Gravitational waves from neutron stars binaries: accuracy and tidal effects in the late inspiral S. Bernuzzi TPI-PAF FSU Jena / SFB-TR7
|
|
- Maximillian Boone
- 8 years ago
- Views:
Transcription
1 Gravitational waves from neutron stars binaries: accuracy and tidal effects in the late inspiral S. Bernuzzi TPI-PAF FSU Jena / SFB-TR7 M. Thierfelder, SB, & B.Bruegmann, PRD (2011) SB, MT, & BB arxiv: [gr-qc] (2011) R.Gold, SB, MT, BB, & F.Pretorius arxiv: [gr-qc] (2011) N.Johnson-McDaniel, SB, MT, & BB In Prep. (2012)
2 Motivations Binary neutron stars (BNSs) exist and are among the most promising sources of gravitational waves (GWs) BNS simulations: a complex problem (~ supernovae) necessary to select what physics to simulate! Last orbits + merger tidal interactions, significant finite size effects star parameters (radius, Love #) EoS from GWs measure*! Nonlinear regime numerical relativity (NR) evolutions required! Mostly evolutions of quasi-circular initial data Started a data analysis / analytic methods comparison* *Read et al PRD (2009) *Baiotti et al PRL (2010), PRD (2011)
3 Questions Circular mergers: How large are tidal effect during the last inspiral - merger phase? Small effects Can we extract this info reliably? How accurate are the simulations? * Eccentric mergers: Are there other tidal signatures? # Are astrophysically relevant? * Miller PRD (2005), Lindblom et al. PRD (2008) # Turner ApJ (1977), Lee et al ApJ (2010)
4 Full GR Framework Free evolutions 3+1 NR Einstein: BSSNOK Moving puncture gauge Psi4 GW extraction ideal GRHD No magnetic fields - polytropic/ideal fluid EoS microphysics BAMmatter code 3D Cartesian nested grids with moving boxes technique MoL with Runge-Kutta schemes and Berger-Oliger Metric: high-order finite differencing (centered +lop-sided) Matter: HRSC scheme
5 Quasi - circular mergers SB, MT, & BB arxiv: [gr-qc] (2011) M. Thierfelder, SB, & B.Bruegmann, PRD (2011) Initial data: equal masses, circularized, conformally flat, and irrotational (Lorene, Taniguchi & Gourgoulhon PRD ) Performed ~ 3 orbits and ~ 9 orbits (longest so far!) simulations Investigated truncation errors and finite extraction effects, and systematic source of uncertainties; quantified the former and assigned errorbars (inspiral only!) Checked waveforms against accuracy standard for detection (first time!) Preliminary comparison with post-newtonian approximants
6 Dynamics and GWs
7 Dynamics and GWs
8 Handling singularity formation puncture gauge PRD (2011) t/m t α = β i i α 2α ˆK t β k = Γ k ηβ k + β j j β k r/m Brandt & Bruegmann PRL (1997) Baker et al PRL (2006) Campanelli et al PRL (2006) Hannam et al PRL (2007) Brown PRD (2008)
9 Waveform uncertainties Self-convergence: 2nd order (do not shift!) up to contact (9 orbits) Extrapolation of waveform in resolution (several runs) best case: rad and ~ 0.2 % (contact) Finite radius extraction must be taken into account! Absolute error estimate (upper bound) contact merger
10 Accuracy standards { I 2 = δh w ε/ϱ faithful < h x w 2εM effectual { faithful ϱ 8, ε =0.5, ε M = effectual Miller PRD (2005), Lindblom et al. PRD (2008)
11 Accuracy standards { I 2 = δh w ε/ϱ faithful < h x w 2εM effectual { faithful ϱ 8, ε =0.5, ε M = effectual Miller PRD (2005), Lindblom et al. PRD (2008)
12 Accuracy standards { I 2 = δh w ε/ϱ faithful < h x w 2εM effectual { faithful ϱ 8, ε =0.5, ε M = effectual REM not necessarily the optimal error estimate for DA, but upper bound... Miller PRD (2005), Lindblom et al. PRD (2008)
13 NR Vs PN waveforms T4pp: T4 3.5PN waveform pointparticle, T4td: T4 3.5PN waveform + NLO tidal contribute* ~3 rad Time domain comparison Assume PN valid... Align waves dependency on matching interval are significant significant tidal effects > NLO *Hinderer et al PRD (2010) Vines & Flanagan arxiv: [gr-qc] (2010) Vines et al PRD (2011) Damour & Nagar PRD (2010) ~1.5 rad
14 Systematic uncertainties Effect of different grid configurations, Berger-Oliger Numerical viscosity of the HRSC scheme Gauge effects on numerically extracted waves Spurious thermal effect during inspiral... They all potentially contribute (~same order of magnitude), slowly improve with resolution - larger grids ( 2nd or 1/r converging behaviour), only partially under control! M. Thierfelder, SB, & B.Bruegmann, PRD (2011) L.Baiotti, B.Giacomazzo, & L.Rezzolla, CQG (2008)
15 Highly eccentric mergers R.Gold, SB, MT, BB, & F.Pretorius arxiv: [gr-qc] (2011) Initial data: superposition of two boosted spherical configurations (constraint violating), 50M separation, boost parameter ξ. Equal masses, non-conformally flat, approximately irrotational Performed several simulations varying the initial boost ξ [0.01,0.07] Characterization of orbital dynamics and waves as function of ξ Disk mass in the remnant as function of ξ Relevance for detectability, SNR, accuracy and astrophysical population Role of mass ratio
16 Orbital dynamics /1 Model 1 ξ = 0.01 Model 2 ξ = 0.02 Model 3 ξ = 0.022
17 Orbital dynamics /1 Model 1 ξ = 0.01 Model 2 ξ = 0.02 Model 3 ξ = 0.022
18 Orbital dynamics /2 Orbital dynamics (as ξ increases) : direct plunge 2 encounters + merger multipole encounters (with precession) circular Radial oscillations (trigger by spurious effects?) Non-radial oscillations excited during encounters Model ~ 2: mass exchange during encounter Model ~ 2: massive disk ~ 10% M0(0)
19 Orbital dynamics /2 Orbital dynamics (as ξ increases) : direct plunge 2 encounters + merger multipole encounters (with precession) circular Radial oscillations (trigger by spurious effects?) Non-radial oscillations excited during encounters Model ~ 2: mass generic exchange for several during encounter models! Model ~ 2: massive disk ~ 10% M0(0)
20 Waveforms bursts encounters oscillations compatible with f-mode frequency
21 Mode analysis Spherical harmonics projections ρ lm = d 3 xy lmρ Main modes excited: (2,2), (2,0) f-mode frequency (2,0) strongly modulated by encounters frequency Upper limit on star rotation
22 Conclusions /1 GWs from NR quasi-circular mergers 2nd order convergent up to merger (3 orbits simulations) or up to contact (9 orbits simulations) Estimated uncertainties the waveforms may be used for some quantitative analysis, but extensive error analysis of the numerical data is imperative in every case! Impact on data analysis? Post-Newtonian comparison significant dephasing due to tidal effects contribute during the last 9 orbits Several systematic uncertainties: more work required to obtain accurate waveforms
23 Conclusions /2 GWs from eccentric mergers present burst-like structures (encounters) and can contain the star modes signature, as indicated by some Newtonian analysis e.g. Turner (1970), Lee et al (2010) The first set of NR simulations of highly eccentric binaries confirms qualitatively these characteristics In particular a strong f-mode (l=2) signature is produced quite generically for several eccentricity values, and can persist for several encounters (> 6) More work is ongoing about the impact of these results for the third generation of detectors, role of masses, accretion disks, and on possible dynamical instabilities
Orbital Dynamics of Eccentric Compact Binaries
Orbital Dynamics of Eccentric Compact Binaries Laboratoire Univers et Théories Observatoire de Paris / CNRS Collaborators: S. Akcay, L. Barack, N. Sago, N. Warburton Phys. Rev. D 91 124014 (2015), arxiv:1503.01374
More informationGravitational waves from compact object binaries
Gravitational waves from compact object binaries Laboratoire Univers et Théories Observatoire de Paris / CNRS aligo, avirgo, KAGRA, elisa, ( DECIGO, ET,... ( Main sources of gravitational waves (GW) elisa
More informationComplete gravitational waveforms from black-hole binaries with non-precessing spins
Complete gravitational waveforms from black-hole binaries with non-precessing spins P. Ajith LIGO Lab & Theoretical Astrophysics - Caltech / AEI Hannover In collaboration with M. Hannam, S. Husa, B. Bruegmann,
More informationGravitational self-force in the ultra-relativistic regime Chad Galley, California Institute of Technology
Gravitational self-force in the ultra-relativistic regime Chad Galley, California Institute of Technology with Rafael Porto (IAS) arxiv: 1302.4486 v2 soon! (with details) Capra16; Dublin, Ireland; July
More informationRadiation reaction for inspiralling binary systems with spin-spin
Radiation reaction for inspiralling binary systems with spin-spin coupling 1 Institute of Theoretical Physics, Friedrich-Schiller-University Jena December 3, 2007 1 H. Wang and C. M. Will, Phys. Rev. D,
More informationBinary Orbital Dynamics from the Analysis of Spherical Harmonic Modes of Gravitational Waves
Intro Motivations Binary Orbital Dynamics from the Analysis of Spherical Harmonic Modes of Gravitational Waves Dr. Jennifer Seiler (NASA GSFC) Gravity Theory Seminars University of Maryland College Park
More informationStructure formation in modified gravity models
Structure formation in modified gravity models Kazuya Koyama Institute of Cosmology and Gravitation University of Portsmouth Dark energy v modified gravity Is cosmology probing the breakdown of general
More informationX-ray observations and nuclear physics of GW-driven r-modes
X-ray observations and nuclear physics of GW-driven r-modes Wynn Ho University of Southampton, UK Nils Andersson Ian Jones University of Southampton, UK Nathalie Degenaar University of Michigan, USA Bryn
More informationNeutron Stars. How were neutron stars discovered? The first neutron star was discovered by 24-year-old graduate student Jocelyn Bell in 1967.
Neutron Stars How were neutron stars discovered? The first neutron star was discovered by 24-year-old graduate student Jocelyn Bell in 1967. Using a radio telescope she noticed regular pulses of radio
More informationMass transfer dynamics in white dwarf binary systems
Mass transfer dynamics in white dwarf binary systems In collaboration with: Stephan Rosswog & Marcus Brüggen EUROWD10, Tübingen, 2010 Numbers on Galactic WDs total number of WDs: 10 10 Napiwotzki (2009)
More information= = GM. v 1 = Ωa 1 sin i.
1 Binary Stars Consider a binary composed of two stars of masses M 1 and We define M = M 1 + and µ = M 1 /M If a 1 and a 2 are the mean distances of the stars from the center of mass, then M 1 a 1 = a
More informationResonant Orbital Dynamics in Extrasolar Planetary Systems and the Pluto Satellite System. Man Hoi Lee (UCSB)
Resonant Orbital Dynamics in Extrasolar Planetary Systems and the Pluto Satellite System Man Hoi Lee (UCSB) Introduction: Extrasolar Planetary Systems Extrasolar planet searches have yielded ~ 150 planetary
More informationGravitomagnetism and complex orbit dynamics of spinning compact objects around a massive black hole
Gravitomagnetism and complex orbit dynamics of spinning compact objects around a massive black hole Kinwah Wu Mullard Space Science Laboratory University College London United Kingdom kw@mssl.ucl.ac.uk
More informationExtra-solar massive planets with small semi-major axes?
Monografías de la Real Academia de Ciencias de Zaragoza. 25: 115 120, (2004). Extra-solar massive planets with small semi-major axes? S. Fernández, D. Giuliodori and M. A. Nicotra Observatorio Astronómico.
More informationTesting dark matter halos using rotation curves and lensing
Testing dark matter halos using rotation curves and lensing Darío Núñez Instituto de Ciencias Nucleares, UNAM Instituto Avanzado de Cosmología A. González, J. Cervantes, T. Matos Observational evidences
More informationPablo Laguna Center for Relativistic Astrophysics School of Physics Georgia Tech, Atlanta, USA
Pablo Laguna Center for Relativistic Astrophysics School of Physics Georgia Tech, Atlanta, USA The Transient Sky SN, GRBs, AGN or TDEs? Arcavi et al. 2014, ApJ, 793, 38 van Velzen et al. 2011, ApJ, 741,
More informationWhat Can We Learn From Simulations of Tilted Black Hole Accretion Disks?
What Can We Learn From Simulations of Tilted Black Hole? Dr. P. Chris Fragile College of Charleston, SC Collaborators: Omer Blaes (UCSB), Ken Henisey (UCSB), Bárbara Ferreira (Cambridge), Chris Done (Durham),
More informationLecture 2. Gravitational Waves from Binary Systems: Probes of the Universe. Historical importance of orbiting systems.
Gravitational Waves Notes for Lectures at the Azores School on Observational Cosmology September 2011 B F Schutz Albert Einstein Institute (AEI), Potsdam, Germany http://www.aei.mpg.de, Bernard.Schutz@aei.mpg.de
More informationNeutron stars as laboratories for exotic physics
Ian Jones Neutron stars as laboratories for exotic physics 1/20 Neutron stars as laboratories for exotic physics Ian Jones D.I.Jones@soton.ac.uk General Relativity Group, Southampton University Context
More informationLIGO SCIENTIFIC COLLABORATION VIRGO COLLABORATION
LIGO SCIENTIFIC COLLABORATION VIRGO COLLABORATION Document Type LIGO-T070083-00-Z VIR-023A-084 The LSC-Virgo white paper on gravitational wave data analysis Science goals, data analysis methods, status
More informationProbability of detecting compact binary coalescence with enhanced LIGO
Probability of detecting compact binary coalescence with enhanced LIGO Richard O Shaughnessy [V. Kalogera, K. Belczynski] GWDAW-12, December 13, 2007 Will we see a merger soon? Available predictions Isolated
More informationPhysics 9e/Cutnell. correlated to the. College Board AP Physics 1 Course Objectives
Physics 9e/Cutnell correlated to the College Board AP Physics 1 Course Objectives Big Idea 1: Objects and systems have properties such as mass and charge. Systems may have internal structure. Enduring
More information3-rd lecture: Modified gravity and local gravity constraints
3-rd lecture: Modified gravity and local gravity constraints Local gravity tests If we change gravity from General Relativity, there are constraints coming from local gravity tests. Solar system tests,
More informationThe Orbital Period Distribution of Wide Binary Millisecond Pulsars
Binary Radio Pulsars ASP Conference Series, Vol. 328, 2005 F. A. Rasio and I. H. Stairs The Orbital Period Distribution of Wide Binary Millisecond Pulsars B. Willems Northwestern University, Department
More informationData Provided: A formula sheet and table of physical constants is attached to this paper. DARK MATTER AND THE UNIVERSE
Data Provided: A formula sheet and table of physical constants is attached to this paper. DEPARTMENT OF PHYSICS AND ASTRONOMY Autumn Semester (2014-2015) DARK MATTER AND THE UNIVERSE 2 HOURS Answer question
More informationWave-particle and wave-wave interactions in the Solar Wind: simulations and observations
Wave-particle and wave-wave interactions in the Solar Wind: simulations and observations Lorenzo Matteini University of Florence, Italy In collaboration with Petr Hellinger, Simone Landi, and Marco Velli
More informationWolfgang Tichy. Address: Science & Engineering Building, Room 444 Physics Department Florida Atlantic University 777 Glades Road Boca Raton, FL 33431
Wolfgang Tichy Address: Science & Engineering Building, Room 444 Physics Department Florida Atlantic University 777 Glades Road Boca Raton, FL 33431 Phone: (561) 318 0442 Fax: (561) 297 2662 E-Mail: wolf@fau.edu
More informationarxiv:1207.3646v1 [cs.ce] 16 Jul 2012
jcis@epacis.org OGCOSMO: An auxiliary tool for the study of the Universe within hierarchical scenario of structure formation arxiv:1207.3646v1 [cs.ce] 16 Jul 2012 Eduardo S. Pereira 1, Oswaldo D. Miranda
More informationRF Measurements Using a Modular Digitizer
RF Measurements Using a Modular Digitizer Modern modular digitizers, like the Spectrum M4i series PCIe digitizers, offer greater bandwidth and higher resolution at any given bandwidth than ever before.
More informationon Recent Developments on Theoretical and Experimental General Relativity, Astrophysics, and Relativistic Field Theories
Thirteenth Marcel Grossman Meeting on Recent Developments on Theoretical and Experimental General Relativity, Astrophysics, and Relativistic Field Theories ON GENERAL RELATIVISTIC UNIFORMLY ROTATING WHITE
More informationAT THE INTERFACE: GRAVITATIONAL WAVES AS TOOLS TO TEST QUANTUM GRAVITY AND PROBE THE ASTROPHYSICAL UNIVERSE
The Pennsylvania State University The Graduate School Department of Physics AT THE INTERFACE: GRAVITATIONAL WAVES AS TOOLS TO TEST QUANTUM GRAVITY AND PROBE THE ASTROPHYSICAL UNIVERSE A Dissertation in
More informationChapter 15.3 Galaxy Evolution
Chapter 15.3 Galaxy Evolution Elliptical Galaxies Spiral Galaxies Irregular Galaxies Are there any connections between the three types of galaxies? How do galaxies form? How do galaxies evolve? P.S. You
More informationarxiv:1405.3693v1 [gr-qc] 14 May 2014
International Journal of Modern Physics D c World Scientific Publishing Company arxiv:1405.3693v1 [gr-qc] 14 May 2014 Key Elements of Robustness in Binary Black Hole Evolutions using Spectral Methods Béla
More informationMASSACHUSETTS INSTITUTE OF TECHNOLOGY Department of Physics. 8.02 Spring 2013 Conflict Exam Two Solutions
MASSACHUSETTS INSTITUTE OF TECHNOLOGY Department of Physics 802 Spring 2013 Conflict Exam Two Solutions Problem 1 (25 points): answers without work shown will not be given any credit A uniformly charged
More informationThe Milky Way Galaxy is Heading for a Major Cosmic Collision
The Milky Way Galaxy is Heading for a Major Cosmic Collision Roeland van der Marel (STScI) [based on work with a team of collaborators reported in the Astrophysical Journal July 2012] Hubble Science Briefing
More informationPart IV. Conclusions
Part IV Conclusions 189 Chapter 9 Conclusions and Future Work CFD studies of premixed laminar and turbulent combustion dynamics have been conducted. These studies were aimed at explaining physical phenomena
More informationAttitude and Orbit Dynamics of High Area-to-Mass Ratio (HAMR) Objects and
Attitude and Orbit Dynamics of High Area-to-Mass Ratio (HAMR) Objects and Carolin Früh National Research Council Postdoctoral Fellow, AFRL, cfrueh@unm.edu Orbital Evolution of Space Debris Objects Main
More informationNumerical Methods for Differential Equations
Numerical Methods for Differential Equations Course objectives and preliminaries Gustaf Söderlind and Carmen Arévalo Numerical Analysis, Lund University Textbooks: A First Course in the Numerical Analysis
More informationMcLachlan: An Open Community Code for Numerical Relativity
McLachlan: An Open Community Code for Numerical Relativity Peter Diener Center for Computation and Technology and Department of Physics and Astronomy Louisiana State University Collaborators: Erik Schnetter,
More informationarxiv:astro-ph/0101553v1 31 Jan 2001
Evidence for Large Stellar Disks in Elliptical Galaxies. Andreas Burkert and Thorsten Naab Max-Planck-Institut für Astronomie, D-69242 Heidelberg, Germany arxiv:astro-ph/0101553v1 31 Jan 2001 Abstract.
More informationHow Do Galeries Form?
8-5-2015see http://www.strw.leidenuniv.nl/ franx/college/ mf-sts-2015-c9-1 8-5-2015see http://www.strw.leidenuniv.nl/ franx/college/ mf-sts-2015-c9-2 Galaxy Formation Leading questions for today How do
More informationDIRECT ORBITAL DYNAMICS: USING INDEPENDENT ORBITAL TERMS TO TREAT BODIES AS ORBITING EACH OTHER DIRECTLY WHILE IN MOTION
1 DIRECT ORBITAL DYNAMICS: USING INDEPENDENT ORBITAL TERMS TO TREAT BODIES AS ORBITING EACH OTHER DIRECTLY WHILE IN MOTION Daniel S. Orton email: dsorton1@gmail.com Abstract: There are many longstanding
More informationInternational Year of Light 2015 Tech-Talks BREGENZ: Mehmet Arik Well-Being in Office Applications Light Measurement & Quality Parameters
www.led-professional.com ISSN 1993-890X Trends & Technologies for Future Lighting Solutions ReviewJan/Feb 2015 Issue LpR 47 International Year of Light 2015 Tech-Talks BREGENZ: Mehmet Arik Well-Being in
More information(Long-Baseline) Interferometric Measurements of Binary Stars
(Long-Baseline) Interferometric Measurements of Binary Stars A. Boden MSC/Caltech & GSU C. Hummel USNO/ESO G. Torres & D. Latham CfA H. McAlister CHARA/GSU Outline Introduction: Why study binary stars
More informationJeff Thomas Tom Holmes Terri Hightower. Learn RF Spectrum Analysis Basics
Jeff Thomas Tom Holmes Terri Hightower Learn RF Spectrum Analysis Basics Learning Objectives Name the major measurement strengths of a swept-tuned spectrum analyzer Explain the importance of frequency
More informationTEMPERATURE DEPENDENCE OF GRAVITATIONAL FORCE: EXPERIMENTS, ASTROPHYSICS, PERSPECTIVES. A.L. Dmitriev
TEMPERATURE DEPENDENCE OF GRAVITATIONAL FORCE: EXPERIMENTS, ASTROPHYSICS, PERSPECTIVES A.L. Dmitriev St-Petersburg University of Information Technologies, Mechanics and Optics 49, Kronverksky Prospect,
More informationOrbital Dynamics with Maple (sll --- v1.0, February 2012)
Orbital Dynamics with Maple (sll --- v1.0, February 2012) Kepler s Laws of Orbital Motion Orbital theory is one of the great triumphs mathematical astronomy. The first understanding of orbits was published
More informationDO PHYSICS ONLINE FROM QUANTA TO QUARKS QUANTUM (WAVE) MECHANICS
DO PHYSICS ONLINE FROM QUANTA TO QUARKS QUANTUM (WAVE) MECHANICS Quantum Mechanics or wave mechanics is the best mathematical theory used today to describe and predict the behaviour of particles and waves.
More informationFrequency-domain and stochastic model for an articulated wave power device
Frequency-domain stochastic model for an articulated wave power device J. Cândido P.A.P. Justino Department of Renewable Energies, Instituto Nacional de Engenharia, Tecnologia e Inovação Estrada do Paço
More informationThe rate of change of velocity with respect to time. The average rate of change of distance/displacement with respect to time.
H2 PHYSICS DEFINITIONS LIST Scalar Vector Term Displacement, s Speed Velocity, v Acceleration, a Average speed/velocity Instantaneous Velocity Newton s First Law Newton s Second Law Newton s Third Law
More informationDynamics of Iain M. Banks Orbitals. Richard Kennaway. 12 October 2005
Dynamics of Iain M. Banks Orbitals Richard Kennaway 12 October 2005 Note This is a draft in progress, and as such may contain errors. Please do not cite this without permission. 1 The problem An Orbital
More informationNonlinear evolution of unstable fluid interface
Nonlinear evolution of unstable fluid interface S.I. Abarzhi Department of Applied Mathematics and Statistics State University of New-York at Stony Brook LIGHT FLUID ACCELERATES HEAVY FLUID misalignment
More informationarxiv:astro-ph/0602533v1 24 Feb 2006
Astronomy & Astrophysics manuscript no. paper c EO 2008 February 5, 2008 arxiv:astro-ph/0602533v1 24 Feb 2006 VIRGO sensitivity to binary coalescences and the Population III black hole binaries K. Kulczycki
More informationarxiv:0803.1853v2 [gr-qc] 30 Mar 2011
Accuracy of the Post-Newtonian Approximation: Optimal Asymptotic Expansion for Quasi-Circular, Extreme-Mass Ratio Inspirals Nicolás Yunes 1 and Emanuele Berti 2 1 Institute for Gravitational Physics and
More informationCarol and Charles see their pencils fall exactly straight down.
Section 24-1 1. Carol is in a railroad car on a train moving west along a straight stretch of track at a constant speed of 120 km/h, and Charles is in a railroad car on a train at rest on a siding along
More informationAMS Verification at SoC Level: A practical approach for using VAMS vs SPICE views
AMS Verification at SoC Level: A practical approach for using VAMS vs SPICE views Nitin Pant, Gautham Harinarayan, Manmohan Rana Accellera Systems Initiative 1 Agenda Need for SoC AMS Verification Mixed
More informationThe Essence of Gravitational Waves and Energy
The Essence of Gravitational Waves and Energy F. I. Cooperstock Department of Physics and Astronomy University of Victoria P.O. Box 3055, Victoria, B.C. V8W 3P6 (Canada) March 26, 2015 Abstract We discuss
More informationHow To Understand General Relativity
Chapter S3 Spacetime and Gravity What are the major ideas of special relativity? Spacetime Special relativity showed that space and time are not absolute Instead they are inextricably linked in a four-dimensional
More informationPulsed Fourier Transform NMR The rotating frame of reference. The NMR Experiment. The Rotating Frame of Reference.
Pulsed Fourier Transform NR The rotating frame of reference The NR Eperiment. The Rotating Frame of Reference. When we perform a NR eperiment we disturb the equilibrium state of the sstem and then monitor
More informationOn a Flat Expanding Universe
Adv. Studies Theor. Phys., Vol. 7, 2013, no. 4, 191-197 HIKARI Ltd, www.m-hikari.com On a Flat Expanding Universe Bo Lehnert Alfvén Laboratory Royal Institute of Technology, SE-10044 Stockholm, Sweden
More informationThe Hidden Lives of Galaxies. Jim Lochner, USRA & NASA/GSFC
The Hidden Lives of Galaxies Jim Lochner, USRA & NASA/GSFC What is a Galaxy? Solar System Distance from Earth to Sun = 93,000,000 miles = 8 light-minutes Size of Solar System = 5.5 light-hours What is
More informationAssessment Plan for Learning Outcomes for BA/BS in Physics
Department of Physics and Astronomy Goals and Learning Outcomes 1. Students know basic physics principles [BS, BA, MS] 1.1 Students can demonstrate an understanding of Newton s laws 1.2 Students can demonstrate
More informationDepartment of Electrical and Computer Engineering Ben-Gurion University of the Negev. LAB 1 - Introduction to USRP
Department of Electrical and Computer Engineering Ben-Gurion University of the Negev LAB 1 - Introduction to USRP - 1-1 Introduction In this lab you will use software reconfigurable RF hardware from National
More informationThe Quantum Harmonic Oscillator Stephen Webb
The Quantum Harmonic Oscillator Stephen Webb The Importance of the Harmonic Oscillator The quantum harmonic oscillator holds a unique importance in quantum mechanics, as it is both one of the few problems
More informationNumerical Simulations of Black-Hole Spacetimes
Numerical Simulations of Black-Hole Spacetimes Thesis by Tony Chu In Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy California Institute of Technology Pasadena, California
More informationFluid structure interaction of a vibrating circular plate in a bounded fluid volume: simulation and experiment
Fluid Structure Interaction VI 3 Fluid structure interaction of a vibrating circular plate in a bounded fluid volume: simulation and experiment J. Hengstler & J. Dual Department of Mechanical and Process
More informationAnalysis of Wing Leading Edge Data. Upender K. Kaul Intelligent Systems Division NASA Ames Research Center Moffett Field, CA 94035
Analysis of Wing Leading Edge Data Upender K. Kaul Intelligent Systems Division NASA Ames Research Center Moffett Field, CA 94035 Abstract Some selected segments of the STS114 ascent and on-orbit data
More informationHalliday, Resnick & Walker Chapter 13. Gravitation. Physics 1A PHYS1121 Professor Michael Burton
Halliday, Resnick & Walker Chapter 13 Gravitation Physics 1A PHYS1121 Professor Michael Burton II_A2: Planetary Orbits in the Solar System + Galaxy Interactions (You Tube) 21 seconds 13-1 Newton's Law
More informationEvolution of Close Binary Systems
Evolution of Close Binary Systems Before going on to the evolution of massive stars and supernovae II, we ll think about the evolution of close binary systems. There are many multiple star systems in the
More informationInstability, dispersion management, and pattern formation in the superfluid flow of a BEC in a cylindrical waveguide
Instability, dispersion management, and pattern formation in the superfluid flow of a BEC in a cylindrical waveguide Michele Modugno LENS & Dipartimento di Fisica, Università di Firenze, Italy Workshop
More informationGravitational waves: Understanding and Detection
Gravitational waves: Understanding and Detection Final draft Physics 222 November 11, 1999 Aaron Astle Dan Hale Dale Kitchen Wesley Krueger Abstract Gravitational waves carry information about catastrophic
More informationModified Gravity and the CMB
Modified Gravity and the CMB Philippe Brax, IphT Saclay, France arxiv:1109.5862 PhB, A.C. Davis Work in progress PhB, ACD, B. Li Minneapolis October 2011 PLANCK will give us very precise information on
More informationDepartment of Physics University of Wisconsin-Milwaukee Phone: (414) 229-2590 E-mail: chang65@uwm.edu Milwaukee, WI 53201
Philip Chang Contact Information Education Department of Physics University of Wisconsin-Milwaukee Phone: (414) 229-2590 PO Box 413 E-mail: chang65@uwm.edu Milwaukee, WI 53201 University of California
More informationIntroduction to spectral methods
Introduction to spectral methods Eric Gourgoulhon Laboratoire de l Univers et de ses Théories (LUTH) CNRS / Observatoire de Paris Meudon, France Based on a collaboration with Silvano Bonazzola, Philippe
More informationMASTER OF SCIENCE IN PHYSICS MASTER OF SCIENCES IN PHYSICS (MS PHYS) (LIST OF COURSES BY SEMESTER, THESIS OPTION)
MASTER OF SCIENCE IN PHYSICS Admission Requirements 1. Possession of a BS degree from a reputable institution or, for non-physics majors, a GPA of 2.5 or better in at least 15 units in the following advanced
More informationIntroductory FLUENT Training
Chapter 10 Transient Flow Modeling Introductory FLUENT Training www.ptecgroup.ir 10-1 Motivation Nearly all flows in nature are transient! Steady-state assumption is possible if we: Ignore transient fluctuations
More informationA Universe of Galaxies
A Universe of Galaxies Today s Lecture: Other Galaxies (Chapter 16, pages 366-397) Types of Galaxies Habitats of Galaxies Dark Matter Other Galaxies Originally called spiral nebulae because of their shape.
More information2.1 CFD PROJECT PLANNING. 2006 ANSYS, Inc. All rights reserved. ANSYS, Inc. Proprietary
2.1 CFD PROJECT PLANNING 2006 ANSYS, Inc. All rights reserved. 2008 ANSYS, Inc. All rights reserved. 6-2 CFD PROJECT PLANNING Task definition Resources Timing and deliverables Design review Assumed part
More informationPuzzling features of data from asteroseismology space missions
Puzzling features of data from asteroseismology space missions Javier Pascual Granado Rafael Garrido Haba XI CoRoT Week La Laguna, Tenerife, Spain 19-22 March 2013 Motivation Old problems like the search
More informationME6130 An introduction to CFD 1-1
ME6130 An introduction to CFD 1-1 What is CFD? Computational fluid dynamics (CFD) is the science of predicting fluid flow, heat and mass transfer, chemical reactions, and related phenomena by solving numerically
More informationPower System Harmonics
Pacific Gas and Electric Company Power System Harmonics What are power system harmonics? Ideally, voltage and current waveforms are perfect sinusoids. However, because of the increased popularity of electronic
More informationSIESMIC SLOSHING IN CYLINDRICAL TANKS WITH FLEXIBLE BAFFLES
SIESMIC SLOSHING IN CYLINDRICAL TANKS WITH FLEXIBLE BAFFLES Kayahan AKGUL 1, Yasin M. FAHJAN 2, Zuhal OZDEMIR 3 and Mhamed SOULI 4 ABSTRACT Sloshing has been one of the major concerns for engineers in
More informationMODULE VII LARGE BODY WAVE DIFFRACTION
MODULE VII LARGE BODY WAVE DIFFRACTION 1.0 INTRODUCTION In the wave-structure interaction problems, it is classical to divide into two major classification: slender body interaction and large body interaction.
More informationLow-Mass X-Ray Binary Models for Ellipticals NGC3379 and NGC4278
Low-Mass X-Ray Binary Models for Ellipticals NGC3379 and NGC4278 Tassos Fragos with V. Kalogera, K. Belczynski, G. Fabbiano et al. Department of Physics and Astronomy Northwestern University MODEST 7b
More informationTheoretical Perspective
Preface Motivation Manufacturer of digital products become a driver of the world s economy. This claim is confirmed by the data of the European and the American stock markets. Digital products are distributed
More informationAntelope Contributed Software Development Status for Detectors, Focal Mechanisms, Moment Tensors, Locations
Antelope Contributed Software Development Status for Detectors, Focal Mechanisms, Moment Tensors, Locations Text Frank Vernon IGPP UCSD Antelope User Group Papagayo, Costa Rica 4-6 November 2013 1 Topics
More informationWhite Dwarf Properties and the Degenerate Electron Gas
White Dwarf Properties and the Degenerate Electron Gas Nicholas Rowell April 10, 2008 Contents 1 Introduction 2 1.1 Discovery....................................... 2 1.2 Survey Techniques..................................
More informationEfficient Curve Fitting Techniques
15/11/11 Life Conference and Exhibition 11 Stuart Carroll, Christopher Hursey Efficient Curve Fitting Techniques - November 1 The Actuarial Profession www.actuaries.org.uk Agenda Background Outline of
More informationAPPENDIX N. Data Validation Using Data Descriptors
APPENDIX N Data Validation Using Data Descriptors Data validation is often defined by six data descriptors: 1) reports to decision maker 2) documentation 3) data sources 4) analytical method and detection
More informationarxiv:gr-qc/9409057v1 27 Sep 1994
Gravitational Radiation from Nonaxisymmetric Instability in a Rotating Star J. L. Houser, J. M. Centrella, and S. C. Smith Department of Physics and Atmospheric Science, Drexel University, Philadelphia,
More informationGravity Testing and Interpreting Cosmological Measurement
Cosmological Scale Tests of Gravity Edmund Bertschinger MIT Department of Physics and Kavli Institute for Astrophysics and Space Research January 2011 References Caldwell & Kamionkowski 0903.0866 Silvestri
More informationarxiv:0908.0620v1 [gr-qc] 5 Aug 2009
A new numerical method to construct binary neutron star initial data arxiv:0908.060v1 [gr-qc] 5 Aug 009 Wolfgang Tichy Department of Physics, Florida Atlantic University, Boca Raton, FL 33431, USA Abstract.
More informationSimulation of Spiral Density Waves with Rotating, Shallow water
Simulation of Spiral Density Waves with Rotating, Shallow water R. Merrill, C. Buckey, M. Katschke, T. Manuszak, and J. Pinkney Department of Physics and Astronomy Ohio Northern University Abstract We
More informationPrecession of spin and Precession of a top
6. Classical Precession of the Angular Momentum Vector A classical bar magnet (Figure 11) may lie motionless at a certain orientation in a magnetic field. However, if the bar magnet possesses angular momentum,
More informationMass flux fluctuation in a cloud resolving simulation with diurnal forcing
Mass flux fluctuation in a cloud resolving simulation with diurnal forcing Jahanshah Davoudi Norman McFarlane, Thomas Birner Physics department, University of Toronto Mass flux fluctuation in a cloud resolving
More informationWIMP dark matter and the isotropic radio signal Roberto A. Lineros R. Instituto de Física Corpuscular - CSIC/U. Valencia @Roberto_Lineros Outline Introduction Cosmic ray propagation Synchrotron emission
More informationThe Layout of the Solar System
The Layout of the Solar System Planets fall into two main categories Terrestrial (i.e. Earth-like) Jovian (i.e. Jupiter-like or gaseous) [~5000 kg/m 3 ] [~1300 kg/m 3 ] What is density? Average density
More informationLecture 7 Formation of the Solar System. Nebular Theory. Origin of the Solar System. Origin of the Solar System. The Solar Nebula
Origin of the Solar System Lecture 7 Formation of the Solar System Reading: Chapter 9 Quiz#2 Today: Lecture 60 minutes, then quiz 20 minutes. Homework#1 will be returned on Thursday. Our theory must explain
More informationCensus of Exoplanets (w/ Doppler observations) NASA
Planetary Dynamics in the Kepler Era Eric B. Ford UF Frontiers September 2, 2011 w/ results from UF students/postdocs (Althea Moorhead, Robert Morehead, Benjamin Nelson, Matthew Payne), Kepler Follow-Up
More information