Edward P. Richards, the Lessons of Human Adaptation to Climate
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Apocalypse Now? Initial Lessons from the Covid-19 Pandemic for the Governance of Existential and Global Catastrophic Risks
journal of international humanitarian legal studies 11 (2020) 295-310 brill.com/ihls Apocalypse Now? Initial Lessons from the Covid-19 Pandemic for the Governance of Existential and Global Catastrophic Risks Hin-Yan Liu, Kristian Lauta and Matthijs Maas Faculty of Law, University of Copenhagen, Copenhagen, Denmark [email protected]; [email protected]; [email protected] Abstract This paper explores the ongoing Covid-19 pandemic through the framework of exis- tential risks – a class of extreme risks that threaten the entire future of humanity. In doing so, we tease out three lessons: (1) possible reasons underlying the limits and shortfalls of international law, international institutions and other actors which Covid-19 has revealed, and what they reveal about the resilience or fragility of institu- tional frameworks in the face of existential risks; (2) using Covid-19 to test and refine our prior ‘Boring Apocalypses’ model for understanding the interplay of hazards, vul- nerabilities and exposures in facilitating a particular disaster, or magnifying its effects; and (3) to extrapolate some possible futures for existential risk scholarship and governance. Keywords Covid-19 – pandemics – existential risks – global catastrophic risks – boring apocalypses 1 Introduction: Our First ‘Brush’ with Existential Risk? All too suddenly, yesterday’s ‘impossibilities’ have turned into today’s ‘condi- tions’. The impossible has already happened, and quickly. The impact of the Covid-19 pandemic, both directly and as manifested through the far-reaching global societal responses to it, signal a jarring departure away from even the © koninklijke brill nv, leiden, 2020 | doi:10.1163/18781527-01102004Downloaded from Brill.com09/27/2021 12:13:00AM via free access <UN> 296 Liu, Lauta and Maas recent past, and suggest that our futures will be profoundly different in its af- termath. -
UC Santa Barbara Other Recent Work
UC Santa Barbara Other Recent Work Title Geopolitics, History, and International Relations Permalink https://escholarship.org/uc/item/29z457nf Author Robinson, William I. Publication Date 2009 Peer reviewed eScholarship.org Powered by the California Digital Library University of California OFFICIAL JOURNAL OF THE CONTEMPORARY SCIENCE ASSOCIATION • NEW YORK Geopolitics, History, and International Relations VOLUME 1(2) • 2009 ADDLETON ACADEMIC PUBLISHERS • NEW YORK Geopolitics, History, and International Relations 1(2) 2009 An international peer-reviewed academic journal Copyright © 2009 by the Contemporary Science Association, New York Geopolitics, History, and International Relations seeks to explore the theoretical implications of contemporary geopolitics with particular reference to territorial problems and issues of state sovereignty, and publishes papers on contemporary world politics and the global political economy from a variety of methodologies and approaches. Interdisciplinary and wide-ranging in scope, Geopolitics, History, and International Relations also provides a forum for discussion on the latest developments in the theory of international relations and aims to promote an understanding of the breadth, depth and policy relevance of international history. Its purpose is to stimulate and disseminate theory-aware research and scholarship in international relations throughout the international academic community. Geopolitics, History, and International Relations offers important original contributions by outstanding scholars and has the potential to become one of the leading journals in the field, embracing all aspects of the history of relations between states and societies. Journal ranking: A on a seven-point scale (A+, A, B+, B, C+, C, D). Geopolitics, History, and International Relations is published twice a year by Addleton Academic Publishers, 30-18 50th Street, Woodside, New York, 11377. -
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. -
The Most Extreme Risks: Global Catastrophes Seth D
The Most Extreme Risks: Global Catastrophes Seth D. Baum and Anthony M. Barrett Global Catastrophic Risk Institute http://sethbaum.com * http://tony-barrett.com * http://gcrinstitute.org In Vicki Bier (editor), The Gower Handbook of Extreme Risk. Farnham, UK: Gower, forthcoming. This version 5 February 2015. Abstract The most extreme risk are those that threaten the entirety of human civilization, known as global catastrophic risks. The very extreme nature of global catastrophes makes them both challenging to analyze and important to address. They are challenging to analyze because they are largely unprecedented and because they involve the entire global human system. They are important to address because they threaten everyone around the world and future generations. Global catastrophic risks also pose some deep dilemmas. One dilemma occurs when actions to reduce global catastrophic risk could harm society in other ways, as in the case of geoengineering to reduce catastrophic climate change risk. Another dilemma occurs when reducing one global catastrophic risk could increase another, as in the case of nuclear power reducing climate change risk while increasing risks from nuclear weapons. The complex, interrelated nature of global catastrophic risk suggests a research agenda in which the full space of risks are assessed in an integrated fashion in consideration of the deep dilemmas and other challenges they pose. Such an agenda can help identify the best ways to manage these most extreme risks and keep human civilization safe. 1. Introduction The most extreme type of risk is the risk of a global catastrophe causing permanent worldwide destruction to human civilization. In the most extreme cases, human extinction could occur. -
Catastrophe, Social Collapse, and Human Extinction
Catastrophe, Social Collapse, and Human Extinction Robin Hanson∗ Department of Economics George Mason University† August 2007 Abstract Humans have slowly built more productive societies by slowly acquiring various kinds of capital, and by carefully matching them to each other. Because disruptions can disturb this careful matching, and discourage social coordination, large disruptions can cause a “social collapse,” i.e., a reduction in productivity out of proportion to the disruption. For many types of disasters, severity seems to follow a power law distribution. For some of types, such as wars and earthquakes, most of the expected harm is predicted to occur in extreme events, which kill most people on Earth. So if we are willing to worry about any war or earthquake, we should worry especially about extreme versions. If individuals varied little in their resistance to such disruptions, events a little stronger than extreme ones would eliminate humanity, and our only hope would be to prevent such events. If individuals vary a lot in their resistance, however, then it may pay to increase the variance in such resistance, such as by creating special sanctuaries from which the few remaining humans could rebuild society. Introduction “Modern society is a bicycle, with economic growth being the forward momentum that keeps the wheels spinning. As long as the wheels of a bicycle are spinning rapidly, it is a very stable vehicle indeed. But, [Friedman] argues, when the wheels stop - even as the result of economic stagnation, rather than a downturn or a depression - political democracy, individual liberty, and social tolerance are then greatly at risk even in countries where the absolute level of material prosperity remains high....” (DeLong, 2006) ∗For their comments I thank Jason Matheny, the editors, and an anonymous referee. -
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]. -
Double Catastrophe: Intermittent Stratospheric Geoengineering Induced by Societal Collapse
Double Catastrophe: Intermittent Stratospheric Geoengineering Induced By Societal Collapse Seth D. Baum1,2,3,4,*, Timothy M. Maher, Jr.1,5, and Jacob Haqq-Misra1,4 1. Global Catastrophic Risk Institute 2. Department of Geography, Pennsylvania State University 3. Center for Research on Environmental Decisions, Columbia University 4. Blue Marble Space Institute of Science 5. Center for Environmental Policy, Bard College * Corresponding author. [email protected] Environment, Systems and Decisions 33(1):168-180. This version: 23 March 2013 Abstract Perceived failure to reduce greenhouse gas emissions has prompted interest in avoiding the harms of climate change via geoengineering, that is, the intentional manipulation of Earth system processes. Perhaps the most promising geoengineering technique is stratospheric aerosol injection (SAI), which reflects incoming solar radiation, thereby lowering surface temperatures. This paper analyzes a scenario in which SAI brings great harm on its own. The scenario is based on the issue of SAI intermittency, in which aerosol injection is halted, sending temperatures rapidly back toward where they would have been without SAI. The rapid temperature increase could be quite damaging, which in turn creates a strong incentive to avoid intermittency. In the scenario, a catastrophic societal collapse eliminates society’s ability to continue SAI, despite the incentive. The collapse could be caused by a pandemic, nuclear war, or other global catastrophe. The ensuing intermittency hits a population that is already vulnerable from the initial collapse, making for a double catastrophe. While the outcomes of the double catastrophe are difficult to predict, plausible worst-case scenarios include human extinction. The decision to implement SAI is found to depend on whether global catastrophe is more likely from double catastrophe or from climate change alone. -
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. -
Overpopulation Is Not the Problem - Nytimes.Com Page 1 of 3
Overpopulation Is Not the Problem - NYTimes.com Page 1 of 3 September 13, 2013 Overpopulation Is Not the Problem By ERLE C. ELLIS BALTIMORE — MANY scientists believe that by transforming the earth’s natural landscapes, we are undermining the very life support systems that sustain us. Like bacteria in a petri dish, our exploding numbers are reaching the limits of a finite planet, with dire consequences. Disaster looms as humans exceed the earth’s natural carrying capacity. Clearly, this could not be sustainable. This is nonsense. Even today, I hear some of my scientific colleagues repeat these and similar claims — often unchallenged. And once, I too believed them. Yet these claims demonstrate a profound misunderstanding of the ecology of human systems. The conditions that sustain humanity are not natural and never have been. Since prehistory, human populations have used technologies and engineered ecosystems to sustain populations well beyond the capabilities of unaltered “natural” ecosystems. The evidence from archaeology is clear. Our predecessors in the genus Homo used social hunting strategies and tools of stone and fire to extract more sustenance from landscapes than would otherwise be possible. And, of course, Homo sapiens went much further, learning over generations, once their preferred big game became rare or extinct, to make use of a far broader spectrum of species. They did this by extracting more nutrients from these species by cooking and grinding them, by propagating the most useful species and by burning woodlands to enhance hunting and foraging success. Even before the last ice age had ended, thousands of years before agriculture, hunter- gatherer societies were well established across the earth and depended increasingly on sophisticated technological strategies to sustain growing populations in landscapes long ago transformed by their ancestors. -
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.