A Nature of Science Guided Approach to the Physics Teaching of Cosmic Rays
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Igor Tamm 1895 - 1971 Awarded the Nobel Prize for Physics in 1958
Igor Tamm 1895 - 1971 Awarded the Nobel Prize for Physics in 1958 The famous Russian physicist Igor Evgenievich Tamm is best known for his theoretical explanation of the origin of the Cherenkov radiation. But really his works covered various fields of physics: nuclear physics, elementary particles, solid-state physics and so on. In about 1935, he and his colleague, Ilya Frank, concluded that although objects can’t travel faster than light in a vacuum, they can do so in other media. Cherenkov radiation is emitted if charged particles pass the media faster than the speed of light ! For this research Tamm together with his Russian colleagues was awarded the 1958 Nobel Prize in Physics. Igor Tamm was born in 1895 in Vladivostok when Russia was still ruled by the Tsar. His father was a civil engineer who worked on the electricity and sewage systems. When Tamm was six years old his family moved to Elizavetgrad, in the Ukraine. Tamm led an expedition to He graduated from the local Gymnasium in 1913. Young Tamm dreamed of becoming a revolutionary, but his father disapproved . However only his mother was able to convince him to search for treasure in the Pamirs change his plans. She told him that his father’s weak heart could not take it if something happened to him. In 1923 Tamm was offered a teaching post at the Second Moscow University and later he was And so, in 1913, Tamm decided to leave Russia for a year and continue his studies in Edinburgh. awarded a professorship at Moscow State University. -
People and Things
sure that it is good for us to search though we could predict how every chaos. And of course it's even for them, in the same way that molecule in a glass of water would more true for sciences outside the Spanish explorers, whey they first behave, nowhere in the mountain area of physics, especially for pushed northward from the central of computer printout would we find sciences like astronomy and biolo parts of Mexico, were searching for the properties of water that really gy, for which also an element of the seven golden cities of Cibola. interest us, properties like tempera history enters. They didn't find them, but they ture and entropy. These properties I'm also not saying that elemen found other useful things, like have to be dealt with in their own tary particle physics is more impor Texas. terms, and for this we have the tant than other branches of phys Let me also say what I don't science of thermodynamics, which ics. All I'm saying is that, because mean by final, underlying, laws of deals with heat without at every of its concern with underlying laws, physics. I don't mean that other step reducing it to the properties of elementary particle physics has a branches of physics are in danger molecules or elementary particles. special importance of its own, even of being replaced by some ultimate There is no doubt today that, ul though it's not necessarily of great version of elementary particle timately, thermodynamics is what it immediate practical value. -
Ninety Years of X-Ray Spectroscopy in Italy 1896-1986
Ninety years of X-ray spectroscopy in Italy 1896-1986 Vanda Bouché1,2, Antonio Bianconi1,3,4 1 Rome Int. Centre Materials Science Superstripes (RICMASS), Via dei Sabelli 119A, 00185Rome, Italy 2 Physics Dept., Sapienza University of Rome, P.le A. Moro 2, 00185 Rome, Italy 3 Institute of Crystallography of Consiglio Nazionale delle Ricerche, IC-CNR, Montero- tondo, Rome, Italy 4 National Research Nuclear University MEPhI (Moscow Engineering Physics Institute), Kashirskoeshosse 31, 115409 Moscow, Russia Ninety years of X-ray spectroscopy research in Italy, from the X-rays dis- covery (1896), and the Fermi group theoretical research (1922-1938) to the Synchrotron Radiation research in Frascati from 1963 to 1986 are here summarized showing a coherent scientific evolution which has evolved into the actual multidisciplinary research on complex phases of condensed mat- ter with synchrotron radiation 1. The early years of X-ray research The physics community was very quick to develop an intense research in Italy on X rays, after the discovery on 5th January, 1896 by Röngten in Munich. Antonio Garbasso in Pisa [1], and then in Rome Alfonso Sella, with Quirino Majorana, Pietro Blaserna and Garbasso, published several papers on Nuovo Cimento [2], starting the Italian experimental school on X-rays research in XIX century [3]. The focus was on the mechanism of the emission by the X-ray tubes, the nature of X-rays (wave or particles), the propagation characteristics in the matter, the absorption and diffusion. Cambridge and Edinburgh at the beginning of the XX century became the world hot spots of X-ray spectroscopy with Charles Barkla who demonstrated the electromagnetic wave nature of X-ray propagation in the vacuum, similar with light and Henry Moseley, who studied the X-ray emission spectra, recorded the X-ray emission lines of most of the elements of the Mendeleev atomic table. -
Marietta Blau in the History of Cosmic Rays Per Carlson
Physics Today Marietta Blau in the history of cosmic rays Per Carlson Citation: Physics Today 65(10), 8 (2012); doi: 10.1063/PT.3.1729 View online: http://dx.doi.org/10.1063/PT.3.1729 View Table of Contents: http://scitation.aip.org/content/aip/magazine/physicstoday/65/10?ver=pdfcov Published by the AIP Publishing Reuse of AIP Publishing content is subject to the terms at: https://publishing.aip.org/authors/rights-and-permissions. Download to IP: 149.28.91.2 On: Thu, 30 Jun 2016 17:53:16 readers’ forum Marietta Blau in the history of cosmic rays er Carlson, in his article “A century have been formed by cosmic particles ex- contributions deserve a prominent and Pof cosmic rays” (PHYSICS TODAY, plosively disintegrating heavy nuclei in permanent place in any history of February 2012, page 30), states that the emulsion. That discovery, in 1937, cosmic-ray and particle physics. And I the investigation of cosmic rays opened created a sensation among nuclear and believe it is also important, given the up the field of particle physics. How- cosmic-ray physicists worldwide, and by much-discussed problem of the under- ever, he neglects the importance of nu- demonstrating that nuclear emulsions representation of women in physics, clear emulsions in the progress of par- had come of age for recording rare high- that PHYSICS TODAY take care not to ticle physics, and he fails to mention a energy nuclear events, it paved the way overlook women who, like Blau, made key figure, Austrian physicist Marietta for further research in particle physics. -
Marietta Blau's Work After World War II Arnold Perlmutter Department Of
View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by CERN Document Server Marietta Blau's Work After World War II Arnold Perlmutter Department of Physics University of Miami Coral Gables, Florida 33124 completed, October 27, 2000 This paper has been translated into German and will be included, in a somewhat altered form, in a book Sterne der Zertrummerung, Marietta Blau, Wegbereiterin der Moderne Teilchenphysik, Brigitte Strohmaier and Robert Rosner, eds., Boehlau Verlag, Wien. 1 A. Introduction While it is clear that the seminal work of Dr. Marietta Blau was done in the 1920’s and especially in the 1930’s, it is also evident that her separation from the great research centers from 1938 to 1944 had a devastating effect on her productivity. It was during this period that Cecil F. Powell, at Bristol University, made use of Blau’s earlier tutelage on the preparation and analysis of photographic emulsions. According to Blau’s conversations with me (much later), she consulted with Ilford in the 1930’s to improve emulsion sensitivity and uniformity, and presumably had also imparted crucial lore of the technique to Powell. C.F. Powell, who had been a student of C.T.R. Wilson, had employed cloud chambers in a wide variety of studies in vulcanology, mechanical engineering, and nuclear physics. In 1938 and 1939 Powell’s experimental efforts turned to the use of photographic emulsions to investigate neutron interactions, and then to nuclear reactions1. With the coming of the war and then the British nuclear atomic bomb project, Powell established a formidable laboratory and collaboration for the analysis of emulsions and for their improvement by Ilford and Kodak. -
Electron-Positron Pairs in Physics and Astrophysics
Electron-positron pairs in physics and astrophysics: from heavy nuclei to black holes Remo Ruffini1,2,3, Gregory Vereshchagin1 and She-Sheng Xue1 1 ICRANet and ICRA, p.le della Repubblica 10, 65100 Pescara, Italy, 2 Dip. di Fisica, Universit`adi Roma “La Sapienza”, Piazzale Aldo Moro 5, I-00185 Roma, Italy, 3 ICRANet, Universit´ede Nice Sophia Antipolis, Grand Chˆateau, BP 2135, 28, avenue de Valrose, 06103 NICE CEDEX 2, France. Abstract Due to the interaction of physics and astrophysics we are witnessing in these years a splendid synthesis of theoretical, experimental and observational results originating from three fundamental physical processes. They were originally proposed by Dirac, by Breit and Wheeler and by Sauter, Heisenberg, Euler and Schwinger. For almost seventy years they have all three been followed by a continued effort of experimental verification on Earth-based experiments. The Dirac process, e+e 2γ, has been by − → far the most successful. It has obtained extremely accurate experimental verification and has led as well to an enormous number of new physics in possibly one of the most fruitful experimental avenues by introduction of storage rings in Frascati and followed by the largest accelerators worldwide: DESY, SLAC etc. The Breit–Wheeler process, 2γ e+e , although conceptually simple, being the inverse process of the Dirac one, → − has been by far one of the most difficult to be verified experimentally. Only recently, through the technology based on free electron X-ray laser and its numerous applications in Earth-based experiments, some first indications of its possible verification have been reached. The vacuum polarization process in strong electromagnetic field, pioneered by Sauter, Heisenberg, Euler and Schwinger, introduced the concept of critical electric 2 3 field Ec = mec /(e ). -
50 31-01-2018 Time: 60 Min
8thAHMED BIN ABOOD MEMORIAL State Level Physics-Maths Knowledge Test-2018 Organized by Department of Physics Department of Mathematics Milliya Arts, Science and Management Science College, BEED Max. Marks: 50 31-01-2018 Time: 60 min Instructions:- All the questions carry equal marks. Mobile and Calculators are not allowed. Student must write his/her names, college name and allotted seat number on the response sheet provided. Student must stick the answer in the prescribed response sheet by completely blacken the oval with black/blue pen only. Incorrect Method Correct Method Section A 1) If the earth completely loses its gravity, then for any body……… (a) both mass and weight becomes zero (b) neither mass nor weight becomes zero (c) weight becomes zero but not the mass (d) mass becomes zero but not the weight 2) The angular speed of a flywheel is 3π rad/s. It is rotating at…….. (a) 3 rpm (b) 6 rpm (c) 90 rpm (d) 60 rpm 3) Resonance occurs when …. (a) a body vibrates at a frequency lower than its normal frequency. (b) a body vibrates at a frequency higher than its normal frequency. (c) a body is set into vibrations with its natural frequency of another body vibrating with the same frequency. (d) a body is made of the same material as the sound source. 4) The SI unit of magnetic flux density is…… (a) tesla (b) henry (c) volt (d) volt-second 5) Ampere’s circuital law is integral form of….. (a) Lenz’s law (b) Faraday’s law (c) Biot-Savart’s law (d) Coulomb’s law 1 6) The energy band gap is highest in the case of ……. -
Muons for Time-Dependent Studies in Magnetism
Muons for time-dependent studies in magnetism D. Andreica, Faculty of Physics, Babeş-Bolyai University Cluj-Napoca, ROMANIA The European School on Magnetism, 22.08-01.09 2011, Târgovişte, ROMANIA Muons for time-dependent studies in magnetism Content: Introduction: muon properties; history. SR method: muon beams; sample environment; Muons for solid state physics & examples. ESM 2011-Târgovişte, ROMANIA Muons for time-dependent studies in magnetism In a few words: Polarized muons (S=1/2) are implanted into the sample The spin of the muon precesses around the local magnetic field The muons decay (2.2 s) by emitting a positron preferentially along the spin direction. The positrons are counted/recorded in hystograms along certain directions = the SR spectra = the physics of your sample. ESM 2011-Târgovişte, ROMANIA Muons for time-dependent studies in magnetism It belongs to the family of NMR, EPR, PAC, neutron scattering and Mossbauer experimental methods. ESM 2011-Târgovişte, ROMANIA Muons for time-dependent studies in magnetism ESM 2011-Târgovişte, ROMANIA Muons for time-dependent studies in magnetism -Small magnetic probe. Spin: 1/2, Mass: m = 206.7682838(54) me = 0.1126095269(29) mp -Charge: +-e - Muon beam 100% polarized → possibility to perform ZF measurements - Can be implanted in all type of samples - Gyromagnetic ratio: = 2 x 13.553882 (0.2 ppm) kHz/Gauss → senses weak magnetism. - Allows independent determination of the magnetic volume and of magnetic moment. - Possibility to detect disordered magnetism (spin glass) or short range magnetism. How ? ESM 2011-Târgovişte, ROMANIA Muons for time-dependent studies in magnetism The muon decay into an electron and two neutrinos after an average lifetime of = 2.19703(4) s: + + e + e + The decay is highly anisotropic. -
Photon Mapping Superluminal Particles
EUROGRAPHICS 2020/ F. Banterle and A. Wilkie Short Paper Photon Mapping Superluminal Particles G. Waldemarson1;2 and M. Doggett2 1Arm Ltd, Sweden 2 Lund University, Sweden Abstract One type of light source that remains largely unexplored in the field of light transport rendering is the light generated by superluminal particles, a phenomenon more commonly known as Cherenkov radiation [C37ˇ ]. By re-purposing the Frank-Tamm equation [FT91] for rendering, the energy output of these particles can be estimated and consequently mapped to photons, making it possible to visualize the brilliant blue light characteristic of the effect. In this paper we extend a stochastic progressive photon mapper and simulate the emission of superluminal particles from a source object close to a medium with a high index of refraction. In practice, the source is treated as a new kind of light source, allowing us to efficiently reuse existing photon mapping methods. CCS Concepts • Computing methodologies ! Ray tracing; 1. Introduction in the direction of the particle but will not otherwise cross one an- other, as depicted in figure 1. However, if the particle travels faster In the late 19th and early 20th century, the phenomenon today than these spheres the waves will constructively interfere, generat- known as Cherenkov radiation were predicted and observed a num- ing coherent photons at an angle proportional to the velocity of the ber of times [Wat11] but it was first properly investigated in 1934 particle, similar to the propagation of a sonic boom from supersonic by Pavel Cherenkov under the supervision of Sergey Vavilov at the aircraft. Formally, this occurs when the criterion c0 = c < v < c Lebedev Institute [C37ˇ ]. -
Harvey Fletcher and Henry Eyring: Men of Faith and Science
Edward L. Kimball Harvey Fletcher and Henry Eyring: Men of Faith and Science The year 1981 saw the deaths of Harvey Fletcher and Henry Eyring, men of great religious faith whose superb professional achievements placed them in the first ranks of the nation's scientists. (See Steven H. Heath's "The Reconcilia- tion of Faith and Science: Henry Eyring's Achievement," this issue.) Both could be said to have had simple religious faith — not because they were un- complicated people incapable of subtlety, but because their religious character was early and firmly grounded in a few fundamentals. This freed them from a life of continuing doubt and struggle. The two men, seventeen years apart in age, had a kind of family relation- ship. Henry Eyring's uncle Carl Eyring (after whom BYU's Eyring Science Center is named) married Fern Chipman; Harvey Fletcher married her sister Lorena. After their spouses died, Harvey Fletcher and Fern Chipman Eyring married. As a result, Henry Eyring called him Uncle Harvey. But that was not unique. Nearly everyone else did, too. Harvey Fletcher was born in 1884 in a little frame house in Provo, Utah. Among his memories are attending the dedication of the Salt Lake Temple and shaking President Wilford Woodruff's hand. As a young boy, he recited a short poem at a program in the Provo Tabernacle; and after he finished, Karl G. Maeser, principal of the Brigham Young Academy, stopped him before he could resume his seat, put his hand on Harvey's head, and said, "I want this congregation to know that this little boy will one day be a great man." Instead of being pleased, Harvey was bothered; he perceived it as a prediction of politi- cal leadership, which he did not want. -
The Ship 2014/2015
A more unusual focus in your magazine this College St Anne’s year: architecture and the engineering skills that make our modern buildings possible. The start of our new building made this an obvious choice, but from there we go on to look at engineering as a career and at the failures and University of Oxford follies of megaprojects around the world. Not that we are without the usual literary content, this year even wider in range and more honoured by awards than ever. And, as always, thanks to the generosity and skills of our contributors, St Anne’s College Record a variety of content and experience that we hope will entertain, inspire – and at times maybe shock you. My thanks to the many people who made this issue possible, in particular Kate Davy, without whose support it could not happen. Hope you enjoy it – and keep the ideas coming; we need 2014 – 2015 them! - Number 104 - The Ship Annual Publication of the St Anne’s Society 2014 – 2015 The Ship St Anne’s College 2014 – 2015 Woodstock Road Oxford OX2 6HS UK The Ship +44 (0) 1865 274800 [email protected] 2014 – 2015 www.st-annes.ox.ac.uk St Anne’s College St Anne’s College Alumnae log-in area Development Office Contacts: Lost alumnae Register for the log-in area of our website Over the years the College has lost touch (available at https://www.alumniweb.ox.ac. Jules Foster with some of our alumnae. We would very uk/st-annes) to connect with other alumnae, Director of Development much like to re-establish contact, and receive our latest news and updates, and +44 (0)1865 284536 invite them back to our events and send send in your latest news and updates. -
Appendix I Lunar and Martian Nomenclature
APPENDIX I LUNAR AND MARTIAN NOMENCLATURE LUNAR AND MARTIAN NOMENCLATURE A large number of names of craters and other features on the Moon and Mars, were accepted by the IAU General Assemblies X (Moscow, 1958), XI (Berkeley, 1961), XII (Hamburg, 1964), XIV (Brighton, 1970), and XV (Sydney, 1973). The names were suggested by the appropriate IAU Commissions (16 and 17). In particular the Lunar names accepted at the XIVth and XVth General Assemblies were recommended by the 'Working Group on Lunar Nomenclature' under the Chairmanship of Dr D. H. Menzel. The Martian names were suggested by the 'Working Group on Martian Nomenclature' under the Chairmanship of Dr G. de Vaucouleurs. At the XVth General Assembly a new 'Working Group on Planetary System Nomenclature' was formed (Chairman: Dr P. M. Millman) comprising various Task Groups, one for each particular subject. For further references see: [AU Trans. X, 259-263, 1960; XIB, 236-238, 1962; Xlffi, 203-204, 1966; xnffi, 99-105, 1968; XIVB, 63, 129, 139, 1971; Space Sci. Rev. 12, 136-186, 1971. Because at the recent General Assemblies some small changes, or corrections, were made, the complete list of Lunar and Martian Topographic Features is published here. Table 1 Lunar Craters Abbe 58S,174E Balboa 19N,83W Abbot 6N,55E Baldet 54S, 151W Abel 34S,85E Balmer 20S,70E Abul Wafa 2N,ll7E Banachiewicz 5N,80E Adams 32S,69E Banting 26N,16E Aitken 17S,173E Barbier 248, 158E AI-Biruni 18N,93E Barnard 30S,86E Alden 24S, lllE Barringer 29S,151W Aldrin I.4N,22.1E Bartels 24N,90W Alekhin 68S,131W Becquerei