DOCSLIB.ORG

The Hubble Space Telescope

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
The Hubble Space Telescope Lecture 25-1 Aberrations Chromatic aberration Cameras, … correct nblue > nred Spherical aberration Parabolic mirrror Large telescopes, … Lecture 25-2 The Human Eye (1) ° Refraction at the cornea and lens surfaces produces an inverted real image on the retina of the eye (the brain interprets it upright !) ° For an object to be seen clearly, the image must be formed at the location of the retina ° The shape of the lens controls the distance of the image ≈ 2.5 cm Lecture 25 - 3 The Human Eye (2) • The lens is held in place by ligamen that connect it to the ciliary muscle that allows the lens to change shape and thus change the focus of the lens • The index of refraction of the two fluids in the eye are close to that of water with a value of 1.34; the index of refraction of the material making up the lens is 1.40 • Thus most of the refraction occurs at the air/cornea boundary. ≈ 2.5 cm Lecture 25-4 The Human Eye (3) ≈ 2.5 cm 111 += dd0 i f f depends on d0 d0 ↓ => f↓ to keep di at ≈ 2.5 cm Lecture 25-6 READING QUIZ 1 Which of the following statements is incorrect ? The statements describe the optical characteristics of the human eye. A| A near sighted eye focuses in front of the retina when observing an object located at infinity. B| A far sighted eye focuses behind the retina when observing an object located at infinity. C| A converging lens is used to correct the vision of a near sighted eye. D| Astigmatism is a condition where the eye does not have cylindrical symmetry about the central optical axis. E| A cataract operation of the second lens inside the eye removes the clouded lens and replaces it with a plastic implant. Lecture 25-5 Example: Corrective Lenses (1) Question: A hyperopic (far-sighted) person whose uncorrected near point is 75 cm wishes to read a newspaper at a distance of 25 cm. What is the power of the corrective lens needed for this person? Answer: • The corrective lens must produce a virtual, upright image of the newspaper at the near point of the person’s vision as shown below • The object and image are on the same side so the image distance is negative Lecture 25-6 Example: Corrective Lenses (2) • Thus the object distance is 25 cm and image distance is -75 cm 111 111 += +==+2.66 D 0.25 m- 0.75 m f dd0 i f • The required lens is a converging lens with a power of +2.66 diopters or +2.66 D (focal length of +0.376 m = 1/ 2.66 D) Lecture 25-21 Compound Microscope A microscope consists of two converging lenses: an objective (the front lens) and an eyepiece. An object is placed near the first focal point of the yL' objective. The separation of the lenses is adjusted so mo that the image produced by the objective is formed yfo just inside the first focal point of the eyepiece. The lateral magnification of the objective is xnp The eyepiece angular magnification (eye near point = xnp ) M e f e The overall magnifying power is defined as L xnp MmMoe foef Lecture 25-14 The Telescope • Like the microscope, telescopes come in many forms • First we will discuss (1) the refracting telescope and then (2) reflecting telescopes • The refracting telescope consists of two lenses – The objective lens and the eyepiece • In our example we represent the telescope using two thin lenses • However, an actual refracting telescope will use more sophisticated lenses Lecture 25-22 Astronomical Telescopes Refractor Telescope Same combination (except image at ∞) as compound microscope: Objective creates a real image which allows the eyepiece to magnify. The angular magnification M of the telescope is defined as θe /θo yy'' oe, fo fe f M eo o fe Lecture 25-15 Geometry of the Telescope • Because the object to be viewed is at a large distance, the incoming light rays can be thought of as being parallel (the object is at infinity) • The objective lens forms a real image of the distance object at distance fo • The eyepiece is placed so that the image formed by the objective is at distance fe from the eyepiece • The eyepiece forms a virtual, magnified image of the image formed by the objective • The image is at infinity, again producing parallel rays Lecture 25-16 Magnification of a Telescope • The magnification of the telescope is defined as the angle observed in the eyepiece, qe, divided by the angle subtended by the object being viewed, qo qeof mq =- =- qoef • Because the telescope deals with objects at very large distances, we cannot calculate the magnification of the telescope using the lens law • For example, one might try to express the magnification of the objective lens using the lens equation dd m =-ii =- =0 d Ñ o • We can still get the angular magnification, but we need to use angles rather than distances Lecture 25-17 Calculation of the Magnification of a Telescope (1) • Let’s calculate the angular magnification of a refracting telescope • The angle qo is the angle subtended by a distant object d qqooö=tan fo Lecture 25-18 Calculation of the Magnification of a Telescope (2) • The angle qe is the apparent angle seen in the eyepiece d qqö=tan eef e • The magnification is qeeodf/ f fo == Ω=- mq (inverted) qooedf/ f fe Lecture 25-19 Example: Refracting Telescope • The world’s largest refracting telescope was completed in 1897 and installed in Williams Bay, Wisconsin. It had an objective lens of diameter 40 inches (1.0 m) with a focal length of 62 feet (19 m). Question: What should the focal length of the eyepiece be to give a magnification of 250? Answer: fmo ==19 m 250 The 40-inch fo m = refracting telescope fe at Yerkes f 19 m Observatory f ==o =0.076 m = 7.6 cm e m 250 Lecture 25-20 Problems with Refracting Telescopes • The objective lens of a refracting telescope is large and heavy – The 40-inch refractor at Yerkes weighed 500 pounds • Supporting a large glass lens is difficult – Must be supported by its edges • Constructing large glass lenses is difficult • Glass lenses are thick and absorbe light • A glass lens has chromatic aberration – Different focal lengths for different colors • Solution: Replace the objective lens with a mirror Lecture 25-21 The Reflecting Telescope • Most large astronomical telescopes are reflecting telescopes with the objective lens being replaced with a concave mirror • Large mirrors are easier to fabricate and position than large lenses • The eyepiece is still a lens • Various types of reflecting telescopes have been developed • We will discuss three examples of the geometries of reflecting telescope – Reflector – Newtonian – Cassegrain Lecture 25-22 Basic Reflecting Telescope • Basic reflector • Replace the objective lens with a parabolic mirror • This design is impractical because the observer must be in the line of the incident light Lecture 25-23 Newtonian Reflecting Telescope • In 1670, Newton presented his design for a reflecting telescope to the Royal Society – The idea for a reflecting telescope came from James Gregory • Newton solved the observer problem by placing a small mirror that reflect the light out to an eyepiece • This mirror is small compared with the objective mirror and causes only a small loss of light from the image Lecture 25-24 Cassegrain Geometry for Reflecting Telescope • A further improvement on the geometry of the reflecting telescope is the Cassegrain geometry (named for the French sculptor Sieur Guillaume Cassegrain) first proposed in 1672 • Here a small mirror is used to reflect the image through a hole in the center of the objective mirror • This design and many improvements to this basic idea are the basis of modern astronomical telescopes Lecture 25-25 Reflector Telescope ‹ No chromatic aberration ‹ Large mirrors can be made (large amount of light gathered) ‹ Easier to support ‹ View center blocked off fo ‹ Maginfication m q =- fe (same as a refracting telescope) Whipple Telescope Lecture 25-26 The Hubble Space Telescope (1) • The Hubble Space Telescope (HST) was deployed April 25, 1990 from the Space Shuttle mission STS-31 • The HST orbits the Earth 590 km above the surface of the Earth, far above the atmosphere that disturbs the images gathered by ground-based telescopes • The HST is a Ritchey-Chrétien reflecting telescope arranged in a Cassegrain geometry Lecture 25-27 The Hubble Space Telescope (2) • The HST is a Ritchey-Chrétien reflecting telescope arranged in a Cassegrain geometry • This type of telescope uses a concave hyperbolic objective mirror rather than a spherical mirror and a convex hyperbolic secondary mirror • This arrangement gives the HST a wide field of view and eliminates spherical aberration • The objective mirror is 2.40 m in diameter and has an effective focal length of 57.6 m Lecture 25-28 Hubble Corrected • The original HST objective mirror was produced with a flaw caused by a defective testing instrument (deployed on April 25, 1990) • In December 1993, Space Shuttle Service Mission 1 (STS-61) deployed the COSTAR package that corrected the flaw in the objective mirror and allowed the HST to produce spectacular pictures • The two images of the galaxy M100 shown on the left and on the right demonstrate the image quality of the HST before and after the installation of COSTAR .
Load more

Recommended publications
  • The Reflecting Telescope
    The Reflecting Telescope Lens telescopes exist since 1609 when the Dutch maker of The optical properties data of the AstroMedia* reflecting tel- spectacles, Jan Lippershey, sold the first telescopes, then as escope roughly correspond to those of the first instrument a curiosity, to his astonished customers. It was made out of a built by Newton. The mirror has a focal length f=450mm (”f” concave and a convex lens, produced an upright standing from the Latin ”focus” is the abbreviation of focal length). It’s image and had a 3 1/2 times magnification. Galileo Galilei curve is spherical, i.e. is has the same round surface as a (1564-1642) improved on this invention and was the first to globe. make astronomical observations with it. Today almost A spherical concave mirror has one disadvantage: the all lens telescopes are built according to the prin- light rays reflected from the edge meet a little nearer ciples of Johannes Kepler (1571-1630). His tel- to the mirror than those reflected from the centre, escope, based on two convex lenses, produced causing a slight focus distortion. However, since an upside down but much bigger and better this distortion is is not grave and such mirrors focused image which of course for observing are relatively easy to grind, they are neverthe- the heavens are the most important factors. less used in smaller telescopes. In telescopes Building larger telescopes however with larger openings and stronger mag- brings two problems with it: Firstly, nification mirrors with parabolic curves in a lens the light rays are broken, are used.
    [Show full text]
  • Telescopes and Binoculars
    Continuing Education Course Approved by the American Board of Opticianry Telescopes and Binoculars National Academy of Opticianry 8401 Corporate Drive #605 Landover, MD 20785 800-229-4828 phone 301-577-3880 fax www.nao.org Copyright© 2015 by the National Academy of Opticianry. All rights reserved. No part of this text may be reproduced without permission in writing from the publisher. 2 National Academy of Opticianry PREFACE: This continuing education course was prepared under the auspices of the National Academy of Opticianry and is designed to be convenient, cost effective and practical for the Optician. The skills and knowledge required to practice the profession of Opticianry will continue to change in the future as advances in technology are applied to the eye care specialty. Higher rates of obsolescence will result in an increased tempo of change as well as knowledge to meet these changes. The National Academy of Opticianry recognizes the need to provide a Continuing Education Program for all Opticians. This course has been developed as a part of the overall program to enable Opticians to develop and improve their technical knowledge and skills in their chosen profession. The National Academy of Opticianry INSTRUCTIONS: Read and study the material. After you feel that you understand the material thoroughly take the test following the instructions given at the beginning of the test. Upon completion of the test, mail the answer sheet to the National Academy of Opticianry, 8401 Corporate Drive, Suite 605, Landover, Maryland 20785 or fax it to 301-577-3880. Be sure you complete the evaluation form on the answer sheet.
    [Show full text]
  • Find Your Telescope. Your Find Find Yourself
    FIND YOUR TELESCOPE. FIND YOURSELF. FIND ® 2008 PRODUCT CATALOG WWW.MEADE.COM TABLE OF CONTENTS TELESCOPE SECTIONS ETX ® Series 2 LightBridge ™ (Truss-Tube Dobsonians) 20 LXD75 ™ Series 30 LX90-ACF ™ Series 50 LX200-ACF ™ Series 62 LX400-ACF ™ Series 78 Max Mount™ 88 Series 5000 ™ ED APO Refractors 100 A and DS-2000 Series 108 EXHIBITS 1 - AutoStar® 13 2 - AutoAlign ™ with SmartFinder™ 15 3 - Optical Systems 45 FIND YOUR TELESCOPE. 4 - Aperture 57 5 - UHTC™ 68 FIND YOURSEL F. 6 - Slew Speed 69 7 - AutoStar® II 86 8 - Oversized Primary Mirrors 87 9 - Advanced Pointing and Tracking 92 10 - Electronic Focus and Collimation 93 ACCESSORIES Imagers (LPI,™ DSI, DSI II) 116 Series 5000 ™ Eyepieces 130 Series 4000 ™ Eyepieces 132 Series 4000 ™ Filters 134 Accessory Kits 136 Imaging Accessories 138 Miscellaneous Accessories 140 Meade Optical Advantage 128 Meade 4M Community 124 Astrophotography Index/Information 145 ©2007 MEADE INSTRUMENTS CORPORATION .01 RECRUIT .02 ENTHUSIAST .03 HOT ShOT .04 FANatIC Starting out right Going big on a budget Budding astrophotographer Going deeper .05 MASTER .06 GURU .07 SPECIALIST .08 ECONOMIST Expert astronomer Dedicated astronomer Wide field views & images On a budget F IND Y OURSEL F F IND YOUR TELESCOPE ® ™ ™ .01 ETX .02 LIGHTBRIDGE™ .03 LXD75 .04 LX90-ACF PG. 2-19 PG. 20-29 PG.30-43 PG. 50-61 ™ ™ ™ .05 LX200-ACF .06 LX400-ACF .07 SERIES 5000™ ED APO .08 A/DS-2000 SERIES PG. 78-99 PG. 100-105 PG. 108-115 PG. 62-76 F IND Y OURSEL F Astronomy is for everyone. That’s not to say everyone will become a serious comet hunter or astrophotographer.
    [Show full text]
  • Solar System Solar System
    Delta Science Reader SolarSolar SystemSystem Delta Science Readers are nonfiction student books that provide science background and support the experiences of hands-on activities. Every Delta Science Reader has three main sections: Think About . , People in Science, and Did You Know? Be sure to preview the reader Overview Chart on page 4, the reader itself, and the teaching suggestions on the following pages. This information will help you determine how to plan your schedule for reader selections and activity sessions. Reading for information is a key literacy skill. Use the following ideas as appropriate for your teaching style and the needs of your students. The After Reading section includes an assessment and writing links. OVERVIEW Students will: discover facts about the Solar System In the Delta Science Reader Solar System, students take a tour of the Sun and the explore the planets and other objects in the planets. Other space objects such as dwarf Solar System planets, comets, asteroids, and meteoroids discuss the function of a table of contents, are explored. Students read about the headings, and a glossary rotation and revolution of the planets and interpret photographs and graphics to the causes of night and day, seasonal answer questions changes, and the phases of the Moon. The book describes the work of a planetary complete a KWL chart geologist. In addition, students discover organize information in a variety of ways how telescopes work. delta science modules Solar System 119 © Delta Education LLC. All rights reserved.
    [Show full text]
  • First Telescope Purchase
    Recommendation Report: First Telescope Purchase Purchasing a telescope can be very confusing for a person who is new to astronomy. This reports provides a comparison of entry-level telescopes for the amateur astronomer and recommends a specific type of telescope for the typical beginning astronomer. This report will focus on different types of telescopes, and not on specific brands. In addition to comparing several different types of telescopes, this report also compares different telescope mounts. Note: This report was prepared for the Austin Telescope Society, which is a non-profit organization dedicated to the enjoyment of astronomy and the education of the public about astronomy. Many people interested in astronomy waste money on a telescope of poor quality. A telescope in a department store may advertise that it can magnify several hundred times; however, the user is often disappointed when the image is dim, shaky, and hazy. To help avoid this confusion, it is important that the beginning astronomer understand the advantages and disadvantages of various types of telescopes. It is vitally important that the telescope have high quality optics and a sturdy mount. No extra gadgets and frills will help a telescope that has poor optics. Definition of Terms Before the actual comparison report, it is vital that several common terms are defined. The following terms must be understood before proceeding with this comparison: • Alt-azimuth mount. A type of telescope mount that moves in two directions: altitude and azimuth. This is the type of motion best illustrated by a cannon. It can be moved up or down, or rotated left or right.
    [Show full text]
  • A Guide to Smartphone Astrophotography National Aeronautics and Space Administration
    National Aeronautics and Space Administration A Guide to Smartphone Astrophotography National Aeronautics and Space Administration A Guide to Smartphone Astrophotography A Guide to Smartphone Astrophotography Dr. Sten Odenwald NASA Space Science Education Consortium Goddard Space Flight Center Greenbelt, Maryland Cover designs and editing by Abbey Interrante Cover illustrations Front: Aurora (Elizabeth Macdonald), moon (Spencer Collins), star trails (Donald Noor), Orion nebula (Christian Harris), solar eclipse (Christopher Jones), Milky Way (Shun-Chia Yang), satellite streaks (Stanislav Kaniansky),sunspot (Michael Seeboerger-Weichselbaum),sun dogs (Billy Heather). Back: Milky Way (Gabriel Clark) Two front cover designs are provided with this book. To conserve toner, begin document printing with the second cover. This product is supported by NASA under cooperative agreement number NNH15ZDA004C. [1] Table of Contents Introduction.................................................................................................................................................... 5 How to use this book ..................................................................................................................................... 9 1.0 Light Pollution ....................................................................................................................................... 12 2.0 Cameras ................................................................................................................................................
    [Show full text]
  • Astronomy Alphabet
    Astronomy Alphabet Educational video for children Teacher https://vimeo.com/77309599 & Learner Guide This guide gives background information about the astronomy topics mentioned in the video, provides questions and answers children may be curious about, and suggests topics for discussion. Alhazen A Alhazen, called the Father of Optics, performed NASA/Goddard/Lunar Reconnaissance Orbiter, Apollo 17 experiments over a thousand years ago Can you find Alhazen crater when you look at the Moon? to learn about how light travels and Why does the Moon look bigger near the behaves. He also studied astronomy, horizon? separated light into colors, and sought to Believe it or not, scientists still don’t know for sure why explain why the Moon looks bigger near we perceive the Moon to be larger when it lies near to the the horizon. horizon. Though photos of the Moon at different points in the sky show it to be the same size, we humans think we I’ve never heard of Abu Ali al-Hasan ibn al- see something quite different. Try this experiment yourself Hasan ibn al-Hatham (Alhazen). sometime! One possibility is that objects we see next to the Tell me more about him. Moon when it’s near to them give us the illusion that it’s We don’t know that much about Alhazen be- bigger, because of a sense of scale and reference. cause he lived so long ago, but we do know that he was born in Persia in 965. He wrote hundreds How many craters does the Moon have, and what of books on math and science and pioneered the are their names? scientific method of experimentation.
    [Show full text]
  • Women of Astronomy
    WOMEN OF ASTRONOMY AND A TIMELINE OF EVENTS… Time line of Astronomy • 2350 B.C. – EnHeduanna (ornament of heaven) – • Chief Astronomer Priestess of the Moon Goddess of the City in Babylonia. • Movement of the Stars were used to create Calendars • 2000 B.C. - According to legend, two Chinese astronomers are executed for not predicting an eclipse. • 129 B.C. - Hipparchos completes the first catalog of the stars, and invented stellar magnitude (still in use today!) • 150 A.D. - Claudius Ptolemy publishes his theory of the Earth- centered universe. • 350 A.D – Hypatia of Alexandria – First woman Astronomer • Hypatia of Alexandria Born approximately in 350 A.D. • Accomplished mathematician, inventor, & philosopher of Plato and Aristotle • Designed astronomical instruments, such as the astrolabe and the planesphere. The first star chart to have the name An early astrolabe was invented in "planisphere" was made in 1624 by 150 BC and is often attributed to Jacob Bartsch. Son of Johannes Hipparchus Kepler, who solved planetary motion. Time line of Astronomy • 970 - al-Sufi, a Persian Astronomer prepares catalog of over 1,000 stars. • 1420 Ulugh-Beg, prince of Turkestan, builds a great observatory and prepares tables of planet and stars • 1543 While on his deathbed, Copernicus publishes his theory that planets orbit around the sun. • 1609 Galileo discovers craters on Earth’s moon, the moons of Jupiter, the turning of the sun, and the presence of innumerable stars in the Milky Way with a telescope that he built. • 1666 Isaac Newton begins his work on the theory of universal gravitation. • 1671 Newton demonstrates his invention, the reflecting telescope.
    [Show full text]
  • Ritchey Chretien Telescope Hyperbola Hyperbola
    Last Lecture: Astronomical Optics ! 2. Fundamentals of Telescopes designs ! 2.1. Telescope types: refracting, reflecting ! OUTLINE: ! Shaping light into an image: first principles Telescopes for different wavelengths Telescope elements: lenses and mirrors ! Telescope types – refracting (lenses) – reflecting (mirrors) ! ! Keeping the image sharp on large telescopes: challenges !1 Astronomical Optics ! 2. Fundamentals of Telescope designs ! 2.2. Wide Field of View designs and aberration correction ! Outline, Key concepts: ! ! Importance of the location of focus and instruments ! Main reflecting telescope designs: – Newtonian (parabolic mirror) – Gregorian – Cassegrain – RC ! ! Wide field telescope designs, correctors ! Location of focus & instrument(s) is key to telescope design ! Telescopes are designed with instrument(s) in mind. ! Sometime, a specialized telescope + instrument are designed together. ! Subaru telescope (8.2m): location of the 4 telescope focii ! Location of focus & instrument ! A wide field of view requires a large beam, difficult to squeeze through relay optics (see Lagrange invariant) → prime focus is often preferred for wide field instruments, or very large central obstruction (OK if wide field is single purpose of telescope) Examples (next few slides): – PanSTARRS – LBT LBC – LSST ! Heavy large/heavy instruments, or instruments requiring outstanding stability cannot easily be mounted on the telescope tube → Nasmyth focus, or coude focus, preferred Examples: – Subaru HDS – HARPS (requires outstanding spectroscopic stability) ! IR instruments require minimal number of reflections to limit thermal emission from optics → Cassegrain focus is preferred Pan-STARRS : 1.8m diameter telescope, 3 deg. diameter FOV Large Binocular Telescope's wide field cameras 0.4 deg. on a side. If the cameras are the same for Pan-STARRS and LBC, which can form a deeper image? ! ! LBC requires (3/0.4)^2 pointings to survey the field Pan-STARRS gets in a single pointing.
    [Show full text]
  • The Cassegrain Antenna
    The Cassegrain Antenna Principle of a Cassegrain telescope: a convex secondary reflector is located at a concave primary reflector. Figure 1: Principle of a Cassegrain telescope Sieur Guillaume Cassegrain was a French sculptor who invented a form of reflecting telescope. A Cassegrain telescope consists of primary and secondary reflecting mirrors. In a traditional reflecting telescope, light is reflected from the primary mirror up to the eye-piece and out the side the telescope body. In a Cassegrain telescope, there is a hole in the primary mirror. Light enters through the aperture to the primary mirror and is reflected back up to the secondary mirror. The viewer then peers through the hole in the primary reflecting mirror to see the image. A Cassegray antenna used in a fire-control radar. Figure 2: A Cassegray antenna used in a fire-control radar. In telecommunication and radar use, a Cassegrain antenna is an antenna in which the feed radiator is mounted at or near the surface of a concave main reflector and is aimed at a convex subreflector. Both reflectors have a common focal point. Energy from the feed unit (a feed horn mostly) illuminates the secondary reflector, which reflects it back to the main reflector, which then forms the desired forward beam. Advantages Disadvantage: The subreflectors of a Cassegrain type antenna are fixed by bars. These bars The feed radiator is more easily and the secondary reflector constitute supported and the antenna is an obstruction for the rays coming geometrically compact from the primary reflector in the most effective direction. It provides minimum losses as the receiver can be mounted directly near the horn.
    [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]
  • Planets of Our Solar System - Iwan P
    ASTRONOMY AND ASTROPHYSICS - Planets Of Our Solar System - Iwan P. Williams PLANETS OF OUR SOLAR SYSTEM Iwan P. Williams Astronomy Unit, Queen Mary University of London, London UK Keywords: Solar System, Small Bodies, Planets, Dwarf Planets, Satellites, Trans- Neptunian Objects, Asteroids, Plutoids Contents 1. Introduction 2. The Copernican Revolution 3. New telescopes - New discoveries 3.1. The Titius-Bode Law 3.2. The Discovery of Uranus 3.3. Four New Planets 3.4. The Discovery of Neptune 3.5. The Asteroid Belt is discovered 3.6. The Discovery of Pluto 3.7. The True Size of Pluto 4. Trans Neptunian Objects 4.1. The Edgeworth-Kuiper Belt is discovered 5. Planets and Dwarf PLanets 6. The larger members of the Solar System 6.1. Mercury 6.2. Venus 6.3. Earth 6.4. The Moon 6.5. Mars 6.6. Ceres 6.7. Jupiter 6.8. Io 6.9. Europa 6.10. Ganymede 6.11. CallistoUNESCO – EOLSS 6.12. Saturn 6.13. Titan 6.14. Uranus 6.15. Neptune SAMPLE CHAPTERS 6.16. Triton 6.17. Pluto 6.18. Haumea 6.19. Makemake 6.20. Eris 6.21. Other Large Bodies 7. Extra-solar Planets 8. Conclusions Glossary ©Encyclopedia of Life Support Systems (EOLSS) ASTRONOMY AND ASTROPHYSICS - Planets Of Our Solar System - Iwan P. Williams Bibliography Biographical Sketch Summary When humans noticed that most stars appeared to stay in fixed pattern in the sky, they realized that a few moved against this background. They called these wandering stars, or planets. Over the centuries, our knowledge of these has vastly increased and, in the process, our understanding of the system as a whole has changed.
    [Show full text]