Views, Comments & Opinions

Total Page:16

File Type:pdf, Size:1020Kb

Views, Comments & Opinions views, comments & opinions Destination Earth via the moon by Hans van de Groenendaal ZS6AKV, corresponding editor, EngineerIT Radio amateurs are known for their ingenuity and experimental spirit, which often takes them into territories that some believe are reserved for scientists living their lives in laboratories in search of new frontiers. Sometimes I wonder if earth moon earth communication (EME) does not belong to that category. In radio astronomy the desired signal consists of to enhance the weak signal quest. This again noise power as well! Often, but not always, path puts to rest the prophecy from the doom loss varies over time. In space, path loss can be merchants that computers will be the death of very stable and constant over the propagation amateur radio. distances. Radio amateurs speak of so-called Joe Taylor K1JT wrote the WSJT application for “conditions”. It is the interaction of these the purpose of working meteor scatter and “conditions” with the properties of the equipment making weak signal contacts using a mode that form the weak signal domain. For a small but called FSK441. Later the weak signal modes JT44 important segment of the amateur radio world, and JT65 were introduced. These modes are this weak signal domain presents an exciting for extending the range of amateur radio VHF field of application, study, experimentation and stations in weak signal communication. observation. The name WSJT was picked by Joe to mean In the earlier days EME success was very much (Weak Signal JT). Joe’s radio call is K1JT. The dependant on huge antenna arrays and high program provides a method of saving wave power transmitters with sensitive receivers and files and saving the decoded text to a text file low noise preamplifiers fitted at the antenna. if one wishes to use these features. Distances To overcome noise and feed line losses many Hans van de Groenendaal between stations (grids) and antenna direction amateurs fit receive converters at the masthead, pointing are provided on the screen. One of its converting signals to much lower frequencies. operating modes is particularly well optimised for The output of the converter is then fed by EME communication is also known as moon amateur EME communications. WSJT is open ordinary coax cable to the receiver. bounce. It uses the moon as a passive reflector source software and is licensed under the GNU for VHF and UHF signals. Involvement in moon Software and the soundcard to the rescue general public licence. bounce by radio amateurs grew out of experiments by the military after World War II. Next to an antenna and radio, the PC and a The software supports five principal operating While the first amateur radio signals reflected sound card are important pieces of electronics modes: from the moon were received in 1953, the first two-way contact only took place in June of 1960. Using surplus parabolic dish antennas and high power klystron amplifiers, the Eimac Radio Club W6HB and the Rhododendron Swamp VHF Society W1BU achieved the first two-way EME contact on 1296 MHz. EME activity belongs to a group of activity often referred to as weak signal communication. Weak signal communication is where radio signals have signal strength levels that are close to or partially embedded in the natural noise. The noise level is influenced by several factors such as antenna and receiver properties - the noise generated in the antenna and receiver and the noise power that is received by the antenna. The signal strength of the detected information is determined by the transmitter output, antenna gain and the path loss between the receiver and the transmit antennas. 12 September 2006 - EngineerIT Nobel Prize winner makes amateur radio his hobby Joseph Hooton Taylor, Jr. K1JT is an American astrophysicist and winner of the 1993 Nobel Prize in Physics, shared with his former student Russell Alan Hulse, for the discovery of a new type of pulsar, a discovery that has opened up new possibilities for the study of gravitation. Educated at Haverford College (BA Physics 1963) and Harvard University (Ph.D. Astronomy 1968) and after a brief research position at Harvard, Taylor went to the University of Massachusetts, eventually becoming professor of astronomy and associate director of the Five College Radio Astronomy Observatory. Taylor’s thesis work was on lunar occultation measurements. About the time he completed his Ph.D., Jocelyn Bell discovered the first radio pulsars with a telescope near Cambridge, England. Taylor immediately went to the National Radio Astronomy Observatory’s telescopes in Green Bank, West Virginia, and participated in the discovery of the first pulsars discovered outside Cambridge. Since then, he has worked on all aspects of pulsar astrophysics. In 1980, he moved to Princeton University, where he was the James S. McDonnell Distinguished University Professor in Physics, having also served for six years as faculty dean. He has a keen interest in weak communication and developed the suite of WSJT software for weak signal experimentation by radio amateurs. He retired from teaching in 2006 and undoubtedly the amateur radio fraternity can expect some more exciting developments. • FSK441: for meteor scatter • JT65: for EME and extreme troposcatter • JT6M: for meteor scatter (optimised for 50 MHz) • EME Echo: for measuring your own echoes from the moon • CW: for EME QSOs using 15 WPM Morse code Local radio amateur shows how easy it really is Even with software support it is often said that EME is difficult and that one needs massive arrays of antennas that make one’s garden look like the Sentech antenna park in Meyerton. Not so, and Hannes Enslin ZS6JDE from Pretoria proved it. He was recently on a three week visit to Zambia (9J) and operated on 2m using the WSJT software. On 25 and 26 May 2006, during only two moonrise and two moonset windows, he made a total of 20 EME contacts on 144 MHz and at least eight other stations were heard but not worked due to the basic station he was running. The station consisted of a Yaesu FT857D running 9 W into a TE Systems 400W linear amplifier and feeding a 9 element 2M antenna using low loss coaxial cable. The antenna was mounted on a portable tripod and elevated with a weight and rope system. Of course a call like 9J2JD is sought after in the log for 2m EME everywhere in the world. But it is still quite remarkable that so many stationsw were worked in such a short time with what can be described as minimal equipment for EME. Contact Hans van de Groenendaal, Connected Communication, Tel (012) 991-4662, [email protected] ☐ 13 EngineerIT - September 2006 .
Recommended publications
  • Investigation and Analysis of Gravitational Waves Using Data from the Lvt151012 Event
    INVESTIGATION AND ANALYSIS OF GRAVITATIONAL WAVES USING DATA FROM THE LVT151012 EVENT Joalda Morancy September 11th, 2017 Pioneer Academics: Summer 2017 Mentor: Eric Myers ABSTRACT The LVT151012 event produces numerous questions on its validity due to various factors. In this paper, I investigate this and analyze the LIGO data for this specific event. I will first give background on what gravitational waves are and how they’re measured, my methodology in investigating the event, and a conclusion of my results. This paper is targeted at anyone who is interested in learning about gravitational waves and has a basic understanding of physics. INTRODUCTION On October 12th, 2015, LIGO made its second detection of gravitational waves. This event, known as LVT151012, is theorized to be the result of the inspiral of two black holes in a binary system of 23 and 13 solar masses (Figure 1). This event isn’t confirmed completely yet, which is the reason why it is given the acronym LVT, meaning “LIGO-Virgo Trigger”, and not GW like others, which stands for “Gravitational Wave” [1]. Figure 1: Graphic showing the number of solar masses of all known gravitational wave detections, including the LVT151012 event. [2] A major difference between this specific detection and others is that the confidence is significantly lower, and it is not enough to make the cut for an official detection. The confidence level is 1.7σ, and the traditional amount that a detection has to be greater than is 5σ. LVT151012 also has a much greater distance compared to all other detections, which comes out to be approximately 1000 Mpc.
    [Show full text]
  • Recent Observations of Gravitational Waves by LIGO and Virgo Detectors
    universe Review Recent Observations of Gravitational Waves by LIGO and Virgo Detectors Andrzej Królak 1,2,* and Paritosh Verma 2 1 Institute of Mathematics, Polish Academy of Sciences, 00-656 Warsaw, Poland 2 National Centre for Nuclear Research, 05-400 Otwock, Poland; [email protected] * Correspondence: [email protected] Abstract: In this paper we present the most recent observations of gravitational waves (GWs) by LIGO and Virgo detectors. We also discuss contributions of the recent Nobel prize winner, Sir Roger Penrose to understanding gravitational radiation and black holes (BHs). We make a short introduction to GW phenomenon in general relativity (GR) and we present main sources of detectable GW signals. We describe the laser interferometric detectors that made the first observations of GWs. We briefly discuss the first direct detection of GW signal that originated from a merger of two BHs and the first detection of GW signal form merger of two neutron stars (NSs). Finally we present in more detail the observations of GW signals made during the first half of the most recent observing run of the LIGO and Virgo projects. Finally we present prospects for future GW observations. Keywords: gravitational waves; black holes; neutron stars; laser interferometers 1. Introduction The first terrestrial direct detection of GWs on 14 September 2015, was a milestone Citation: Kro´lak, A.; Verma, P. discovery, and it opened up an entirely new window to explore the universe. The combined Recent Observations of Gravitational effort of various scientists and engineers worldwide working on the theoretical, experi- Waves by LIGO and Virgo Detectors.
    [Show full text]
  • Neutron Stars
    Neutron Stars and their importance in the general scheme of physics J.R.Stone Oxford/Tennessee/Oak Ridge OUTLINE: I. Compact objects: white dwarfs, neutron stars and black holes Collapse of massive stars Pulsars II. Cooling of proto-neutron stars and formaon of microscopic make-up of the star. Possible exoc stars III. Theorecal models of neutron stars and their impact in the general context of physics. Type II supernovae core collapse: forms a neutron star or a black hole. A BIT OF HISTORY: 1931: Collapse of red giants and white dwarfs are known. White dwarfs (1910 – Henry Norris Russel, named 1922 Willem Luyten): When red giants consume all their accessible fuel, the cores of the stars shrink to a very hot very dense object – not a star in technical sense: Mass ~ 1 solar mass , radius ~ 7000 km Energy comes from gravitaonal contracSon Radiaon comes from emission of stored heat (not fusion reacSons) Example: Sirius B (Hubble image) Material Density in kg/m3 Notes Water (fresh) 1,000 At STP Osmium 22,610 Near room temperature The core of the Sun ~150,000 White dwarf star 1 × 109 Atomic nuclei 2.3 × 1017 Neutron star core 8.4 × 1016 − 1 × 1018 Black hole 2 × 1030 CriScal density of an Earth-mass black hole Final stage of stars which are not very massive (over 97% of stars of our Galaxy): I. Hydrogen-fusing (main-sequence star of low or medium mass below 9-10 solar masses) II. Helium fusing to carbon and oxygen red giant in the core by the triple alpha process III.
    [Show full text]
  • The Einstein Toolkit: an Open Framework for Numerical General Relativistic Astrophysics
    Roberto De Pietri Parma University and INFN http://www.einsteintoolkit.org The Einstein Toolkit: an open framework for Numerical General Relativistic Astrophysics. The Einstein Toolkit (ET) is an open-source computational infrastructure for that allows to solve the Einstein’s Equations coupled to Matter on a three-dimensional grid. I will discuss the implemented numerical methods and its scaling on modern HPC environment. Moreover, I will give details on its usage to model the merger of Neutron Stars and to computed the Gravitational Waves signal emitted in the process. Bologna, November the 2th, 2016. HPC Methods for Computational Fluid Dynamics and Astrophysics @ CINECA 1 Main target: Gravitational Wave Physics Models & Simulation Observations Scientific Discovery! Theory Gµν = 8π Tµν Compact binaries, supernovae collapse, gamma-ray bursts, oscillating NSs, gravitational waves, … Bologna, November the 2th, 2016. HPC Methods for Computational Fluid Dynamics and Astrophysics @ CINECA 2 Observation of Gravitational Waves from a Binary Black Hole Merger B. P. Abbott et al. (LIGO Scientific Collaboration and Virgo Collaboration) Phys. Rev. Lett. 116, 061102 – Published 11 February 2016 Need to model source: GW has been detected ❖ The gravitational waves were detected on September 14, 2015 at 5:51 a.m. Eastern Daylight Time (09:51 UTC) by both of the twin Laser Interferometer Gravitational-wave Observatory (LIGO) detectors, located in Livingston, Louisiana, and Hanford, Washington, USA. ❖ The signal was observed with a matched- filter signal-to-noise ratio of 24 and a false alarm rate estimated to be less than 1 event per 203 000 years, equivalent to a significance greater than 5.1σ.
    [Show full text]
  • Recent Astronomical Tests of General Relativity
    Vol. 10(2), pp. 90-105, 30 Janaury, 2015 DOI: 10.5897/IJPS2014.4236 Article Number: 26552F450052 International Journal of Physical ISSN 1992 - 1950 Copyright © 2015 Sciences Author(s) retain the copyright of this article http://www.academicjournals.org/IJPS Review Recent astronomical tests of general relativity Keith John Treschman 51 Granville Street Wilston 4051 Australia. Received 16 November, 2014; Accepted 22 December, 2014 This history of experimentation relevant to general relativity covers the time post-1928. Classes of investigation are the weak equivalence principle (equivalence of inertial and gravitational mass and gravitational redshift), orbital precession of a body in gravitational fields (the relativistic perihelion advance of the planets, the relativistic periastron advance of binary pulsars, geodetic precession and Lense-Thirring effect), light propagation in gravitational fields (gravitational optical light deflection, gravitational radio deflection due to the Sun, gravitational lensing, time dilation and atomic clocks) and strong gravity implications (Nordtved effect and potential gravitational waves). The results of experiments are analysed to conclude to what extent they support general relativity. A number of questions are then answered: (a) how much evidence exists to support general relativity, (b) is it a reasonable way of thinking and (c) what is the niche it may occupy? Key words: general relativity, equivalence principle, orbital precession, gravitational fields. INTRODUCTION The special theory of relativity came from the mind of concepts to include an accelerated frame of reference Albert Einstein (1879-1955) in 1905 (Einstein, 1905). In it (Einstein, 1916). Within his general theory of relativity he he proposed that the laws of physics take the same form united space and time and presented gravity as a in all inertial frames and that the velocity of light is geometrical interpretation of how bodies move in the constant irrespective of the motion of the emitting body.
    [Show full text]
  • Contributions of Civilizations to International Prizes
    CONTRIBUTIONS OF CIVILIZATIONS TO INTERNATIONAL PRIZES Split of Nobel prizes and Fields medals by civilization : PHYSICS .......................................................................................................................................................................... 1 CHEMISTRY .................................................................................................................................................................... 2 PHYSIOLOGY / MEDECINE .............................................................................................................................................. 3 LITERATURE ................................................................................................................................................................... 4 ECONOMY ...................................................................................................................................................................... 5 MATHEMATICS (Fields) .................................................................................................................................................. 5 PHYSICS Occidental / Judeo-christian (198) Alekseï Abrikossov / Zhores Alferov / Hannes Alfvén / Eric Allin Cornell / Luis Walter Alvarez / Carl David Anderson / Philip Warren Anderson / EdWard Victor Appleton / ArthUr Ashkin / John Bardeen / Barry C. Barish / Nikolay Basov / Henri BecqUerel / Johannes Georg Bednorz / Hans Bethe / Gerd Binnig / Patrick Blackett / Felix Bloch / Nicolaas Bloembergen
    [Show full text]
  • University of Groningen the Final State Tsang, Ka Wa
    University of Groningen The Final State Tsang, Ka Wa DOI: 10.33612/diss.160948839 IMPORTANT NOTE: You are advised to consult the publisher's version (publisher's PDF) if you wish to cite from it. Please check the document version below. Document Version Publisher's PDF, also known as Version of record Publication date: 2021 Link to publication in University of Groningen/UMCG research database Citation for published version (APA): Tsang, K. W. (2021). The Final State: the fate of relativistic compact objects after merger. University of Groningen. https://doi.org/10.33612/diss.160948839 Copyright Other than for strictly personal use, it is not permitted to download or to forward/distribute the text or part of it without the consent of the author(s) and/or copyright holder(s), unless the work is under an open content license (like Creative Commons). The publication may also be distributed here under the terms of Article 25fa of the Dutch Copyright Act, indicated by the “Taverne” license. More information can be found on the University of Groningen website: https://www.rug.nl/library/open-access/self-archiving-pure/taverne- amendment. Take-down policy If you believe that this document breaches copyright please contact us providing details, and we will remove access to the work immediately and investigate your claim. Downloaded from the University of Groningen/UMCG research database (Pure): http://www.rug.nl/research/portal. For technical reasons the number of authors shown on this cover page is limited to 10 maximum. Download date: 03-10-2021 The Final State The fate of relativistic compact objects after merger Ka Wa Tsang A thesis presented for the degree of Doctor of Philosophy Nikhef The Netherlands 2020 Summer © 2020 Ka Wa Tsang ISBN: 978-94-6419-125-7 Printed in the Netherlands by: Gildeprint Cover design by: Helena CYC This work is part of the research program supported by the Nederlandse organisatie voor Weten- schappelijk Onderzoek (NWO).
    [Show full text]
  • 24 August 2013 Seminar Held
    PROCEEDINGS OF THE NOBEL PRIZE SEMINAR 2012 (NPS 2012) 0 Organized by School of Chemistry Editor: Dr. Nabakrushna Behera Lecturer, School of Chemistry, S.U. (E-mail: [email protected]) 24 August 2013 Seminar Held Sambalpur University Jyoti Vihar-768 019 Odisha Organizing Secretary: Dr. N. K. Behera, School of Chemistry, S.U., Jyoti Vihar, 768 019, Odisha. Dr. S. C. Jamir Governor, Odisha Raj Bhawan Bhubaneswar-751 008 August 13, 2013 EMSSSEM I am glad to know that the School of Chemistry, Sambalpur University, like previous years is organizing a Seminar on "Nobel Prize" on August 24, 2013. The Nobel Prize instituted on the lines of its mentor and founder Alfred Nobel's last will to establish a series of prizes for those who confer the “greatest benefit on mankind’ is widely regarded as the most coveted international award given in recognition to excellent work done in the fields of Physics, Chemistry, Physiology or Medicine, Literature, and Peace. The Prize since its introduction in 1901 has a very impressive list of winners and each of them has their own story of success. It is heartening that a seminar is being organized annually focusing on the Nobel Prize winning work of the Nobel laureates of that particular year. The initiative is indeed laudable as it will help teachers as well as students a lot in knowing more about the works of illustrious recipients and drawing inspiration to excel and work for the betterment of mankind. I am sure the proceeding to be brought out on the occasion will be highly enlightening.
    [Show full text]
  • Black Holes and Gravitational Waves
    Black Holes and Gravitational Waves Maria Teodora Stanescu Content 1.What are black holes? ➢ Definition & characteristics ➢ How do they form? ➢ Types of black holes 2.What are gravitational waves? ➢ Types of gravitational waves 3.History 4.How can we detect gravitational waves? ➢ LIGO ➢ Gravitational waves observatories ➢ Results 5. Conclusions 6.Bibliography 1. What are black holes? Definition and characteristics ● Black holes are so dense and ● If there is matter around, the compact objects that not even object is surrounded by an light can escape their accretion disc (a disc shaped gravitational field zone consisting in gas, dust and other material that orbits around the black hole) ● Every black hole has a gravitational singularity (a compact center that is constantly collapsing toward 0 volume) and an event horizon (an invisible limit surrounding the singularity where the escape velocity is equal to the speed of light) → according to general relativity How do they form? ● It is believed that a black hole is an ending stage of a star’s life cycle ● A star starts “dying” when it uses up most of it’s fuel. At that point, nothing can balance the gravitational pull and the core collapses ● Depending on the star’s mass, it can turn into a white dwarf (m ≤ 1,4M☉ ), a neutron star (1,4M☉ < m < 3 M ☉ ) or a stellar mass black hole (m > 3M☉ ) 1 solar mass = 1M☉ = 2 x 10³ºkg Types of black holes Observed ● Stellar-mass black holes ➢ Have less than 20 solar masses ● Supermassive black holes ➢ Have more than one million solar masses Theoretically predicted ● Intermediate-mass black holes ➢ have between 20 and 1.000.000 solar masses ● Miniature black holes ➢ hypothetical tiny black holes; ➢ are smaller than stellar mass black holes ● Another classification is based on the rotation ➢ Spinning black holes ➔ Kerr black holes ➢ Non-spinning black holes ➔ Schwarzschild black holes 2.
    [Show full text]
  • Imprints of Early Universe on Gravitational Waves from First-Order Phase Transition in QCD
    Prepared for submission to JHEP Imprints of Early Universe on Gravitational Waves from First-Order Phase Transition in QCD Meng-Wei Lia, Yi Yanga;b and Pei-Hung Yuana;c;d;e aDepartment of Electrophysics, National Chiao Tung University, Hsinchu, ROC bPhysics Division, National Center for Theoretical Sciences, Hsinchu, ROC cDepartment of Physics, Chung Yuan Christian University, Taoyuan City, ROC dSchool of physics, University of Chinese Academy of Sciences, Beijing 100049, China eKavli Insititute for Theoretical Sciences, University of Chinese Academy of Sciences, Beijing 100049, China E-mail: [email protected], [email protected], [email protected] Abstract: We study the gravitational wave spectrum from the confinement-deconfinement phase transi- tion in the holographic QCD models for both light quark and heavy quark. We obtain the gravitational wave spectrum in the deflagration, detonation and runaway cases for different chemical potentials and duration of the phase transition. We find that the gravitational wave spectrum could be observed by EPTA/IPTA and eLISA for large chemical potential and short duartion of phase transtions. arXiv:1812.09676v1 [hep-th] 23 Dec 2018 Contents 1 Introduction 1 2 Deconfinement Phase Transition in Holographic QCD5 2.1 Review of EMS System5 2.2 Meson Mass Spectrum7 2.3 Phase Structure of the Black Hole Background9 2.3.1 Phase Transition for Light Quarks9 2.3.2 Phase Transition for Heavy Quarks 11 3 Gravitational Waves 12 3.1 Bubbles Collision 14 3.2 Sound Waves and MHD Turbulence 15 3.3 Gravitational Waves Spectrum 17 4 Conclusion 21 1 Introduction The idea of Gravitational wave (GW) was first proposed by Albert Einstein in 1916 [1,2], and have been developing our understanding by Josh Goldberg in 1957, especially how a binary star system generates GWs [3].
    [Show full text]
  • 1Pg 1 Reading the Works of Isaac Asimov the American Author Isaac Asimov (1920–1992) Was One of the 20Th Century’S Most Prolific Authors
    Notes Where Is Everybody? 1Pg 1 reading the works of Isaac Asimov The American author Isaac Asimov (1920–1992) was one of the 20th century’s most prolific authors. He wrote on a vast number of topics—from the Bible to Shakespeare—but it was his science books, both fiction and non-fiction, that had the most impact on me. For a memoir, written towards the end of his life, see Asimov (1994). 2Pg 1 appeared in successive issues The “pro-Fermi” article, by the American geologist and science fiction writer Stephen Lee Gillett (1953–), appeared in the August 1984 issue of Asimov’s. The rebuttal, by the American scientist and author Robert A. Freitas Jr (1952–), appeared in the September issue. A few years later, Gillett expanded upon his original article and pointed out a different interpretation of the “lemming paradox” introduced by Freitas and discussed here on page 2. If Earth were empty except for lemmings then the creatures would be everywhere; but Earth teems with other living things, which out-compete lemmings and limit their spread. The correct conclusion to draw from the non-observation of lemmings is that Earth has an abundance of living species competing for resources (which we knew anyway, because we see life all around us). When we look into space, however, we see nothing that indicates the presence of life. 3Pg 5 latest cosmological measurements The WMAP and Planck space mis- sions have tied down the key numbers describing our universe. For details see, for example, NASA (2012) and ESA (2014). The Physicist Enrico Fermi 4Pg 10 precocious ability in mathematics For details of Fermi’s life I consulted two sources: a biography written by his wife Laura (Fermi 1954); and © Springer International Publishing Switzerland 2015 339 S.
    [Show full text]
  • Nobelovy Ceny Za Fyziku - Obor Astrofyzika
    MASARYKOVA UNIVERZITA PEDAGOGICKÁ FAKULTA KATEDRA FYZIKY BAKALÁŘSKÁ PRÁCE NOBELOVY CENY ZA FYZIKU - OBOR ASTROFYZIKA Brno 2008 Vedoucí bakalářské práce: prof. RNDr. Vladislav Navrátil, CSc. Autor práce: Svobodová Petra 1 Bibliografický záznam Svobodová, Petra. Nobelovy za fyziku – obor astrofyzika: Bakalářská práce. Brno: Masarykova univerzita, Fakulta pedagogická, Katedra fyziky, 2008. 54s. Vedoucí bakalářské práce prof. RNDr. Vladislav Navrátil, Csc. Anotace Bakalářská práce “Nobelovy ceny za fyziku, obor astrofyzika” nabízí pohled na úspěchy astronomie prostřednictvím šesti ročníků Nobelových cen za fyziku, ve kterých získali ocenění právě astronomové. Cílem práce je stručný popis jednotlivých objevů jako je např. reliktní záření, pulzary, nebo vznik některých dílčích podoborů astronomie. Součástí práce je životopis Alfreda Nobela a nástin historického vývoje astronomie. Klíčová slova Alfred Nobel, historie astronomie, reliktní záření, pulzary, radioastronomie, rentgenová astronomie, neutrina, vývoj hvězd, družice COBE. Anotation The Bachelor thesis “ Nobel physics prizes, astrophysics field” offers look on successes in astronomy through six year's volume of Nobel physics prizes, in which astronomers were awarded. The goal of this thesis is a brief description of particular findings as relict radiation, pulsars or origin of some subfields of astronomy. Part of the thesis is a biography of Alfred Nobel and an outline of historical development of atronomys. Key words Alfred Nobel , history of astronomy, relict radiation, pulsars, radioastronomy, x – ray astronomy, neutrins, evolution of stars, satellite COBE. 2 PODĚKOVÁNÍ Děkuji prof. RNDr. Vladislavu Navrátilovy, CSc. za cenné rady a poznámky, které jsem při vypracování této bakalářské práce uplatnila a za poskytnutí potřebné literatury. 3 PROHLÁŠENÍ Prohlašuji, že jsem bakalárskou práci „Nobelovy ceny za fyziku – obor astrofyzika“ vypracovala samostatně podle pokynů vedoucího práce a s použitím literatury uvedené v seznamu.
    [Show full text]