APS News September 2020, Vol. 29, No. 8
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
Simulating Physics with Computers
International Journal of Theoretical Physics, VoL 21, Nos. 6/7, 1982 Simulating Physics with Computers Richard P. Feynman Department of Physics, California Institute of Technology, Pasadena, California 91107 Received May 7, 1981 1. INTRODUCTION On the program it says this is a keynote speech--and I don't know what a keynote speech is. I do not intend in any way to suggest what should be in this meeting as a keynote of the subjects or anything like that. I have my own things to say and to talk about and there's no implication that anybody needs to talk about the same thing or anything like it. So what I want to talk about is what Mike Dertouzos suggested that nobody would talk about. I want to talk about the problem of simulating physics with computers and I mean that in a specific way which I am going to explain. The reason for doing this is something that I learned about from Ed Fredkin, and my entire interest in the subject has been inspired by him. It has to do with learning something about the possibilities of computers, and also something about possibilities in physics. If we suppose that we know all the physical laws perfectly, of course we don't have to pay any attention to computers. It's interesting anyway to entertain oneself with the idea that we've got something to learn about physical laws; and if I take a relaxed view here (after all I'm here and not at home) I'll admit that we don't understand everything. -
Wiki Template-1Eb7p59
Wikipedia Reader https://en.wikipedia.org/wiki/Aurora Selected by Julie Madsen - Entry 10 1 Aurora From Wikipedia, the free encyclopedia An aurora, sometimes referred to as a polar lights or north- ern lights, is a natural light display in the sky, predominantly seen in the high latitude (Arctic and Antarctic) regions.[1] Au- roras are produced when the magnetosphere is sufficiently disturbed by the solar wind that the trajectories of charged particles in both solar wind and magnetospheric plasma, mainly in the form of electrons and protons, precipitate them into the upper atmosphere (ther- mosphere/exosphere), where their energy is lost. The resulting ion- ization and excitation of atmospheric constituents emits light of varying color and complexity. The form of the aurora, occur- ring within bands around both polar regions, is also dependent on the amount of acceleration imparted to the precipitating parti- cles. Precipitating protons generally produce optical emissions as incident hydrogen atoms after gaining electrons from the atmosphere. Proton Images of auroras from around the world, auroras are usually observed at including those with rarer red and blue lower latitudes.[2] lights Wikipedia Reader 2 May 1 2017 Contents 1 Occurrence of terrestrial auroras 1.1 Images 1.2 Visual forms and colors 1.3 Other auroral radiation 1.4 Aurora noise 2 Causes of auroras 2.1 Auroral particles 2.2 Auroras and the atmosphere 2.3 Auroras and the ionosphere 3 Interaction of the solar wind with Earth 3.1 Magnetosphere 4 Auroral particle acceleration 5 Auroral events of historical significance 6 Historical theories, superstition and mythology 7 Non-terrestrial auroras 8 See also 9 Notes 10 References 11 Further reading 12 External links Occurrence of terrestrial auroras Most auroras occur in a band known as the auroral zone,[3] which is typically 3° to 6° wide in latitude and between 10° and 20° from the geomagnetic poles at all local times (or longitudes), most clearly seen at night against a dark sky. -
Feynman-Richard-P.Pdf
A Selected Bibliography of Publications by, and about, Richard Phillips Feynman Nelson H. F. Beebe University of Utah Department of Mathematics, 110 LCB 155 S 1400 E RM 233 Salt Lake City, UT 84112-0090 USA Tel: +1 801 581 5254 FAX: +1 801 581 4148 E-mail: [email protected], [email protected], [email protected] (Internet) WWW URL: http://www.math.utah.edu/~beebe/ 07 June 2021 Version 1.174 Title word cross-reference $14.95 [Oni15]. $15 [Ano54b]. $18.00 [Dys98]. $19.99 [Oni15]. 2 + 1 [Fey81, Fey82c]. $22.00 [Dys98]. $22.95 [Oni15]. $24.95 [Dys11a, RS12]. $26.00 [Bro06, Ryc17, Dys05]. $29.99 [Oni15, Roe12, Dys11a]. $30.00 [Kra08, Lep07, W¨ut07]. $35 [Ano03b]. $50.00 [DeV00, Ano99]. $500 [Ano39]. $55.00 [Noe11]. $80.00hb/$30.00pb [Cao06]. $9.95 [Oni15]. α [GN87, Sla72]. e [BC18]. E = mc2 [KN19]. F (t) · r [BS96]. λ [Fey53c, Fey53a]. SU(3) [Fey65a]. U(6) ⊗ U(6) [FGMZ64]. π [BC18]. r [EFK+62]. -Transition [Fey53a]. 0-19-853948-7 [Tay97]. 0-226-42266-6 [W¨ut07]. 0-226-42267-4 [Kra08]. 0-691-03327-7 [Bro96c]. 0-691-03685-3 [Bro96c]. 1965 [Fey64e]. 1988 [Meh02]. 1 2 2.0 [BCKT09]. 2002 [FRRZ04]. 2007 [JP08]. 2010 [KLR13]. 20th [Anoxx, Bre97, Gin01, Kai02]. 235 [FdHS56]. 3 [Ish19, Ryc17]. 3.0 [Sem09]. 3.2 [Sem16]. 40th [MKR87]. 469pp [Cao06]. 8 [Roe12]. 9 [BFB82]. 978 [Ish19, Roe12, Ryc17]. 978-0-06135-132-7 [Oni15]. 978-0-300-20998-3 [Ryc17]. 978-0-8090-9355-7 [Oni15]. 978-1-58834-352-9 [Oni15]. -
Maria Spiropulu; Other Dimensions? She's in Pursuit - New York Times 10/07/2007 01:26 AM
SCIENTIST AT WORK -- Maria Spiropulu; Other Dimensions? She's in Pursuit - New York Times 10/07/2007 01:26 AM September 30, 2003 SCIENTIST AT WORK -- Maria Spiropulu; Other Dimensions? She's in Pursuit By DENNIS OVERBYE Flap harder, urged the little girl with the stopwatch. One by one, the children stepped up and launched themselves off the garden wall, flapping homemade wings with their arms. Always with the same result. Crash. Only the girl herself, 7 years old, an aspiring dancer, astronaut, wing maker and free spirit, could not jump -- not out of fear or lack of confidence in the wings she had made, but because she could not time her own flight. ''And I didn't trust anybody to time it for me,'' she recalled. She already had the soul of a scientist, as well as a knack for leadership. Crash. Just before midnight on a recent summer night, the girl, Dr. Maria Spiropulu, now 33 and a physicist affiliated with the University of California at Santa Barbara, stepped outside a South Side Chicago jazz club and climbed into a cluttered Honda Civic. She was wearing black jeans, a black sleeveless top, Nikes and three rings on her left hand. Spewing noise from a leaky muffler, she drove into the Illinois prairie, through the gates of the Fermi National Accelerator Laboratory, or Fermilab, and past scattered farmhouses too white and neat to be real farmhouses anymore. Mars' bloody stare was high in a hazy sky by the time she parked outside a hulking shedlike building. Inside the shed, the ground floor rimmed a huge pit three stories deep and wide as a basketball court, littered with the toys of industrial strength science -- cranes, racks of electronics, tool chests, cables, long magnets stacked like redwood logs. -
High Energy Physics Quantum Information Science Awards Abstracts
High Energy Physics Quantum Information Science Awards Abstracts Towards Directional Detection of WIMP Dark Matter using Spectroscopy of Quantum Defects in Diamond Ronald Walsworth, David Phillips, and Alexander Sushkov Challenges and Opportunities in Noise‐Aware Implementations of Quantum Field Theories on Near‐Term Quantum Computing Hardware Raphael Pooser, Patrick Dreher, and Lex Kemper Quantum Sensors for Wide Band Axion Dark Matter Detection Peter S Barry, Andrew Sonnenschein, Clarence Chang, Jiansong Gao, Steve Kuhlmann, Noah Kurinsky, and Joel Ullom The Dark Matter Radio‐: A Quantum‐Enhanced Dark Matter Search Kent Irwin and Peter Graham Quantum Sensors for Light-field Dark Matter Searches Kent Irwin, Peter Graham, Alexander Sushkov, Dmitry Budke, and Derek Kimball The Geometry and Flow of Quantum Information: From Quantum Gravity to Quantum Technology Raphael Bousso1, Ehud Altman1, Ning Bao1, Patrick Hayden, Christopher Monroe, Yasunori Nomura1, Xiao‐Liang Qi, Monika Schleier‐Smith, Brian Swingle3, Norman Yao1, and Michael Zaletel Algebraic Approach Towards Quantum Information in Quantum Field Theory and Holography Daniel Harlow, Aram Harrow and Hong Liu Interplay of Quantum Information, Thermodynamics, and Gravity in the Early Universe Nishant Agarwal, Adolfo del Campo, Archana Kamal, and Sarah Shandera Quantum Computing for Neutrino‐nucleus Dynamics Joseph Carlson, Rajan Gupta, Andy C.N. Li, Gabriel Perdue, and Alessandro Roggero Quantum‐Enhanced Metrology with Trapped Ions for Fundamental Physics Salman Habib, Kaifeng Cui1, -
Interplanetary Magnetic Field Control of the Entry of Solar Energetic Particles Into the Magnetosphere R
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 107, NO. A8, 1184, 10.1029/2001JA000099, 2002 Interplanetary magnetic field control of the entry of solar energetic particles into the magnetosphere R. L. Richard, M. El-Alaoui, M. Ashour-Abdalla,1 and R. J. Walker2 Institute of Geophysics and Planetary Physics, University of California at Los Angeles, Los Angeles, California, USA Received 2 April 2001; revised 6 February 2002; accepted 18 March 2002; published 15 August 2002. [1] We have investigated the entry of energetic ions of solar origin into the magnetosphere as a function of the interplanetary magnetic field orientation. We have modeled this entry by following high energy particles (protons and 3He ions) ranging from 0.1 to 50 MeV in electric and magnetic fields from a global magnetohydrodynamic (MHD) model of the magnetosphere and its interaction with the solar wind. For the most part these particles entered the magnetosphere on or near open field lines except for some above 10 MeV that could enter directly by crossing field lines due to their large gyroradii. The MHD simulation was driven by a series of idealized solar wind and interplanetary magnetic field (IMF) conditions. It was found that the flux of particles in the magnetosphere and transport into the inner magnetosphere varied widely according to the IMF orientation for a constant upstream particle source, with the most efficient entry occurring under southward IMF conditions. The flux inside the magnetosphere could approach that in the solar wind implying that SEPs can contribute significantly to the magnetospheric energetic particle population during typical SEP events depending on the state of the magnetosphere. -
APS News, March 2018, Vol. 27, No. 3
March 2018 • Vol. 27, No. 3 A PUBLICATION OF THE AMERICAN PHYSICAL SOCIETY New Members of the PhysTEC 5+ Club APS.ORG/APSNEWS Page 3 2018 APS April Meeting: “Hello, Columbus” Physical Review B: Condensed Attendees in fields from Matter, Then and Now “Quarks to the Cosmos,” includ- ing particle physics, nuclear phys- ics, astrophysics, and gravitation, Getty Images will gather in Columbus, Ohio, April 14–17, at the Columbus Convention Center for the 2018 APS April Meeting. The meeting theme this year is “A Feynman Century,” marking the 100th By Sarma Kancharla and Laurens lished by APS offers a chance to anniversary of the Nobel-winning Molenkamp look back at some of the landmark physicist’s birth with a Kavli The late Peter Adams, found- publications that have led to PRB Foundation Plenary Session and ing editor of Physical Review B becoming not only the largest an invited session on his legacy. (PRB), impishly used to say that journal in all of physics but also a venue for excellence. The Kavli session will be held the journal was created in 1970 on Saturday, April 14 (8:30 a.m.) because The Physical Review and will feature a presentation by had reached its binding limit. Joan Feynman (Jet Propulsion Lab, Forum on the History of Physics Professional Skills Development Apocryphal as that sounds, the retired) on life with her brother invited session on Monday, April Workshop for Women on persua- birth of PRB couldn't have hap- Richard and her concerns about cli- 16 (room B130) at 1:30 p.m., with sive communication, negotiation, mate change. -
Causes of Extremely Fast Cmes
Solar Activity and its Magnetic Origin Proceedings IAU Symposium No. 233, 2006 c 2006 International Astronomical Union V. Bothmer & A. A. Hady, eds. doi:10.1017/S1743921306002146 Causes of extremely fast CMEs Joan Feynman and Alexander Ruzmaikin Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA email: [email protected] Abstract. We study CMEs observed by LASCO to have plane of the sky velocities exceeding 1500 km/sec. We find that these extremely fast CMEs are typically associated with flares ac- companied by erupting prominences. Our results are consistent with a single CME initiation process that consists of three stages. The initial stage is brought about by the emergence of new magnetic flux, which interacts with the pre-existing magnetic configuration and results in a slow rise of the magnetic structure. The second stage is a fast reconnection phase with flaring, filament eruption and a sudden increase of the rise velocity of the magnetic structure (CME). The third stage consists of propagation in the corona. We discuss the sources of these CMEs and the need for improved understanding of the first and third stages. Keywords. Sun:coronal mass ejections (CMEs), Sun: prominences, Sun: flares, Sun: magnetic fields 1. Introduction The distribution of the plane of the sky velocities of CMEs observed by SOHO is showninFigure1(Yurchyshynet al., 2005). This distribution of 4315 CMEs shows few CMEs with velocities greater than 1500 km/sec and none with velocities exceeding 2000 km/sec. However these are the CMEs that cause the most important solar energetic particle events and the most intense geomagnetic storms. -
Fall 2015 Newsletter the American Physical Society
APS Forum on International Physics Fall 2015 Newsletter page 1 The American Physical Society website: http://www.aps.org/units/fip Fall 2015 Newsletter Ernie Malamud, Editor Message from the Chair, Edmond Berger 2 Report from the APS International Affairs Office (INTAF), Amy Flatten 4 From the Editor, Ernie Malamud 7 APS SPRING MEETINGS Invited talks in FIP sponsored or co-sponsored sessions: 8 March 2 – 6, 2015, San Antonio April 11 – 14, 2015, Baltimore Photos FIP co-sponsored reception at the San Antonio meeting, from Ercan Esen Alp 9 FIP Executive Committee meeting at the Baltimore meeting, from Ercan Esen Alp 10 SAVE THE DATES ! March 14 – 18, 2016 April 16 - 19, 2016 Baltimore Salt Lake City ARTICLES SESAME Moves towards Commissioning, Chris Llewellyn-Smith 11 The São Paulo School of Advanced Sciences (ESPCA) on Recent Developments in Synchrotron Radiation, Harry Westfahl, Helio Tolentino and Esen Ercan Alp 14 Industrial Use of Japanese Synchrotron Radiation (SR) and the X-ray Free Electgron Laser (XFEL) Facilites, Tetsuya Ishikawa 15 Momentum gathers towards a Mexican Light Source, Armando Antillón, José Jimenéz and Matías Moreno 17 The Gulf Nuclear Energy Infrastructure Institute (GNEII), Amir Mohagheghi, Adam Williams, Phil Beeley, and Alex Solodov 20 The Radiation Measurements Cross Calibration (RMCC) Project, Amir Mohagheghi Al-Sharif Nasser Bin Nasser, and Matthew Sternat 22 Improvement in Education and Research through Recognition, a report from Bangladesh, Sultana Nahar 25 APS International Research Travel Award Program, IRTAP: Providing Support to International Collaborators, Michele Irwin 28 International Linear Collider Collaboration Status, Maria Spiropulu 30 NEW Distinguished Student Seminar Program 31 FIP Committees-2015 32 Disclaimer—The articles and opinion pieces found in this issue of the APS Forum on International Physics Newsletter are not peer refereed and represent solely the views of the authors and not necessarily the views of the APS. -
Edward P. Richards, the Lessons of Human Adaptation to Climate
RICHARDS - FINAL WORD (DO NOT DELETE) 11/30/2018 11:02 AM 18 Hous. J. Health L. & Pol’y 131 Copyright © 2018 Edward P. Richards Houston Journal of Health Law & Policy THE SOCIETAL IMPACTS OF CLIMATE ANOMALIES DURING THE PAST 50,000 YEARS AND THEIR IMPLICATIONS FOR SOLASTALGIA AND ADAPTATION TO FUTURE CLIMATE CHANGE1 Edward P. Richards INTRODUCTION................................................................................................ 132 I. PRE-SCIENTIFIC KNOWLEDGE OF THE NATURAL WORLD .......................... 134 II. UNDERSTANDING CLIMATE CHANGE AND CLIMATE ANOMALIES .......... 140 III. MEDIEVAL WARM PERIOD/MEDIEVAL CLIMATE ANOMALY IN THE AMERICAS ............................................................................................ 146 IV. IMPACT OF POST-LAST GLACIAL MAXIMUM SEA LEVEL RISE ................. 150 V. THE NEW THREAT: HEAT........................................................................... 154 VI. SENSE OF PLACE AND CLIMATE CHANGE DRIVEN MIGRATION ............. 158 VII. SOLASTALGIA AND FUTURE ENVIRONMENTAL RISK .............................. 164 CONCLUSION ................................................................................................... 167 1 This paper does not deal with mitigating global warming and ocean acidification through limiting carbon dioxide and other greenhouse gases. It also does not deal with potential con- sequences of ocean acidification. RICHARDS - FINAL WORD (DO NOT DELETE) 11/30/2018 11:02 AM 132 HOUS. J. HEALTH L. & POL’Y INTRODUCTION The earth is warming, local -
Early Prediction of Geomagnetic Storms (And Other Space Weather Hazards) Abstract Introduction
1 Early Prediction of GeomagneticStorms (andOther Space WeatherHazards) David H. Collins and Joan Feynman Jet Propulsion Laboratory, California Institute of Technology Abstract A detailed conceptual design has been developed for a mission and microspacecraft that can provide information needed to answer key questions about the physics of space weather and also both provide and validate a system for early warning of hazardous space weather. A single small launch vehicleand individually tailored Venus gravity assists disperse nine microspacecraft in a 0.53-0.85 AU band around the Sun. Collectively, the microspacecraft can investigate large-scale organization of coronal mass ejections (CMEs) andparticle acceleration mechanisms near their shocks. Radial and longitudinaldependencies, magnetohydrodynamic (MHD) turbulence in the solar wind, and variations in solar wind velocities and densities can allbe studied.Simultaneously, at least one of themicrospacecraft is nearthe Sun-Earthline almost continuously and can be monitored for earlywarning of hazardous space weather. Introduction In their paper, “On Space Weather Consequences and Predictions,” Feynman and Gabriel [2000]conclude that an important next step in thedevelopment of the understanding and prediction of hazardous space weather is to observe CMEs at 2 heliocentric distances significantly less than 1 AU and along the Sun-Earth line. These observations are needed to test interplanetary shock acceleration and release models for protons and ions with energies >10 MeV and to provide improved long- lead-time predictions of geomagnetic storms. High-velocity CMEs cause geomagnetic storms [Tsurutani and Gonzalez, 19971 and energetic particle events [Kahler et a/., 1984; Gosling, 19931 that present major hazards to both space systems and humans in space [Feynmanand Gabriel, 20001. -
Annual Report 2010 Supporting Only the Best, So That They Can Become Even Better
Foundation for Polish Science Annual Report 2010 Supporting only the best, so that they can become even better The programmes WELCOME, International PhD Projects (MPD), TEAM, VENTURES, HOMING PLUS and PARENT-BRIDGE are co-financed from the European Regional Development Fund within the Innovative Economy Operational Programme. annual report 2010 he Foundation for Polish Science is a non-governmental, apolitical, non-profit organization active T since 1991. Its mission is to support science in Poland. The Foundation fulfils its statutory role by financing individual projects of scientists and research teams, as well as initiatives serving Polish science. As the largest Polish non-budgetary source of funding scientific research, the Foundation also tries to propagate throughout society an understanding of the significance of science in the development of Poland. The Foundation presents individual awards, scholarships and research grants to the best scholars, while actively supporting international scientific cooperation and the development of initiatives that foster greater academic independence among young researchers. Beneficiaries of the Foundation’s programmes are selected through competitions. All the applications for competitions are assessed by way of the peer- -review system; the review body working with the Foundation comprises several thousand scientists from Poland and abroad, who are renowned specialists in their fields. The most important criterion for awarding financial support is the quality of the candidate’s scientific knowledge and achievements, in accordance with the Foundation’s guiding motto: Supporting only the best, so that they can become even better. The Foundation’s founding capital of 95 million zlotys originated from the Central Fund for the Development of Science and Technology, which was liquidated in 1990, whereupon the capital was directed to the FNP by a decision of the Polish parliament.