattern produced by two sources. The middle diagram shows the effect of decreasing the wavelength of the waves produced by the sources, while the bottom diagram shows the effect of decreasing the distance between the sources. 25-2 The Diffraction Grating Now that we understand what happens when we have two sources emitting waves that interfere, let’s see if we can understand what happens when we add additional sources. The distance d between neighboring sources is the same as the distance between the original two sources, and the sources are arranged in a line. -
7.12 Comm Mx
commentary The quantum centennial One hundred years ago, a simple concept changed our world view forever. spectrum, but did not agree with experi- tion of this experimentally successful radia- Anton Zeilinger ments for all wavelengths. Planck had the tion law from other known laws of physics, When Max Planck announced his quantum advantage of close access to the most recent but he slowly had to accept that he had found assumption in his talk at the German Physical experimental results obtained by Otto Lum- something fundamentally new. Society in Berlin on 14 December 1900, mer and Ernst Pringsheim and by Ferdinand The next important step in the early days nobody, including himself, realized that he Kurlbaum and Heinrich Rubens, also work- of quantum mechanics came in 1905, when was opening the door to a completely new ing in Berlin, on the spectral distribution of Albert Einstein introduced his radical theoretical description of nature. Quantum black-body heat radiation emerging from a hypothesis of quanta of light to explain the physics has had unsurpassed success in hole in a box kept at a certain temperature. photoelectric effect. For a while, this explaining many phenomena — from the Planck eventually found a full explana- remained the only significant instance of the structure of elementary particles, through tion, but only after forcing himself “to an act quantum being taken seriously. Einstein’s the essence of chemical bonds or the nature of of despair” by assuming that energy can only hypothesis met with strong objections from many solid-state phenomena, all the way to be exchanged between the light field inside the his contemporaries, including Planck him- the physics of the early Universe. -
Three Gratings System for the Measurement of Refractive Index of Liquids
International Journal of Applied Science and Mathematics Volume 3, Issue 3, ISSN (Online): 2394-2894 Three Gratings System for the Measurement of Refractive Index of Liquids Shyam Singh Physics Department, University of Namibia Private Bag 13301, Windhoek, NAMIBIA Fax: 264-61-206-3791 Email: [email protected] Abstract – This paper describes a very exciting method of a distance x from the third grating due to the interference finding the refractive index of liquids using a three of diffracted light from the third grating. The central point transmission diffraction gratings. An especially design glass is brighter than the other two points but the other two cell is used whose width can be changed using a railing. Light points are at equidistant from the central point as can be from a low power helium-neon laser is diffracted by a seen in Fig 1. This situation confirms the perfect transmission diffraction grating and is collimated by a lens L of short focal length. The parallel beams of light are received alignment and setup of the experiment. The distance by the second grating mounted on the first wall of the glass between the walls of the glass cell d is predetermined cell and its first order diffraction is formed on the second based on the experimental liquid and this is the only wall of the glass cell. The interference is received on a screen drawback of this experiment. However, this drawback is at a distance x from the third grating mounted on the second not so crucial as the distance d can easily be adjusted by a wall of the glass cell. -
Diffraction Grating Revisited: a High-Resolution Plasmonic Dispersive Element
1 Diffraction grating revisited: a high-resolution plasmonic dispersive element V. Mikhailov1, J. Elliott2, G. Wurtz2, P. Bayvel1, A. V. Zayats2* 1 Department of Electronic and Electrical Engineering, University College London, Torrington Place, London WC1E 7JE, UK 2 School of Mathematics and Physics, The Queen’s University of Belfast, Belfast BT7 1NN, UK Abstract The spectral dispersion of light is critical in applications ranging from spectroscopy to sensing and optical communication technologies. We demonstrate that ultra-high spectral dispersion can be achieved with a finite-size surface plasmon polaritonic (SPP) crystal. The 3D to 2D reduction in light diffraction dimensions due to interaction of light with collective electron modes in a metal is shown to increase the dispersion by some two orders of magnitude, due to a two-stage process: (i) conversion of the incident light to SPP Bloch waves on a nanostructured surface and (ii) Bloch waves traversing the SPP crystal boundary. This has potential for high-resolution spectrograph applications in photonics, optical communications and lab-on-a-chip, all within a planar device which is compact and easy to fabricate. 2 The spectral dispersion of light, that is the dependence of generalised refractive index on frequency (1), is ubiquitous in applications ranging from optical spectral devices to sensing and novel optical communication technologies (2-4). Conventionally, both prisms and diffraction gratings can be used to disperse incident light, with gratings preferred because of their high dispersion and, thus, higher spectral resolution. Optical spectroscopy based on light-wave dispersion is employed for studying the optical properties and the internal structure of materials, atoms and molecules. -
The History of the Spectroscope
Nuncius 18, fasc. 2 (2003), 808-823 AN UNCONVINCING TRANSFORMATION? MICHELSON’S INTERFERENTIAL SPECTROSCOPY Sean F. Johnston∗ Introduction Albert Abraham Michelson (1852-1931), the American optical physicist best known for his precise determination of the velocity of light and for his experiments concerning aether drift, is less often acknowledged as the creator of new spectroscopic instrumentation and new spectroscopies. His researches on the velocity of light (1878-9) and aether drift (1881-7)1 exploited his excellence in precision optical measurement and metrology. They were closely followed by work on standards of length (1887- 93) and the diameters of stars (1890-1). The measurement of the standard meter brought Michelson to the exploration of spectroscopy. He devised a new method of light analysis relying upon his favourite instrument – a particular configuration of optical interferometer – and published investigations of spectral line separation, Doppler-broadening and simple high-resolution spectra (1887-1898). Contemporaries did not pursue his method. Michelson himself discarded the technique by the end of the decade, promoting a new device, the ‘echelon spectroscope’, as a superior instrument. High-resolution spectroscopy was taken up by others at the turn of the century using the echelon, Fabry-Pérot etalon and similar instruments. Michelson’s ‘Light Wave Analysis’ was largely forgotten, but was ‘rediscovered’ c1950 and developed over the following three decades into a technique rechristened ‘Fourier transform spectroscopy’.2 -
Max Planck and the Birth of the Quantum Hypothesis
Max Planck and the birth of the quantum hypothesis Michael Nauenberg Department of Physics, University of California, Santa Cruz, California 95060 (Received 25 August 2015; accepted 14 June 2016) Based on the functional dependence of entropy on energy, and on Wien’s distribution for black- body radiation, Max Planck obtained a formula for this radiation by an interpolation relation that fitted the experimental measurements of thermal radiation at the Physikalisch Technishe Reichanstalt (PTR) in Berlin in the late 19th century. Surprisingly, his purely phenomenological result turned out to be not just an approximation, as would have been expected, but an exact relation. To obtain a physical interpretation for his formula, Planck then turned to Boltzmann’s 1877 paper on the statistical interpretation of entropy, which led him to introduce the fundamental concept of energy discreteness into physics. A novel aspect of our account that has been missed in previous historical studies of Planck’s discovery is to show that Planck could have found his phenomenological formula partially derived in Boltzmann’s paper in terms of a variational parameter. But the dependence of this parameter on temperature is not contained in this paper, and it wasfirst derived by Planck. VC 2016 American Association of Physics Teachers. [http://dx.doi.org/10.1119/1.4955146] I. INTRODUCTION of black-body radiation known as the ultraviolet catastrophe; this occurs when the equipartition theorem for a system in One of the most interesting episodes in the history of sci- thermal equilibrium is applied to the spectral distribution of ence was Max Planck’s introduction of the quantum hypoth- thermal radiation. -
Early History of Fourier Transform Spectroscopy
Infrared Phys. Vol. 24, No. 2/3. pp. 69-93, 1984 0020-0891/84 $3.00 + 0.00 Printed in Great Britain. All rights reserved Copyright !c 1984 Pergamon Press Ltd EARLY HISTORY OF FOURIER TRANSFORM SPECTROSCOPY PIERRE CONNES Service d’Akonomie du CNRS, B.P. No. 3, 91370 Verrieres-le-Buisson, France (Received 31 October 1983) Abstract-This is an attempt to explain how and why the stage was set for the appearance on the scene of Fourier transform spectroscopy (FTS) in the 1950s and not a whit before. The play begins 100 years earlier with Fizeau and Foucault who first produced high path-difference interference phenomena and used them for measuring solar spectrum wavelengths in the near IR. Next, the story unfolds with Michelson’s contribution, which led to important discoveries around 1890: the hyperfine structures and widths of atomic lines. Somewhat less well known is the Rubens interferometric technique, presented in 1910, because no such striking results were ever collected; still, it represented a distinct advance over the Michelson one. What is the reason why Michelson, Rubens and Lord Rayleigh (who made no experiments himself but understood all about them) never managed to get together and propose the modern form of FTS? Part of the responsibility we must ascribe to chance; however, sufficient motivation could not be felt as long as basic noise limitations had not been understood and closely approached. INTRODUCTION The Durham Conference has just demonstrated that Fourier transform spectroscopy (FTS) is now one of the most versatile and widely useful tools in the paraphernalia of modern optics.