B. Sc. II YEAR Optics

Total Page:16

File Type:pdf, Size:1020Kb

B. Sc. II YEAR Optics BBSCPH202 B. Sc. II YEAR Optics DEPEPARTMENT OF PHYSICS SCSCHOOL OF SCIENCES UTTARARAKHAND OPEN UNIVERSIRSITY Programme Coordinator and Board of Studies Board of Studies Prof. P. D. Pant Prof. C.K. Ghosh, Director I0C School of Sciences Regional Director, Regional Services Division, I.G.N.O.U., New Delhi Uttarakhand Open University, aldwani Prof. R. C. Srivastva, Prof Awadhesh Kumar Rai, Professor and ead, Department of Physics, Department of Physics, CBS , G.B.P.U.1.3T. Pantnagar, India University of 1llaha2ad, 1llaha2ad Dr. Kamal Devlal (Programme Coordinator) Department of Physics School of Sciences, Uttarakhand Open University, aldwani Unit writing and Editing Editing Writing Dr. M. Sharma 1. Dr. Piyush Sinha Department Physics Department Physics Pt. L.M.S. Govt. P.G. College. NB University Campus, Pauri, Uttarakhand Rishikesh, Uttarakhand 2. Dr. Kamal Devlal Department of Physics School of Sciences, Uttarakhand Open University, aldwani 3. Dr. M. Sharma Department Physics Pt. L.M.S. Govt. P.G. College. Rishikesh, Uttarakhand 4. Dr. Santosh K. Joshi Department Physics University of Petroleum and Energy Studies, Prem Nagar, Dehradun-24,00., Uttarakhand Dr. C. C. Dhondiyal Department Physics M.B. G.P.G.C. aldwani, Nainital, Uttarakhand Dr. B S iwari Department Physics University of Petroleum and Energy Studies, Prem Nagar, Dehradun-24,00., Uttarakhand Course itle and code ,ptics (BSCP-.0.) ISBN No. Copyright Uttara0hand ,pen University Edition .012 Published by Uttara0hand ,pen University, -aldwani, Nainital3 .43139 Printed by BSCP-202 ,P ICS DEPAR MEN ,7 P-8SICS SC-,,9 ,7 SCIENCES U ARAK-AND ,PEN UNI:ERSI 8 Phone No. 059443.411.., .411.3 oll free No. 120012040.5 7ax No. 059443.44.3., E. mail [email protected] htpp://uou.ac.in Contents / ,ptics / . /tI / Unit Bloc0 and Unit itle Page number number Bloc0 1: Geometrical optics 1359 1 13.. 7ermatAs principle and its Applications: Optical Path, 5ermat6s principle of E7treme Path,applications of 5ermat6s principle, to deduce law of reflection and refraction etc., Gauss8s general theory of image formation. Refraction by spherical surfaces and Image formation9 Sign Convention, Coa7ial .3341 Optical System , Cardinal Points of an Optical System , Rules of Image 5ormation Magnification of a lens system, elmholt: Lagrange8s Magnification 5ormula Some Important Relations, Newton8s 5ormula 3 4.359 hic0 lens, lenses combinations and telescopes9 Cardinal Points of a Thick Lens, 5ocal Length of a Thick Lens, Variation of 5ocal Length of a Thick Bi-conve7 Lens, Power of a Thick Lens, Telescopes, 1stronomical Telescope, Terrestrial Telescope, Newtonian Reflecting Telescope, Cassegrain Reflecting Telescope, 1dvantages of Reflecting Type Telescope over Refracting Type Telescope B9,CK . Interference of light waves 403112 4 40324 Interference of light: Wave Nature of Light, Principle of Superposition, Introduction to Interference of light, Classification of Interference, Young8s e7periment, coherence Length and Coherence Time, spatial and temporal coherence; Interference Due to Thin Sheet ,intensity distri2ution, 2iprism and 5resnel8s 2iprism, E7perimental 1rrangement of Biprism 1pparatus, Lateral Shift, Measurement of Wave Length of Light (@A 2y 5resnel8s Biprism, Interference with White Light 5 25310C Interference in thin film and NewtonBs rings 9 Interference 2y division of amplitude, interference in thin film, wedge shaped film, Necessity of E7tended Source for Interference Due to Thin 5ilms , Colours of Thin 5ilms, Classification of 5ringes, 5ringes of EBual Thickness, 5ringes of EBual Inclination, Newton8s rings in reflected and refracted light, E7periment 1rrangement for Reflected Light, 5ormation of Bright and Dark Rings, Diameter of Bright and Dark Rings, Determination of Wavelength of a Monochromatic Light Source, Determination of Refractive Inde7 of a LiBuid 2y Newton8s Rings E7periment, Newton8s Rings in Case of Transmitted Light 4 1023112 Multiple beam interferometry9 Interferometery, 5ringes of EBual Inclination ( aidinger 5ringesA, Michelson8s Interferometer, Construction, Working, 5ormation of 5ringes, Determination the Difference 2etween Two Neigh2oring Wavelengths, Determination of Refractive Inde7 of a Material, Michelson- Morley E7periment and Its Result B9,CK3 Diffraction of light waves 11931C4 C 1193144 Diffraction of light waves and 7resnel diffraction: Diffraction of Light, Difference 2etween Interference and Diffraction, ypes of diffraction, 5resnel and 5raunhofer class, 5resnel8s half period :ones; e7planation of rectilinear propagation of light; Rectilinear Propagation of Light, :one plate, comparison of :one plate with lens, wave front, diffraction at a straight edge. 2 7raunhofer diffraction9 Condition for 5raunhofer diffraction, 5raunhofer 14C314. diffraction due to a single slit, 5raunhofer diffraction due to dou2le slit, 5raunhofer diffraction at circular aperture (BualitativeA, Plane diffraction grating (transmissionA, diffraction due to a grating of N parallel slits, Ma7imum num2er of order availa2le in a grating, missing orders. 9 Resolution and resolving power9 Introduction, resolving power, Rayleigh 14331C4 criterion of resolution; resolving power of transmission grating, resolving power of prism, resolving power of telescope, resolving power of microscope. B9,CK 4: PolariDation of light waves 1C53.50 10 1C5319. PolariDation: Introduction to Polari:ation, Types of Polari:ation, Concept of plane polari:ed light, Pictorial Representation of Plane Polari:ed Light , Plane of Vi2ration and Plane of Polari:ation of Plane Polari:ed Light, Methods of Production of Plane Polari:ed Light, Plane Polari:ed Light 2y Reflection, circularly and elliptically polari:ed light, Malus law, Brewster law. 11 Double refraction: Dou2le Refraction or Birefringence, Geometry of Calcite 1933.14 Crystal, Optic 17is, Principal Section and Principal Plane, Optic 17is, Principal Section and Principal Plane, uygen8s E7planation of Dou2le Refraction in Unia7ial Crystal, Positive and Negative Crystals, Nicol Prism 1ction of Polari:er on Light of Different Type of Polari:ations, uygen8s construction for unia7ial crystals; Dou2le Images Polari:ing Prisms, Dichroism or Selective 12sorption, polaroids and their uses, Polari:ation 2y Scattering. 1. Plane, circularly and elliptically PolariDed light9 Introduction, retardation plates, .1C3.33 Production and analysis of plane, circularly and elliptically polari:ed light 2y retardation plates, E7perimental 1rrangements for the Production of Polari:ed Light , C1pplication of Retardation Plates9 1nalysis of Polari:ed Light ,and Rotatory polari:ation. 13 .343.50 ,ptical activity9 Introduction, rotatory polari:ation, optical activity; Laevo-rotatory Su2stances, De7tro-rotatory Su2stances, 5resnel8s e7planation of optical activity; Specific Rotation, Polarimeters, BiBuart: and Laurent8s half shade polarimeter. B9,CK 5: ,ptical Instruments and Aberration in images: .513301 14 ,ptical Instruments: Introduction, uman eye, field of view, need of multiple lens .513.20 eyepieces, Ramsden8s eyepiece, uygen8s eyepiece, Gaussian eyepiece, comparisons o pieces, Spectrometer, electron microscope. 15 Aberration in images9 Introduction, 12erration in images, chromatic a2erration of lens.213301 achromatic com2ination of lenses, monochromatic a2erration, spherical mirrors, Other Monochromatic 12erration and Their Elimination, Spherical Mirrors, Schmidt correcto plate, oil immersion lens. htL/ ./tI UNIT 1: FERMAT‘S PRINCIPLE AND ITS APPLICATION CONTENTS 1.1 Introduction 1.2 Objectives 1.3 Optical Path 1.3.1 Optical path Time Interval 1.4 Fermat‘s Principle of Extreme Path 1.5 Application of Fermat‘s Principle 1.5.1 Laws of Reflection 1.5.2 Laws of Refraction 1.5.3 Refractive Index 1.5.4 Total Internal Reflection 1.6 (auss General Theory of Image Formation 1.7 ,ummary 1.8 (lossary 1.9 References 1.10 ,uggested Readings 1.11 Terminal Questions 1.12 Answers 544!2!+(!.$ /0%. 5.)6%23)49 0°• htL/ ./tI 1.1 INTRODUCTION Light is a form of energy that enables us to see and perceive objects with our eyes. ,cientifically1 light is an electromagnetic wave of wavelength belonging to visible part 2wavelength of 400 nm to 750 nm3 of electromagnetic spectrum. 4e see objects either by the light they produce or by the light they reflect from other objects. Objects that produce their own light are said to be luminous. xamples are the sun, electric bulbs, candle light etc., whereas, non luminous objects do not produce their own light. 4e can see these objects only when light fall on them from other sources and it is thrown bac5 or reflected into our eyes. An important example is that of the moon, which shines in the night because it reflects light coming from the sun and not because it is luminous. Optics is the science or more specifically a branch of physics in which we study the behavior and properties of light. The study also includes the interaction of light with matter and construction of instruments that use or detect it. For the sake of convenience the subject of optics can be divided into two parts6 2i3 physical or wave optics1 which deals with the wave nature of light. It accounts for optical effects such as diffraction and interference etc., and 2ii3 geometrical or ray optics1 which deals with the formation of images by lenses and mirrors and their combinations on the basis of certain geometrical laws obeyed by light. The present block of the course 7optics‘ is dedicated to the geometrical optics only hence, in the following sections, we will concentrate on its learning
Recommended publications
  • The Telescope Lenses, Which Turned the Image Upside Down but Improved the Clarity Dramatically
    The image produced by the first refracting telescope was Name right side up. However, the clarity of the image was less than ideal. Johannes Kepler worked to improve the image produced by the refracting telescope. He used two convex The Telescope lenses, which turned the image upside down but improved the clarity dramatically. His design soon became popular By Phyllis Naegeli and remains in use today. Do you like to lie on your back and gaze One problem associated with the refracting telescope was at the stars? What constellations can you the rainbow halo it produced around the object in view. Sir name? Have you ever used a telescope to Isaac Newton did not care for the halo produced by the get a closer look at the universe? Do you refracting telescope. He set out to improve the design, know how a telescope works? which led him to work on the reflecting telescope. The design used a curved mirror to collect light from an object. A telescope is used to see distant objects A secondary flat mirror reflected the image to the side of up close. There are two basic types of the tube where it is viewed through an eyepiece. Newton telescopes - the refracting telescope and also used a shorter, fatter tube allowing magnification to be the reflecting telescope. Each will help increased by using larger mirrors. Newton's design you to see the planets, moon, or stars. Both eliminated the rainbow halo produced by the convex lenses use a tube and have an eyepiece to focus the image for you of the refracting telescope.
    [Show full text]
  • 5 10 15 20 25 30 35 Class 359 Optical: Systems And
    CLASS 359 OPTICAL: SYSTEMS AND ELEMENTS 359 - 1 359 OPTICAL: SYSTEMS AND ELEMENTS 1 HOLOGRAPHIC SYSTEM OR ELEMENT 197.1 .Using a periodically moving 2 .Authentication element 3 .Having particular recording 198.1 ..With particular mount or driver medium for element 4 ..Recyclable 199.1 ...Oscillating driver 5 ...Magnetic material 199.2 ....Electrostatically driven 6 ...Sandwich having photoconductor 199.3 ....Electromagnetically driven 7 ...Crystalline material 199.4 ....Electromechanically driven 8 ..Having nonplanar recording 200.1 ...Bearing or shaft for rotary medium surface driver 9 .For synthetically generating a 200.2 ....Specific shaft material or hologram structure (e.g., ceramic ring) 10 .Using modulated or plural 200.3 .....Grooved shaft reference beams 200.4 ....Fluid pressure bearing 11 ..Spatial, phase or amplitude 200.5 .....Dynamic fluid bearing modulation 200.6 ...Electrostatic driver 12 .Copying by holographic means 200.7 ...Electromagnetic driver 13 .Head up display 200.8 ...Electromechanical driver 14 ..Holograph on curved substrate 201.1 ..With multiple scanning elements 15 .Using a hologram as an optical (e.g., plural lenses, lens and element prism, etc.) 16 ..With aberration correction 201.2 ...Reflective element (e.g., 17 ..Scanner mirror, reflector, etc.) 18 ...Flat rotating disk 202.1 ...X-Y scanners 19 ..Lens 203.1 ...Having a common axis or 20 ...Multiple point hologram (e.g., rotation fly-eye lens, etc.) 204.1 ..Utilizing multiple light beams 21 .Having defined page composer 204.2 ...Including modulated light
    [Show full text]
  • Spherical Mirror Parabolic Mirror Ray Diagrams for Mirrors
    Ray Diagrams for Mirrors September 8, 2015 1:24 PM Light rays travel in straight lines and so when we see one we assume it is coming straight towards us. But as physics students we know that light can be refracted and bent. Plane Mirror Object Image Plane mirrors form images at the same distance to the mirror as the object. This image is a virtual image as it is behind the mirror and impossible to project on a piece of paper in the real world. Question: Do we see more of ourselves as we get closer to the mirror or less? Question: What size of mirror do we need to see all of ourselves? Question: In a plane mirror is the images height larger, smaller or equal to the objects? Plane Mirrors: Are flat reflective surfaces that create a virtual image with the same height as the object and at the same distance from the mirror as the object. Concave Mirrors These are mirrors that are curved with their outer edges closer to you then their centers. Just like a parenthesis ")". They reflect light towards their focal points. The most ideal curved mirror is a Parabolic Mirror but these are extremely difficult to produce accurately. Most Parabolic Mirrors are approximations created from taking a small portion of a spherical mirror. Parabolic Mirror Spherical Mirror Optics Page 1 Parabolic Mirror Spherical Mirror Principal Axis = focal point = center of circle Convex Mirrors Convex Mirrors are just the opposite of a concave mirror. They are like a backwards parenthesis "(". They reflect light away from the mirrors focal point, which is located on the back side of the mirror.
    [Show full text]
  • 25 Geometric Optics
    CHAPTER 25 | GEOMETRIC OPTICS 887 25 GEOMETRIC OPTICS Figure 25.1 Image seen as a result of reflection of light on a plane smooth surface. (credit: NASA Goddard Photo and Video, via Flickr) Learning Objectives 25.1. The Ray Aspect of Light • List the ways by which light travels from a source to another location. 25.2. The Law of Reflection • Explain reflection of light from polished and rough surfaces. 25.3. The Law of Refraction • Determine the index of refraction, given the speed of light in a medium. 25.4. Total Internal Reflection • Explain the phenomenon of total internal reflection. • Describe the workings and uses of fiber optics. • Analyze the reason for the sparkle of diamonds. 25.5. Dispersion: The Rainbow and Prisms • Explain the phenomenon of dispersion and discuss its advantages and disadvantages. 25.6. Image Formation by Lenses • List the rules for ray tracking for thin lenses. • Illustrate the formation of images using the technique of ray tracking. • Determine power of a lens given the focal length. 25.7. Image Formation by Mirrors • Illustrate image formation in a flat mirror. • Explain with ray diagrams the formation of an image using spherical mirrors. • Determine focal length and magnification given radius of curvature, distance of object and image. Introduction to Geometric Optics Geometric Optics Light from this page or screen is formed into an image by the lens of your eye, much as the lens of the camera that made this photograph. Mirrors, like lenses, can also form images that in turn are captured by your eye. 888 CHAPTER 25 | GEOMETRIC OPTICS Our lives are filled with light.
    [Show full text]
  • Curved Mirror - Wikipedia
    2018/11/5 Curved mirror - Wikipedia Curved mirror A curved mirror is a mirror with a curved reflecting surface. The surface may be either convex (bulging outwards) or concave (bulging inwards). Most curved mirrors have surfaces that are shaped like part of a sphere, but other shapes are sometimes used in optical devices. The most common non-spherical type are parabolic reflectors, found in optical devices such as reflecting telescopes that need to image distant objects, since spherical mirror systems, like spherical lenses, suffer from spherical aberration. Distorting mirrors are used for entertainment. They have convex and concave regions that produce deliberately distorted images. Contents Convex mirrors Uses of convex mirror Image Concave mirrors Reflections in a spherical convex Uses mirror. The photographer is seen Image reflected at top right Mirror shape Analysis Mirror equation, magnification, and focal length Ray tracing Ray transfer matrix of spherical mirrors See also References External links Convex mirrors A convex mirror, diverging mirror, or fish eye mirror is a curved mirror in which the reflective surface bulges toward the light source.[1] Convex mirrors reflect light outwards, therefore they are not used to focus light. Such mirrors always form a virtual image, since the focal point (F) and the centre of curvature (2F) are both imaginary points "inside" the mirror, that cannot be reached. As a result, images formed by these mirrors cannot be projected on a screen, since the image is inside the mirror. The image is smaller than the object, but gets larger as the object approaches the mirror. A collimated (parallel) beam of light diverges (spreads out) after reflection from a convex mirror, since the normal to the surface differs with each spot on the mirror.
    [Show full text]
  • Location of Cardinal Points from the ABCD Matrix for the General Optical System
    EE482 Fall 2000 Handout #2 Page 1 Location of Cardinal Points from the ABCD Matrix for the General Optical System I II n1 n2 F1 P1 N1 P2 N2 F2 f1 f2 Figure 1 Cardinal points of a system which is characterized by an ABCD matrix between an input plane I and an output plane II. Cardinal Point Measured Function Special Case From To (n1=n2) First Focal Point P1 F1 -n1/(n2C)-1/C First Principle Point I P1 (n1-n2D)/(n2C)(1-D)/C First Nodal Point I N1 (1-D)/C (1-D)/C Second Focal Point P2 F2 -1/C -1/C Second Principle Point II P2 (1-A)/C (1-A)/C Second Nodal Point II N2 (n1-n2A)/(n2C)(1-A)/C Table 1 When analyzing an optical system, we often are first interested in basic properties of the system such as the focal length (or optical power of the system) and the location of the focal planes, etc. In the limit of paraxial optics, any optical system, from a simple lens to a combination of lenses, mirrors and ducts, can be described in terms of six special surfaces, called the cardinal surfaces of the system. In paraxial optics, these surfaces are planes, normal to the optical axis. The point where the plane intersects the optical axis is the cardinal point corresponding to that cardinal plane. The six special planes are: First Focal Plane Second Focal Plane First Principle Plane Second Principle Plane First Nodal Plane Second Nodal Plane Once we know the location of these special planes, relative to the physical location of the lenses in the system, we can describe all of the paraxial imaging properties of the system.
    [Show full text]
  • Optical Performance:: Characterization of a Pupillometric Camera
    RELATED TITLES Documents Science & Tech Tech Digital & Social Media 58 views 0 0 Abb Uploaded by Mabel Ruiz AP-Physical Low Light Manual Twilight Retrato Science Sample Photography for Render 1.4.5 Aberration document explaining the Seidel coefficients Full description Save Embed Share Print S-118.4250 PPOSTGRADUATE SEMINAR ON ILLUMINATION ENGINEERING ,, SSPRING 2008 LLIGHTING UUNIT,, DDEPARTMENT OF EELECTRONICS,, HHELSINKI UUNIVERSITY OF TTECHNOLOGY (TKK) OPTICAL PERFORMANCE:: CHARACTERIZATION OF A PUPILLOMETRIC CAMERA Petteri Teikari,, [email protected] Emmi Rautkylä,, emmi.rautkylä@tkk.fi RELATED TITLES Documents Science & Tech Tech Digital & Social Media 58 views 0 0 Abb Uploaded by Mabel Ruiz AP-Physical Low Light Manual Twilight Retrato Science Sample Photography for Render 1.4.5 Aberration document explaining the Seidel coefficients Full description Save Embed Share Print RELATED TITLES Documents Science & Tech Tech Digital & Social Media 58 views 0 0 Abb Uploaded by Mabel Ruiz AP-Physical Low Light Manual Twilight Retrato Science Sample Photography for Render 1.4.5 Aberration document explaining the Seidel coefficients Full description Save Embed Share Print TABLE OF CONTENTS A A BSTRACT .................................................................................................................................. TT ABLE OF CONTENTS ................................................................................................................2 11 IINTRODUCTION.................................................................................................................3
    [Show full text]
  • Picture Perfect Page 1 of 2
    Imaging Notes - March/April 1999 - Picture Perfect Page 1 of 2 Picture Perfect It will be the ultimate Kodak moment when the IKONOS satellite captures its first 1-meter image. By Frans Jurgens, technology writer and consultant, Rochester, N.Y. Imagine a telescope no bigger or heavier than a small desk, yet powerful enough to tell the difference between a car and a truck from 400 miles in space. The challenge of building such a telescope was part of an even larger project facing system designers and engineers at Rochester, N.Y.-based Eastman Kodak Co. (Kodak). Relying on 35 years of remote sensing expertise and in-house resources, Kodak designed and built identical digital camera systems for use aboard IKONOS 1 and IKONOS 2, Thornton, Colo.-based Space Imaging's eagerly awaited 1-meter remote sensing satellites. Each camera system comprises an optical telescope, panchromatic and multispectral imaging sensor arrays, and processing electronics. But the IKONOS cameras are unique in several ways. The near-perfect optical sharpness of their telescopes has never been achieved in any space camera. And, instead of acquiring multispectral imagery in three bands (red, green, blue) across separate photo detectors, each focal plane features four bands (including the near-infrared band) on a single integrated array, a manufacturing coup for the industry. The focal plane unit (above) Optical Perfection containing the digital Kodak engineering teams worked for two years to create a 10-meter focal length telescope for each IKONOS imaging sensors is located camera by perfecting a three-mirror optical form rarely used in visible-light telescopes.
    [Show full text]
  • Exploring Parabolic Mirrors with TI92 Plus/TI89
    Exploring Parabolic Mirrors with TI92 Plus/TI89 Vlajko L. Kocic Department of Mathematics, Xavier University of Louisiana, 1 Drexel Dr., New Orleans, LA 70125, e-mail: [email protected] Reflecting telescope, flashlights, satellite dish antenna, optical illusions like “levitating penny” and “inverted light bulb”… What do they have in common? The answer is in the title of this paper: parabolic mirror. What is a parabolic mirror? It is a mirror whose reflecting surface is in the shape of a paraboloid (surface whose all cross sections are parabolas). Why parabolic mirror? Well, it has a property that the incident rays parallel to the axis of the parabola (for example, those that are coming from distant objects, like planets, stars, galaxies, or electromagnetic signals from satellites) after being reflected from the mirror, pass through the same point – the focus of a parabola. This paper focuses on the reflection from a parabolic mirror and involves activities designed for students enrolled in at least Calculus I. Part III deals with solving differential equations and is suitable for some Calculus II students (where basic differential equations topics are covered) or for students taking Differential Equations course. Part I is suitable as a classroom activity, while part II is more appropriate as a homework assignment or project. Part III might be used as an introduction to Lagrange and Clairaut type differential equations (if they are covered in the course). TI92 Plus scripts for solving Lagrange and Clairaut types of differential equations are given in the Appendix. In this paper we provide the TI92 Plus script for all activities.
    [Show full text]
  • Physics Chapter 13
    CHAPTER 13 Instruction and Intervention Support Light and Reflection 1 Core Instruction Chapter Resources ■ The Teacher’s Edition wrap has extensive teaching support for every lesson, including Misconception Alerts, Teach from Visuals, Demonstrations, Teaching Tips, Differentiated Instruction, and Problem Solving. ■ Several additional presentation tools are available online for every chapter, including Animated Physics features, Interactive Whiteboard activities, and Visual Concepts. Labs and Demonstrations Section Instruction Go Online for Materials Lists and Solutions Lists. ■ Textbook: Characteristics of Light ■ Demonstrations: Infrared Light • Radio Waves • How Light Travels 13.1 Visual Concepts: Characteristics of a Wave • Electromagnetic ■ Lab: Light and Mirrors Waves • Electromagnetic Spectrum • Brightness and Distance ■ Lab: Brightness of Light (Core Skill) from a Light Source ■ Lab: Brightness of Light (Probeware) Teaching Visuals: Components of an Electromagnetic Wave • The Electromagnetic Spectrum • Predicting Wave Front Position Using Huygens’s Principle PowerPresentations ■ Textbook: Flat Mirrors ■ Demonstrations: Diffuse Reflection • Specular Reflection • 13.2 Visual Concepts: Reflection • Comparing Specular and Flat Mirror Images Diffuse Reflections • Angle of Incidence and Angle of Reflection • Comparing Real and Virtual Images Teaching Visuals: Image Formation by a Flat Mirror PowerPresentations ■ Textbook: Curved Mirrors ■ Demonstrations: Image Formed by a Concave Mirror • Focal Point 13.3 Animated Physics: Curved Mirrors
    [Show full text]
  • Optical Telescopes
    Optical Telescopes Introduction The night sky always attracted people by its charming mystery. Observers had been using naked eyes for their explorations for many centuries. Obviously, they could not achieve a lot due to eyesight limitations. It cannot be estimated, how important the invention of telescopes was for astronomers. It opened an enormous field for visual observations, which had lead to many brilliant discoveries. That happened in 1608, when the German-born Dutch eyeglass maker had guessed to combine several lenses and created the first telescope [PRAS]. This occasion is now almost forgotten, because no inventions were made but a Dutchman. His device was not used for astronomical purposes, and it found its application in military use. The event, which remains in people memories, is the Galilean invention of his first telescope in 1609. The first Galilean optical tube was very simple, it could only magnify objects three times. After several modifications, the scientist achieved higher optical power. This helped him to observe the venusian phases, lunar craters and four jovian satellites. The main tasks of a telescope are the following: • Gathering as much light radiation as possible • Increasing an angular separation between objects • Creating a focused image of an object We have now achieved high technical level, which enables us to create colossal telescopes, reaching distant regions of the Universe and making great discoveries. Telescope components The main parts of which any telescope consists with are the following: • Primary lens (for refracting telescopes), which is the main component of a device. Bigger the lens, more light a telescope can gather and fainter objects can be viewed.
    [Show full text]
  • Lens Design I – Seminar 1
    Y. Sekman, X. Lu, H. Gross Friedrich Schiller University Jena Institute of Applied Physics Albert-Einstein-Str 15 07745 Jena Lens Design I – Seminar 1 Exercise 1-1: Stair-mirror-setup (Homework) Setup a system with a stair mirror pair, which decenters an incoming collimated ray bundle with 10 mm diameter by 40 mm in the -y direction. The wavelength of the beam is = 632.8 nm. After this pair of mirrors, a decentered main objective lens with focal length f = 200 mm made of BK7 is located 25 mm below the optical axis and focusses the beam. a) Setup the system b) Generate layout drawings in 2D and in 3D. c) Calculate the beam cross section on the second mirror, what is the size of the pattern? d) Determine the optimal final sensor plane location. Calculate the spot of the focused beam. Discuss the shape of this pattern. Exercise 1-2: Symmetrical 4f-system Setup a telecentric 4f-imaging system with two identical plano-convex lenses made of BK7 with thickness d = 10 mm and approximate focal lengths f = 100 mm. The wavelength of the system is = 546.07 nm and the numerical aperture in the object space is NA = 0.2. The object has a diameter of 10 mm. a) If the setup is perfectly symmetrical, determine the layout and the spot diagram of the system. b) Optimize the image location. Why is the spot size improved? c) If the starting aperture is decreased, the system becomes more and more close to diffraction limited. What is the value of the NA to get a diffraction limited system on axis? Take in mind here, that a re-focussing might be necessary due to the lowered spherical aberrations, which depends on the aperture.
    [Show full text]