Isaac Newton Group of Telescopes
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The Son of Lamoraal Ulbo De Sitter, a Judge, and Catharine Theodore Wilhelmine Bertling
558 BIOGRAPHIES v.i WiLLEM DE SITTER viT 1872-1934 De Sitter was bom on 6 May 1872 in Sneek (province of Friesland), the son of Lamoraal Ulbo de Sitter, a judge, and Catharine Theodore Wilhelmine Bertling. His father became presiding judge of the court in Arnhem, and that is where De Sitter attended gymna sium. At the University of Groniiigen he first studied mathematics and physics and then switched to astronomy under Jacobus Kapteyn. De Sitter spent two years observing and studying under David Gill at the Cape Obsen'atory, the obseivatory with which Kapteyn was co operating on the Cape Photographic Durchmusterung. De Sitter participated in the program to make precise measurements of the positions of the Galilean moons of Jupiter, using a heliometer. In 1901 he received his doctorate under Kapteyn on a dissertation on Jupiter's satellites: Discussion of Heliometer Observations of Jupiter's Satel lites. De Sitter remained at Groningen as an assistant to Kapteyn in the astronomical laboratory, until 1909, when he was appointed to the chair of astronomy at the University of Leiden. In 1919 he be came director of the Leiden Observatory. He remained in these posts until his death in 1934. De Sitter's work was highly mathematical. With his work on Jupi ter's satellites, De Sitter pursued the new methods of celestial me chanics of Poincare and Tisserand. His earlier heliometer meas urements were later supplemented by photographic measurements made at the Cape, Johannesburg, Pulkowa, Greenwich, and Leiden. De Sitter's final results on this subject were published as 'New Math ematical Theory of Jupiter's Satellites' in 1925. -
Foundations of Newtonian Dynamics: an Axiomatic Approach For
Foundations of Newtonian Dynamics: 1 An Axiomatic Approach for the Thinking Student C. J. Papachristou 2 Department of Physical Sciences, Hellenic Naval Academy, Piraeus 18539, Greece Abstract. Despite its apparent simplicity, Newtonian mechanics contains conceptual subtleties that may cause some confusion to the deep-thinking student. These subtle- ties concern fundamental issues such as, e.g., the number of independent laws needed to formulate the theory, or, the distinction between genuine physical laws and deriva- tive theorems. This article attempts to clarify these issues for the benefit of the stu- dent by revisiting the foundations of Newtonian dynamics and by proposing a rigor- ous axiomatic approach to the subject. This theoretical scheme is built upon two fun- damental postulates, namely, conservation of momentum and superposition property for interactions. Newton’s laws, as well as all familiar theorems of mechanics, are shown to follow from these basic principles. 1. Introduction Teaching introductory mechanics can be a major challenge, especially in a class of students that are not willing to take anything for granted! The problem is that, even some of the most prestigious textbooks on the subject may leave the student with some degree of confusion, which manifests itself in questions like the following: • Is the law of inertia (Newton’s first law) a law of motion (of free bodies) or is it a statement of existence (of inertial reference frames)? • Are the first two of Newton’s laws independent of each other? It appears that -
Astronomer Explores Universe Through Remote-Controlled Telescope 24 May 2016
Astronomer explores universe through remote-controlled telescope 24 May 2016 and bring his students into his research. The telescope is in the Western Europe time zone, which is six hours head of U.S. Central Time. "Because of the time difference, students can see in the afternoon what they'd have to wait until midnight to see here," Keel said. "This opens up new possibilities for classroom experiences in our daytime, as well as making it easier to use the telescope without changing a whole day's schedule." In April and May, Keel took some photos using the reopened telescope, including shots of the globular star cluster M3 in Canes Venatici (the constellation of the Hunting Dogs just south of the Big Dipper) and the planetary nebula M27 (the Dumbbell Nebula) in Vulpecula (the Fox, in the summer Milky Way). Eagle Nebula M16. Taken by Dr. William Keel with the Jacobus Kapteyn Telescope. Access by the astronomers at The University of Alabama to the Jacobus Kapteyn Telescope in the Canary Islands will benefit both research and students at UA. Dr. William Keel, UA professor of astronomy and astrophysics, represents UA on the managing board of a 12-institution consortium called the Southeastern Association for Research in Astronomy. He recently obtained some of the first data with the recently reopened Jacobus Kapteyn Telescope through SARA, which operates the telescope. The 1.0-meter telescope is at an altitude of 2,360 meters at the Observatorio del Roque de los Spiral galaxy M83. Taken by Dr. William Keel with the Muchachos on the Spanish Canary Island of La Jacobus Kapteyn Telescope. -
Planets Asteroids Comets the Jacobus Kapteyn Telescope Meteors
Planets A planet is an astronomical body in orbit The Solar System around the Sun, or another star, which has a mass too small for it to become a star itself (less than about one-twentieth the mass of the Sun) and shines only by reflected light. Planets may be basically rocky objects, such as the The Sun, together with the planets and moons, comets, asteroids, meteoroid inner planets - Mercury, Venus, Earth and streams and interplanetary medium held captive by the Sun’s gravitational Mars - or primarily gaseous, with a small solid attraction. The solar system is presumed to have formed from a rotating disc of core like the outer planets - Jupiter, Saturn, gas and dust created around the Sun as it contracted to form a star, about five Uranus and Neptune. Together with Pluto, billion years ago. The planets and asteroids all travel around the Sun in the these are the major planets of the Solar same direction as the Earth, in orbits close to the plane of the Earth’s orbit and System. the Sun’s equator. The planetary orbits lie within 40 astronomical units (6 thousand million kilometres) of the Sun, though the Sun’s sphere of Asteroids gravitational influence can be considered to be much greater. Comets seen in the inner solar system may originate in the Oort cloud, many thousands of astronomical units away. Comets Comets are icy bodies orbiting in the Solar System, which partially vaporises when it nears the Sun, developing a diffuse envelope of dust and gas and, normally, one or more tails. -
Newton.Indd | Sander Pinkse Boekproductie | 16-11-12 / 14:45 | Pag
omslag Newton.indd | Sander Pinkse Boekproductie | 16-11-12 / 14:45 | Pag. 1 e Dutch Republic proved ‘A new light on several to be extremely receptive to major gures involved in the groundbreaking ideas of Newton Isaac Newton (–). the reception of Newton’s Dutch scholars such as Willem work.’ and the Netherlands Jacob ’s Gravesande and Petrus Prof. Bert Theunissen, Newton the Netherlands and van Musschenbroek played a Utrecht University crucial role in the adaption and How Isaac Newton was Fashioned dissemination of Newton’s work, ‘is book provides an in the Dutch Republic not only in the Netherlands important contribution to but also in the rest of Europe. EDITED BY ERIC JORINK In the course of the eighteenth the study of the European AND AD MAAS century, Newton’s ideas (in Enlightenment with new dierent guises and interpre- insights in the circulation tations) became a veritable hype in Dutch society. In Newton of knowledge.’ and the Netherlands Newton’s Prof. Frans van Lunteren, sudden success is analyzed in Leiden University great depth and put into a new perspective. Ad Maas is curator at the Museum Boerhaave, Leiden, the Netherlands. Eric Jorink is researcher at the Huygens Institute for Netherlands History (Royal Dutch Academy of Arts and Sciences). / www.lup.nl LUP Newton and the Netherlands.indd | Sander Pinkse Boekproductie | 16-11-12 / 16:47 | Pag. 1 Newton and the Netherlands Newton and the Netherlands.indd | Sander Pinkse Boekproductie | 16-11-12 / 16:47 | Pag. 2 Newton and the Netherlands.indd | Sander Pinkse Boekproductie | 16-11-12 / 16:47 | Pag. -
The Newton-Leibniz Controversy Over the Invention of the Calculus
The Newton-Leibniz controversy over the invention of the calculus S.Subramanya Sastry 1 Introduction Perhaps one the most infamous controversies in the history of science is the one between Newton and Leibniz over the invention of the infinitesimal calculus. During the 17th century, debates between philosophers over priority issues were dime-a-dozen. Inspite of the fact that priority disputes between scientists were ¡ common, many contemporaries of Newton and Leibniz found the quarrel between these two shocking. Probably, what set this particular case apart from the rest was the stature of the men involved, the significance of the work that was in contention, the length of time through which the controversy extended, and the sheer intensity of the dispute. Newton and Leibniz were at war in the later parts of their lives over a number of issues. Though the dispute was sparked off by the issue of priority over the invention of the calculus, the matter was made worse by the fact that they did not see eye to eye on the matter of the natural philosophy of the world. Newton’s action-at-a-distance theory of gravitation was viewed as a reversion to the times of occultism by Leibniz and many other mechanical philosophers of this era. This intermingling of philosophical issues with the priority issues over the invention of the calculus worsened the nature of the dispute. One of the reasons why the dispute assumed such alarming proportions and why both Newton and Leibniz were anxious to be considered the inventors of the calculus was because of the prevailing 17th century conventions about priority and attitude towards plagiarism. -
Guide for the Use of the International System of Units (SI)
Guide for the Use of the International System of Units (SI) m kg s cd SI mol K A NIST Special Publication 811 2008 Edition Ambler Thompson and Barry N. Taylor NIST Special Publication 811 2008 Edition Guide for the Use of the International System of Units (SI) Ambler Thompson Technology Services and Barry N. Taylor Physics Laboratory National Institute of Standards and Technology Gaithersburg, MD 20899 (Supersedes NIST Special Publication 811, 1995 Edition, April 1995) March 2008 U.S. Department of Commerce Carlos M. Gutierrez, Secretary National Institute of Standards and Technology James M. Turner, Acting Director National Institute of Standards and Technology Special Publication 811, 2008 Edition (Supersedes NIST Special Publication 811, April 1995 Edition) Natl. Inst. Stand. Technol. Spec. Publ. 811, 2008 Ed., 85 pages (March 2008; 2nd printing November 2008) CODEN: NSPUE3 Note on 2nd printing: This 2nd printing dated November 2008 of NIST SP811 corrects a number of minor typographical errors present in the 1st printing dated March 2008. Guide for the Use of the International System of Units (SI) Preface The International System of Units, universally abbreviated SI (from the French Le Système International d’Unités), is the modern metric system of measurement. Long the dominant measurement system used in science, the SI is becoming the dominant measurement system used in international commerce. The Omnibus Trade and Competitiveness Act of August 1988 [Public Law (PL) 100-418] changed the name of the National Bureau of Standards (NBS) to the National Institute of Standards and Technology (NIST) and gave to NIST the added task of helping U.S. -
NEWTON's FIRST LAW of MOTION the Law of INERTIA
NEWTON’S FIRST LAW OF MOTION The law of INERTIA INERTIA - describes how much an object tries to resist a change in motion (resist a force) inertia increases with mass INERTIA EXAMPLES Ex- takes more force to stop a bowling ball than a basket ball going the same speed (bowling ball tries more to keep going at a constant speed- resists stopping) Ex- it takes more force to lift a full backpack than an empty one (full backpack tries to stay still more- resists moving ; it has more inertia) What the law of inertia says…. AKA Newton’s First Law of Motion An object at rest, stays at rest Because the net force is zero! Forces are balanced (equal & opposite) …an object in motion, stays in motion Motion means going at a constant speed & in a straight line The net force is zero on this object too! NO ACCELERATION! …unless acted upon by a net force. Only when this happens will you get acceleration! (speed or direction changes) Forces are unbalanced now- not all equal and opposite there is a net force> 0N! You have overcome the object’s inertia! How does a traveling object move once all the forces on it are balanced? at a constant speed in a straight line Why don’t things just move at a constant speed in a straight line forever then on Earth? FRICTION! Opposes the motion & slows things down or GRAVITY if motion is in up/down direction These make the forces unbalanced on the object & cause acceleration We can’t get away from those forces on Earth! (we can encounter some situations where they are negligible though!) HOW can you make a Bowling -
Newton's First Law of Motion
Mechanics 2.1. Newton’s first law of motion mc-web-mech2-1-2009 Sir Isaac Newton aimed to describe and predict the movement of every object in the Universe using his three laws of motion. Like many other ‘laws’ they give the right answers for the majority of the time. For example, the paths of planets, moons and satellites are all calculated using Newton’s laws. Newton’s first law of motion Newton’s first law of motion states that a body will stay at rest or move with constant velocity unless a resultant external force acts on it. Note: Moving in a straight line at a constant speed, in other words, moving at a constant velocity is commonly referred to as uniform motion. There are two consequences of this law: 1. If a body has an acceleration, then there must be a resultant force acting on it. 2. If a body has no acceleration, then the forces acting on it must be in equilibrium (have zero resultant force). At first glance this law would appear contrary to everyday experience: give an object a push to set it in motion - then, it will slow down and come to rest - it does not ‘continue in a state of uniform motion’. This is due to unseen resistive forces of friction and air resistance opposing the motion. (Figure 1). Figure 1: Resistive forces acting together to oppose motion Bodies resist changes to their motion. In mechanics, inertia is the resistance of a body to a change in its velocity. It is the property discussed in Newton’s first law, sometimes known as the principle of inertia. -
Nova Report 2006-2007
NOVA REPORTNOVA 2006 - 2007 NOVA REPORT 2006-2007 Illustration on the front cover The cover image shows a composite image of the supernova remnant Cassiopeia A (Cas A). This object is the brightest radio source in the sky, and has been created by a supernova explosion about 330 year ago. The star itself had a mass of around 20 times the mass of the sun, but by the time it exploded it must have lost most of the outer layers. The red and green colors in the image are obtained from a million second observation of Cas A with the Chandra X-ray Observatory. The blue image is obtained with the Very Large Array at a wavelength of 21.7 cm. The emission is caused by very high energy electrons swirling around in a magnetic field. The red image is based on the ratio of line emission of Si XIII over Mg XI, which brings out the bi-polar, jet-like, structure. The green image is the Si XIII line emission itself, showing that most X-ray emission comes from a shell of stellar debris. Faintly visible in green in the center is a point-like source, which is presumably the neutron star, created just prior to the supernova explosion. Image credits: Creation/compilation: Jacco Vink. The data were obtained from: NASA Chandra X-ray observatory and Very Large Array (downloaded from Astronomy Digital Image Library http://adil.ncsa.uiuc. edu). Related scientific publications: Hwang, Vink, et al., 2004, Astrophys. J. 615, L117; Helder and Vink, 2008, Astrophys. J. in press. -
Large Telescopes and Why We Need Them Transcript
Large telescopes and why we need them Transcript Date: Wednesday, 9 May 2012 - 1:00PM Location: Museum of London 9 May 2012 Large Telescopes And Why we Need Them Professor Carolin Crawford Astronomy is a comparatively passive science, in that we can’t engage in laboratory experiments to investigate how the Universe works. To study any cosmic object outside of our Solar System, we can only work with the light it emits that happens to fall on Earth. How much we can interpret and understand about the Universe around us depends on how well we can collect and analyse that light. This talk is about the first part of that problem: how we improve the collection of light. The key problem for astronomers is that all stars, nebulae and galaxies are so very far away that they appear both very small, and very faint - some so much so that they can’t be seen without the help of a telescope. Its role is simply to collect more light than the unaided eye can, making astronomical sources appear both bigger and brighter, or even just to make most of them visible in the first place. A new generation of electronic detectors have made observations with the eye redundant. We now have cameras to record the images directly, or once it has been split into its constituent wavelengths by spectrographs. Even though there are a whole host of ingenious and complex instruments that enable us to record and analyse the light, they are still only able to work with the light they receive in the first place. -
The GLENDAMA Database
Technical Report & User's Guide The GLENDAMA Database Luis J. Goicoechea, Vyacheslav N. Shalyapin? and Rodrigo Gil-Merino Universidad de Cantabria, Santander, Spain ABSTRACT This is the first version (v1) of the Gravitational LENses and DArk MAtter (GLENDAMA) database accessible at http://grupos.unican.es/glendama/database The new database contains more than 6000 ready-to-use (processed) astronomical frames corresponding to 15 objects that fall into three classes: (1) lensed QSO (8 objects), (2) binary QSO (3 objects), and (3) accretion-dominated radio-loud QSO (4 objects). Data are also divided into two categories: freely available and available upon request. The second category includes observations related to our yet unpublished analyses. Although this v1 of the GLENDAMA archive incorporates an X-ray monitoring campaign for a lensed QSO in 2010, the rest of frames (imaging, polarimetry and spectroscopy) were taken with NUV, visible and NIR facilities over the period 1999−2014. The monitorings and follow-up observations of lensed QSOs are key tools for discussing the accretion flow in distant QSOs, the redshift and structure of intervening (lensing) galaxies, and the physical properties of the Universe as a whole. Subject headings: astronomical databases | gravitational lensing: strong and micro | quasars: general | quasars: supermassive black holes | quasars: ac- cretion | galaxies: general | galaxies: distances and redshifts | galaxies: halos arXiv:1505.04317v2 [astro-ph.IM] 19 May 2015 | cosmological parameters ?permanent address: Institute for Radiophysics and Electronics, Kharkov, Ukraine { 2 { 1. Target objects and facilities At present, the Gravitational LENses and DArk MAtter (GLENDAMA) project at the Universidad de Cantabria (UC) is conducting a programme of observation of eight lensed QSOs with facilities at the European Northern Observatory (ENO).