Probing Foundations of Quantum Mechanics: a Study Into Nonlocality and Quantum Gravity
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Emergence and Phenomenology in Quantum Gravity
Emergence and Phenomenology in Quantum Gravity by Isabeau Premont-Schwarz´ A thesis presented to the University of Waterloo in fulfillment of the thesis requirement for the degree of Doctor of Philosophy in Physics Waterloo, Ontario, Canada, 2010 © Isabeau Premont-Schwarz´ 2010 AUTHOR’S DECLARATION I hereby declare that I am the sole author of this thesis. This is a true copy of the thesis, including any required final revisions, as accepted by my examiners. I understand that my thesis may be made electronically available to the public. ii AUTHORSHIP STATEMENT This thesis is based on the following five articles: • A. Hamma, F. Markopoulou, I. Pr´emont-Schwarz and S. Severini, “Lieb-Robinson bounds and the speed of light from topological order,” Phys. Rev. Lett. 102 (2009) 017204 [arXiv:0808.2495 [quant-ph]]. • I. Pr´emont-Schwarz ,A. Hamma, I. Klich and F. Markopoulou, “Lieb-Robinson bounds for commutator-bounded operators ,” Phys. Rev. A 81, 040102(R) (2010) .[arXiv:0912.4544 [quant-ph]]. • I. Pr´emont-Schwarz and J. Hnybida, “Lieb-Robinson bounds with dependence on interaction strengths, ” [arXiv:1002.4190 [math-ph]]. • L. Modesto and I. Pr´emont-Schwarz, “Self-dual Black Holes in LQG: Theory and Phenomenology,” Phys. Rev. D 80, 064041 (2009) [arXiv:0905.3170 [hep-th]]. • S. Hossenfelder, L. Modesto and I. Pr´emont-Schwarz, “A model for non-singular black hole collapse and evaporation ,” Phys. Rev. D 81, 044036 (2010) [arXiv:0912.1823 [gr-qc]]. I did the majority of the work in the first article, but the project was initiated by Fotini Markopoulou-Kalamara and Alioscia Hamma and the manuscript was mostly written by Alioscia Hamma. -
Gnc 2021 Abstract Book
GNC 2021 ABSTRACT BOOK Contents GNC Posters ................................................................................................................................................... 7 Poster 01: A Software Defined Radio Galileo and GPS SW receiver for real-time on-board Navigation for space missions ................................................................................................................................................. 7 Poster 02: JUICE Navigation camera design .................................................................................................... 9 Poster 03: PRESENTATION AND PERFORMANCES OF MULTI-CONSTELLATION GNSS ORBITAL NAVIGATION LIBRARY BOLERO ........................................................................................................................................... 10 Poster 05: EROSS Project - GNC architecture design for autonomous robotic On-Orbit Servicing .............. 12 Poster 06: Performance assessment of a multispectral sensor for relative navigation ............................... 14 Poster 07: Validation of Astrix 1090A IMU for interplanetary and landing missions ................................... 16 Poster 08: High Performance Control System Architecture with an Output Regulation Theory-based Controller and Two-Stage Optimal Observer for the Fine Pointing of Large Scientific Satellites ................. 18 Poster 09: Development of High-Precision GPSR Applicable to GEO and GTO-to-GEO Transfer ................. 20 Poster 10: P4COM: ESA Pointing Error Engineering -
Sabine Hossenfelder on “The Case Against Beauty in Physics” Julia
Rationally Speaking #211: Sabine Hossenfelder on “The case against beauty in physics” Julia: Welcome to Rationally Speaking, the podcast where we explore the borderlands between reason and nonsense. I'm your host, Julia Galef, and I'm here with today's guest, Sabine Hossenfelder. Sabine is a theoretical physicist, focusing on quantum gravity. She's a research fellow at the Frankfurt Institute for Advanced Studies, and blogs at Back Reaction. She just published the book, "Lost in Math: How Beauty Leads Physics Astray." "Lost in Math” argues that physicists, in at least certain sub-fields, evaluate theories based heavily on aesthetics, like is this theory beautiful? Instead of simply, what does the evidence suggest is true? The book is full of interviews Sabine did with top physicists, where she tries to ask them: what's the justification for this? Why should we expect beauty to be a good guide to truth? And, spoiler alert, ultimately, she comes away rather unsatisfied with the answers. So, we're going to talk about "Lost in Math" and the case for and against beauty in physics. Sabine, welcome to the show. Sabine: Hello. Julia: So, probably best to start with: what do you mean by beauty, in this context? And is it closer to a kind of “beauty is in the eye of the beholder” thing, like, every physicist has their own sort of aesthetic sense? Or is more like there's a consensus among physicists about what constitutes a beautiful theory? Sabine: Interestingly enough, there's mostly consensus about it. Let me put ahead that I will not try to tell anyone what beauty means, I am just trying to summarize what physicists seem to mean when they speak of beauty, when they say “that theory is beautiful.” There are several ingredients to this sense of beauty. -
Advanced Virgo: Status of the Detector, Latest Results and Future Prospects
universe Review Advanced Virgo: Status of the Detector, Latest Results and Future Prospects Diego Bersanetti 1,* , Barbara Patricelli 2,3 , Ornella Juliana Piccinni 4 , Francesco Piergiovanni 5,6 , Francesco Salemi 7,8 and Valeria Sequino 9,10 1 INFN, Sezione di Genova, I-16146 Genova, Italy 2 European Gravitational Observatory (EGO), Cascina, I-56021 Pisa, Italy; [email protected] 3 INFN, Sezione di Pisa, I-56127 Pisa, Italy 4 INFN, Sezione di Roma, I-00185 Roma, Italy; [email protected] 5 Dipartimento di Scienze Pure e Applicate, Università di Urbino, I-61029 Urbino, Italy; [email protected] 6 INFN, Sezione di Firenze, I-50019 Sesto Fiorentino, Italy 7 Dipartimento di Fisica, Università di Trento, Povo, I-38123 Trento, Italy; [email protected] 8 INFN, TIFPA, Povo, I-38123 Trento, Italy 9 Dipartimento di Fisica “E. Pancini”, Università di Napoli “Federico II”, Complesso Universitario di Monte S. Angelo, I-80126 Napoli, Italy; [email protected] 10 INFN, Sezione di Napoli, Complesso Universitario di Monte S. Angelo, I-80126 Napoli, Italy * Correspondence: [email protected] Abstract: The Virgo detector, based at the EGO (European Gravitational Observatory) and located in Cascina (Pisa), played a significant role in the development of the gravitational-wave astronomy. From its first scientific run in 2007, the Virgo detector has constantly been upgraded over the years; since 2017, with the Advanced Virgo project, the detector reached a high sensitivity that allowed the detection of several classes of sources and to investigate new physics. This work reports the Citation: Bersanetti, D.; Patricelli, B.; main hardware upgrades of the detector and the main astrophysical results from the latest five years; Piccinni, O.J.; Piergiovanni, F.; future prospects for the Virgo detector are also presented. -
Benjamin J. Owen - Curriculum Vitae
BENJAMIN J. OWEN - CURRICULUM VITAE Contact information Mail: Texas Tech University Department of Physics & Astronomy Lubbock, TX 79409-1051, USA E-mail: [email protected] Phone: +1-806-834-0231 Fax: +1-806-742-1182 Education 1998 Ph.D. in Physics, California Institute of Technology Thesis title: Gravitational waves from compact objects Thesis advisor: Kip S. Thorne 1993 B.S. in Physics, magna cum laude, Sonoma State University (California) Minors: Astronomy, German Research advisors: Lynn R. Cominsky, Gordon G. Spear Academic positions Primary: 2015{ Professor of Physics & Astronomy Texas Tech University 2013{2015 Professor of Physics The Pennsylvania State University 2008{2013 Associate Professor of Physics The Pennsylvania State University 2002{2008 Assistant Professor of Physics The Pennsylvania State University 2000{2002 Research Associate University of Wisconsin-Milwaukee 1998{2000 Research Scholar Max Planck Institute for Gravitational Physics (Golm) Secondary: 2015{2018 Adjunct Professor The Pennsylvania State University 2012 (2 months) Visiting Scientist Max Planck Institute for Gravitational Physics (Hanover) 2010 (6 months) Visiting Associate LIGO Laboratory, California Institute of Technology 2009 (6 months) Visiting Scientist Max Planck Institute for Gravitational Physics (Hanover) Honors and awards 2017 Princess of Asturias Award for Technical and Scientific Research (with the LIGO Scientific Collaboration) 2017 Albert Einstein Medal (with the LIGO Scientific Collaboration) 2017 Bruno Rossi Prize for High Energy Astrophysics (with the LIGO Scientific Collaboration) 2017 Royal Astronomical Society Group Achievement Award (with the LIGO Scientific Collab- oration) 2016 Gruber Cosmology Prize (with the LIGO Scientific Collaboration) 2016 Special Breakthrough Prize in Fundamental Physics (with the LIGO Scientific Collabora- tion) 2013 Fellow of the American Physical Society 1998 Milton and Francis Clauser Prize for Ph.D. -
121012-AAS-221 Program-14-ALL, Page 253 @ Preflight
221ST MEETING OF THE AMERICAN ASTRONOMICAL SOCIETY 6-10 January 2013 LONG BEACH, CALIFORNIA Scientific sessions will be held at the: Long Beach Convention Center 300 E. Ocean Blvd. COUNCIL.......................... 2 Long Beach, CA 90802 AAS Paper Sorters EXHIBITORS..................... 4 Aubra Anthony ATTENDEE Alan Boss SERVICES.......................... 9 Blaise Canzian Joanna Corby SCHEDULE.....................12 Rupert Croft Shantanu Desai SATURDAY.....................28 Rick Fienberg Bernhard Fleck SUNDAY..........................30 Erika Grundstrom Nimish P. Hathi MONDAY........................37 Ann Hornschemeier Suzanne H. Jacoby TUESDAY........................98 Bethany Johns Sebastien Lepine WEDNESDAY.............. 158 Katharina Lodders Kevin Marvel THURSDAY.................. 213 Karen Masters Bryan Miller AUTHOR INDEX ........ 245 Nancy Morrison Judit Ries Michael Rutkowski Allyn Smith Joe Tenn Session Numbering Key 100’s Monday 200’s Tuesday 300’s Wednesday 400’s Thursday Sessions are numbered in the Program Book by day and time. Changes after 27 November 2012 are included only in the online program materials. 1 AAS Officers & Councilors Officers Councilors President (2012-2014) (2009-2012) David J. Helfand Quest Univ. Canada Edward F. Guinan Villanova Univ. [email protected] [email protected] PAST President (2012-2013) Patricia Knezek NOAO/WIYN Observatory Debra Elmegreen Vassar College [email protected] [email protected] Robert Mathieu Univ. of Wisconsin Vice President (2009-2015) [email protected] Paula Szkody University of Washington [email protected] (2011-2014) Bruce Balick Univ. of Washington Vice-President (2010-2013) [email protected] Nicholas B. Suntzeff Texas A&M Univ. suntzeff@aas.org Eileen D. Friel Boston Univ. [email protected] Vice President (2011-2014) Edward B. Churchwell Univ. of Wisconsin Angela Speck Univ. of Missouri [email protected] [email protected] Treasurer (2011-2014) (2012-2015) Hervey (Peter) Stockman STScI Nancy S. -
A Natural Introduction to Fine-Tuning
A Natural Introduction to Fine-Tuning Julian De Vuyst ∗ Department of Physics & Astronomy, Ghent University, Krijgslaan, S9, 9000 Ghent, Belgium Abstract A well-known topic within the philosophy of physics is the problem of fine-tuning: the fact that the universal constants seem to take non-arbitrary values in order for live to thrive in our Universe. In this paper we will talk about this problem in general, giving some examples from physics. We will review some solutions like the design argument, logical probability, cosmological natural selection, etc. Moreover, we will also discuss why it's dangerous to uphold the Principle of Naturalness as a scientific principle. After going through this paper, the reader should have a general idea what this problem exactly entails whenever it is mentioned in other sources and we recommend the reader to think critically about these concepts. arXiv:2012.05617v1 [physics.hist-ph] 10 Dec 2020 ∗[email protected] 1 Contents 1 Introduction3 2 A Take on Constants3 2.I The Role of Units . .4 2.II Derived vs Fundamental Constants . .5 3 The Concept of Naturalness6 3.I Technical Naturalness . .6 3.I.a A Wilsonian Perspective . .6 3.I.b A Brief History . .8 3.II Numerical/General Naturalness . .9 4 The Fine-Tuning Problem9 5 Some Examples from Physics 10 5.I The Cosmological Constant Problem . 10 5.II The Flatness Problem . 11 5.III The Higgs Mass . 12 5.IV The Strong CP Problem . 13 6 Resolutions to Fine-Tuning 14 6.I We are here, full stop . 14 6.II Designed like Clockwork . -
Massimo Cerdonio, University of Padua
The gravitational waves network within a global network of observatories Massimo Cerdonio INFN Section & Physics Department, Padova, Italy · ground based gw detectors in the 2010s: efforts in US, Eu, Japan, Brasil (+ Au and Cina) · LISA and beyond · the need for networking gw detectors: sky, frequency and time coverage false alarms and confident detections direction & polarization of incoming gw · violent events in the cosmos involving matter at extreme densities: a gw observatory within an international network for multimessenger searches · imagining gw as one of the astronomies in 2025 (assuming 2010s expectations fulfilled) AURIGA Massimo Cerdonio www.auriga.lnl.infn.it Penn 10/29/04 goals trends needs · optimize performance of gw observatory >>> broaden the geographical distribution of the detectors, upgrade detectors to second (and third) generation, coordinate their on/off · evolve from initial detections to steady observations >>> optimize directed searches: gw an astronomical tool · solicit input from theory >>> accurate waveforms from numerical relativity to enhance SNR · roadmap to second generation detectors LIGO adv-NSF, VIRGO adv-CNRS/INFN, GEO · proposals for additional detectors Europe-EGO/ApPEC/ILIAS, Australia, Cina · seeds for third generation detectors LSC-NSF, EGO-CNRS/INFN/MPG/PPARC · studies on networking GWIC, ILIAS · coordination and collaboration between agencies worldwide to enhance and optimize trends AURIGA Massimo Cerdonio www.auriga.lnl.infn.it Penn 10/29/04 about “the role…” (after all these considerations) -
The Status of Gravitational-Wave Detectors Different Frequency
The Status of Gravitational Wave Detectors The Status of Gravitational-Wave Detectors Reported on behalf of LIGO colleagues by Fred Raab, LIGO Hanford Observatory LIGO-G030249-02-W Different Frequency Bands of Detectors and Sources space terrestrial ● EM waves are studied over ~20 Audio band orders of magnitude » (ULF radio −> HE γ rays) ● Gravitational Wave coverage over ~8 orders of magnitude » (terrestrial + space) LIGO-G030249-02-W LIGO Detector Commissioning 2 Fred Raab, Caltech & LIGO (KITP Gravitation Conference 5/12/03) 1 The Status of Gravitational Wave Detectors Basic Signature of Gravitational Waves for All Detectors LIGO-G030249-02-W LIGO Detector Commissioning 3 Original Terrestrial Detectors Continue to be Improved AURIGA II Resonant Bar Detector 1E-20 AURIGA I run LHe4 vessel Al2081 AURIGA II run Cryo ] 2 / 1 holder - Electronics z 1E-21 H [ 2 / 1 wiring hh support S AURIGA II run UltraCryo 1E-22 Main 850 860 880 900 920 940 950 Frequency [Hz] Attenuator Thermal Sensitive bar Shield •Efforts to broaden frequency range and reduce noise Compression •Size limited by sound speed Spring Transducer Courtesy M. Cerdonnio LIGO-G030249-02-W LIGO Detector Commissioning 4 Fred Raab, Caltech & LIGO (KITP Gravitation Conference 5/12/03) 2 The Status of Gravitational Wave Detectors New Generation of “Free- Mass” Detectors Now Online suspended mirrors mark inertial frames antisymmetric port carries GW signal Symmetric port carries common-mode info Intrinsically broad band and size-limited by speed of light. LIGO-G030249-02-W LIGO Detector -
Members Elect Barry Barish As Next APS Vice-President
October 2008 Volume 17, No. 9 www.aps.org/publications/apsnews 21st Century Campaign Nears Goal APS NEWS and Needs Your Support! A PublicAtion of the AmericAn PhysicAl society • www.APs.org/PublicAtions/APsnews (See insert) Energy Efficiency Crucial to Achieving Energy Security Members Elect Barry Barish and Reducing Global Warming, States APS Report as next APS Vice-President Tapping wasted energy from miles per gallon mileage for cars needs because they require sig- APS members have elected in physics from the University of inefficient automobiles, homes and and other light-duty vehicles by nificant scientific and engineering Barry Barish, Linde Professor of California, Berkeley. He joined businesses is equivalent to discov- 2030 and the elimination of energy breakthroughs in several critical Physics Emeritus at Caltech, as the faculty at Caltech in 1963. ering a hidden energy reserve that from fossil fuels in new residential areas. the Society’s next vice president. Among his noteworthy experi- will help the United States improve buildings by 2020. The study also calls on Congress Barish will assume the office in ments were those performed at its energy security and reduce glob- and the White House to increase January 2009. At the same time, Fermilab using high-energy neu- al warming, an APS study panel has spending on research and develop- Curtis Callan of trino collisions to concluded. ment of next-generation building Princeton Univer- reveal the quark Their report, Energy Future: technologies, training scientists sity will become substructure of Think Efficiency, states that the key who work on building technologies president-elect, and the nucleon. -
Quantized Vortices in Superfluid Dark Matter
Quantized Vortices in Superfluid Dark Matter Renate Mauland Master’s Thesis, Spring 2019 ii Copyright c 2019, Renate Mauland This work, entitled “Quantized Vortices in Superfluid Dark Matter” is distributed under the terms of the Public Library of Science Open Access License, a copy of which can be found at https://journals.plos.org/plosone/s/licenses-and-copyright. Cover Photo: Open Source Image from www.pexels.com. Abstract In a recent paper by Berezhiani and Khoury [1], a superfluid dark matter (DM) model was presented. The model consists of light axion-like DM particles (m ∼ eV), which condense and form a superfluid at galactic scales. The superfluid exhibits collective excitations known as phonons, which interact with baryons and mediate a force similar to that of Modified Newtonian Dynamics (MOND). The superfluid DM model therefore combines the success of MOND at small scales with that of the ΛCDM model at large scales. By analogy with superfluids studied in the lab, we expect a grid of vortices with quantized circulation to form in a rotating galaxy containing superfluid DM. In this thesis, we explore the properties of the superfluid DM vortices and their impact on the surroundings. We find that the vortex cores are small, 10−4 − 10−3 m, and that the vortices are separated by vast distances, ∼ 0:002 AU. The viable parameter space of the model is found to be substantial, and a reduction in the DM particle mass results in larger vortices with a higher energy. Yet, no combination of parameters explored here give vortices energetic enough to have a noticeable effect on the galaxy as a whole. -
Gravitational Waves from Neutron Stars: a Review
Publications of the Astronomical Society of Australia (PASA), Vol. 32, e034, 11 pages (2015). C Astronomical Society of Australia 2015; published by Cambridge University Press. doi:10.1017/pasa.2015.35 Gravitational Waves from Neutron Stars: A Review Paul D. Lasky Monash Centre for Astrophysics, School of Physics and Astronomy, Monash University, VIC 3800, Australia Email: [email protected] (Received August 20, 2015; Accepted August 26, 2015) Abstract Neutron stars are excellent emitters of gravitational waves. Squeezing matter beyond nuclear densities invites exotic physical processes, many of which violently transfer large amounts of mass at relativistic velocities, disrupting spacetime and generating copious quantities of gravitational radiation. I review mechanisms for generating gravitational waves with neutron stars. This includes gravitational waves from radio and millisecond pulsars, magnetars, accreting systems, and newly born neutron stars, with mechanisms including magnetic and thermoelastic deformations, various stellar oscillation modes, and core superfluid turbulence. I also focus on what physics can be learnt from a gravitational wave detection, and where additional research is required to fully understand the dominant physical processes at play. Keywords: gravitational waves – stars: neutron 1 INTRODUCTION during inflation. Continuous gravitational waves are almost monochromatic signals generated typically by rotating, non- The dawn of gravitational wave astronomy is one of the most axisymmetric neutron stars. anticipated scientific advances of the coming decade. The The above laundry list of gravitational wave sources second generation, ground-based gravitational wave interfer- prominently features neutron stars in their many guises. ometers, Advanced Laser Interferometer Gravitational-wave While supranuclear densities, relativistic velocities, and Observatory (aLIGO Aasi et al.