on Recent Developments on Theoretical and Experimental General Relativity, Astrophysics, and Relativistic Field Theories
|
|
|
- Whitney Wilkinson
- 8 years ago
- Views:
Transcription
1 Thirteenth Marcel Grossman Meeting on Recent Developments on Theoretical and Experimental General Relativity, Astrophysics, and Relativistic Field Theories ON GENERAL RELATIVISTIC UNIFORMLY ROTATING WHITE DWARFS Kuantay Boshkayev Jorge A. Rueda, Remo Ruffini and Ivan Siutsou Dipartimento di Fisica, Universita' di Roma La Sapienza, Piazzale Aldo Moro 5, I Roma, Italy ICRANet, Piazzale della Repubblica 10, I Pescara, Italy Stockholm, July 1-7, 2012
2 Outline Introduction; Motivations; The Hartle-Thorne formalism; Stability criteria, i Equation of state; t Results, applications and conclusions.
3 Introduction Rotondo, M., Rueda, J. A., Ruffini, R., & Xue, S.-S. 2011, Phys. Rev. D, 84, Rotondo, R t d M., Rueda, J. A., Ruffini, i R., & Xue, S.-S. S 2011, Phys. Rev. C, 83, Malheiro, M., Rueda, J. A., & Ruffini, R. 2011, PASJ, in press; arxiv: The aim of the work Maximum mass of rotating white dwarfs. Stability (GR, Inverse beta decay, mass shedding and secular). Minimum period (Maximum angular velocity).
4 Motivations 2 P E 4 I 3 rot P R=10 0km, R=10 3 km, I=10 45 [g cm 2 ] I=10 49 [g cm 2 ] X-ray luminosity versus the loss of rotational energy describing SGRs and AXPs by rotation powered neutron stars and white dwarfs. The green star and the green triangle correspond to SGR using respectively the upper and the lower limit of Pdot given by the Eq. above. The blue squares are the only four sources that satisfy L X <E rot dot when described as neutron stars. R=10 km, I=10 45 [g cm 2 ] according to the magnetar model M=1 1.4Msun R=10 3 km, I=10 49 [g cm 2 ] according to the white dwarf (RHMWD) model Malheiro, M., Rueda, J. A., & Ruffini, R. 2011, PASJ, in press; arxiv:
5 The Hartle Thorne formalism, solutions Hartle, J. B. 1967, Astrophys. J., 150, 1005 Hartle, J. B. & Thorne, K. S. 1968, Astrophys. J., 153, 807 Stergioulas, N. 2003, Living Reviews in Relativity, 6, 3 N. K. Glendenning. Compact Stars: Nuclear Physics, Particle Physics & General Relativity
6 M 0, stable, M 0, Stability criteria for NRWDs General Relativity instability M max M 0, unstable., Newtonian Physics General Relativity Inverse β-decay instability p e n, e ( Z, A) ( Z 1, A). R t d M R d J A R ffi i R & X S S 2011 Ph R D Rotondo, M., Rueda, J. A., Ruffini, R., & Xue, S.-S. 2011, Phys. Rev. D, 84, Rotondo, M., Rueda, J. A., Ruffini, R., & Xue, S.-S. 2011, Phys. Rev. C, 83,
7 Stability criteria for RWDs Mass shedding Bini, D., Boshkayev, K., Ruffini, R., & Siutsou, I. 2012, (in press) NCC Secular and dynamical instabilities e= , T/W=0.14 for Maclaurin spheroids e= , T/W=0.25 Chandrasekhar (1969) Axisymmetric secular instability M J M M 0, stable; 0, M max; 0, unstable. J J Friedman, J. L., Ipser, J. R., & Sorkin, R. D. 1988, Astrophys. J., 325, 722
8 Equation of state Rotondo, M., Rueda, J. A., Ruffini, R., & Xue, S.-S. 2011, Phys. Rev. D, 84, T. Hamada and E. E. Salpeter, Astrophys. J. 134, 683 (1961).
9 Surface Pressure for different EoS Rotondo, M., Rueda, J. A., Ruffini, R., & Xue, S.-S. 2011, Phys. Rev. D, 84,
10 Results: Mass vs central density Carbon WD for RFMT EoS. Boshkayev, K., Rueda, J. A. & Ruffini, R., IJMPE, 2011, 20, 136
11 Eccentricity versus central density T/W (kinetic energy/binding energy) versus central density e= , e= T/W=0.14 T/W=0.25 Carbon WD for RFMT EoS. Boshkayev, K., Rueda, J. A. & Ruffini, R., IJMPE, 2011, 20, 136 Boshkayev, y, K., Rueda, J. A. & Ruffini, R., IJMPCS, (in press) 2012
12 Non-rotating case General Relativity! Rotating case Is this period minimum?
13 Constant J sequence Turning point method of Friedman, Ipser & Sorkin, 1988, ApJ, 325, 722
14 Stability region: M vs rho Carbon WD for RFMT EoS. Boshkayev K Rueda J A Ruffini R & Siutsou I ApJ 2012 Boshkayev, K., Rueda, J. A., Ruffini, R., & Siutsou, I. ApJ, 2012, submitted; arxiv:
15 Stability region: M vs rho Oxygen WD for RFMT EoS. Boshkayev, K., Rueda, J. A., Ruffini, R., & Siutsou, I. ApJ, 2012, submitted; arxiv:
16 Stability region: M vs Req P min Carbon WD for RFMT EoS. Boshkayev K Rueda J A Ruffini R & Siutsou I ApJ 2012 Boshkayev, K., Rueda, J. A., Ruffini, R., & Siutsou, I. ApJ, 2012, submitted; arxiv:
17 Minimum periods The minimum period is determined at the crossing point between Keplerian and inverse beta decay sequences! The minimum period is consistent with the observed periods of SGRs and AXPs! Malheiro, M., Rueda, J. A., & Ruffini, R. 2011, PASJ, in press; arxiv: Boshkayev, K., Rueda, J. A. & Ruffini, R., IJMPCS, 2012, in press
18 Conclusion We have investigated the behaviour of general relativistic uniformly rotating WDs for given values of the central density and rotation period on the basis Hartle-Thorne formalism using the EoS of Chandrasekhar, Salpeter and RFMT for WDs introduced in Rotondo, Rueda, Ruffini,Xue, 2011, PRC, 83, and Rotondo, Rueda, Ruffini, Xue, 2011, PRD, 84, We have shown that the minimum rotation periods are approximately 0.3, 0.5, 0.7 and 2.2 seconds for a rotating 4 He, 12 C, 16 O, and 56 Fe WDs (RFMT EoS), respectively. Corresponding maximum masses to the same chemical composition are 1.500, 1.474, and Solar mass. Below these minimum periods the configurations become unstable because of mass shedding, secular and dynamical instabilities. M J 0 max 1.06M We showed that WDs composed of light elements (Helium, Carbon) are unstable against axisymmetric secular instability, whereas WDs with heavy elements (Oxygen,.., Iron) are stable. J 0 max,
19 Thank you for your attention!
Mass 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)
Fridolin Weber San Diego State University San Diego, California USA
Fridolin Weber San Diego State University San Diego, California USA IAU Symposium 291 Neutron Stars and Pulsars: Challenges and OpportuniEes afer 80 years IAU General Assembly XXVIII 20-31 August 2012,
arxiv: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,
Solar Energy Production
Solar Energy Production We re now ready to address the very important question: What makes the Sun shine? Why is this such an important topic in astronomy? As humans, we see in the visible part of the
The Physics of Neutron Stars
The Physics of Neutron Stars Alfred Whitehead Physics 518, Fall 009 The Problem Describe how a white dwarf evolves into a neutron star. Compute the neutron degeneracy pressure and balance the gravitational
Nuclear Physics. Nuclear Physics comprises the study of:
Nuclear Physics Nuclear Physics comprises the study of: The general properties of nuclei The particles contained in the nucleus The interaction between these particles Radioactivity and nuclear reactions
Extra-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.
Lecture 3 Properties and Evolution of Molecular Clouds. Spitzer space telescope image of Snake molecular cloud (IRDC G11.11-0.11
Lecture 3 Properties and Evolution of Molecular Clouds Spitzer space telescope image of Snake molecular cloud (IRDC G11.11-0.11 From slide from Annie Hughes Review CO t in clouds HI: Atomic Hydrogen http://www.atnf.csiro.au/research/lvmeeting/magsys_pres/
Lecture 14. Introduction to the Sun
Lecture 14 Introduction to the Sun ALMA discovers planets forming in a protoplanetary disc. Open Q: what physics do we learn about the Sun? 1. Energy - nuclear energy - magnetic energy 2. Radiation - continuum
Heating & Cooling in Molecular Clouds
Lecture 8: Cloud Stability Heating & Cooling in Molecular Clouds Balance of heating and cooling processes helps to set the temperature in the gas. This then sets the minimum internal pressure in a core
Physics 1104 Midterm 2 Review: Solutions
Physics 114 Midterm 2 Review: Solutions These review sheets cover only selected topics from the chemical and nuclear energy chapters and are not meant to be a comprehensive review. Topics covered in these
White 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..................................
Gamma Ray Detection at RIA
Gamma Ray Detection at RIA Summary Report: Physics & Functional Requirements Cyrus Baktash Physics goals Experimental tools: Techniques & Reactions Functional Requirements Physics Questions (Discussed
Gravitomagnetism 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
1. Degenerate Pressure
. Degenerate Pressure We next consider a Fermion gas in quite a different context: the interior of a white dwarf star. Like other stars, white dwarfs have fully ionized plasma interiors. The positively
Atomic Structure: Chapter Problems
Atomic Structure: Chapter Problems Bohr Model Class Work 1. Describe the nuclear model of the atom. 2. Explain the problems with the nuclear model of the atom. 3. According to Niels Bohr, what does n stand
Solar System Fundamentals. What is a Planet? Planetary orbits Planetary temperatures Planetary Atmospheres Origin of the Solar System
Solar System Fundamentals What is a Planet? Planetary orbits Planetary temperatures Planetary Atmospheres Origin of the Solar System Properties of Planets What is a planet? Defined finally in August 2006!
Chapter Test B. Chapter: Measurements and Calculations
Assessment Chapter Test B Chapter: Measurements and Calculations PART I In the space provided, write the letter of the term or phrase that best completes each statement or best answers each question. 1.
Main properties of atoms and nucleus
Main properties of atoms and nucleus. Atom Structure.... Structure of Nuclei... 3. Definition of Isotopes... 4. Energy Characteristics of Nuclei... 5. Laws of Radioactive Nuclei Transformation... 3. Atom
Miras, Mass-Loss, and the Ultimate Fate of the Earth L. A. Willson & G. H. Bowen, Iowa State University. Fire and Ice:
Miras, Mass-Loss, and the Ultimate Fate of the Earth L. A. Willson & G. H. Bowen, Iowa State University Fire and Ice: Some say the world will end in fire, Some say in ice. From what I've tasted of desire
Laser driven shock experiments at PALS
Laser driven shock experiments at PALS D.Batani, H.Stabile, A.Ravasio, T.Desai, G.Lucchini, F.Strati Dipartimento di Fisica G. Occhialini, Università degli Studi di Milano Bicocca and INFM, 20126 Milano,Italy
Constraints on the explosion mechanism and progenitors of Type Ia supernovae
Constraints on the explosion mechanism and progenitors of Type Ia supernovae Stéphane Blondin Laboratoire d Astrophysique de Marseille Luc Dessart Observatoire de la Côte d Azur John Hillier University
Acoustics of tachyon Fermi gas
Acoustics of tachyon Fermi gas arxiv:1103.2276v4 [hep-ph] 3 Jun 2011 Ernst Trojan and George V. Vlasov Moscow Institute of Physics and Technology PO Box 3, Moscow, 125080, Russia June 6, 2011 Abstract
Data 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
Instability, 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
Central configuration in the planar n + 1 body problem with generalized forces.
Monografías de la Real Academia de Ciencias de Zaragoza. 28: 1 8, (2006). Central configuration in the planar n + 1 body problem with generalized forces. M. Arribas, A. Elipe Grupo de Mecánica Espacial.
Name Class Date. true
Exercises 131 The Falling Apple (page 233) 1 Describe the legend of Newton s discovery that gravity extends throughout the universe According to legend, Newton saw an apple fall from a tree and realized
CORSO DI FISICA NUCLEARE - PAOLO FINELLI DIP. FISICA ED ASTRONOMIA - UNIVERSITÀ DI BOLOGNA
Fission 1 DIP FISICA ED ASTRONOMIA - UNIVERSITÀ DI BOLOGNA Nuclear Fission 2 DIP FISICA ED ASTRONOMIA - UNIVERSITÀ DI BOLOGNA 3 DIP FISICA ED ASTRONOMIA - UNIVERSITÀ DI BOLOGNA Fission timeline - I 4 DIP
Stellar Evolution: a Journey through the H-R Diagram
Stellar Evolution: a Journey through the H-R Diagram Mike Montgomery 21 Apr, 2001 0-0 The Herztsprung-Russell Diagram (HRD) was independently invented by Herztsprung (1911) and Russell (1913) They plotted
Be Stars. By Carla Morton
Be Stars By Carla Morton Index 1. Stars 2. Spectral types 3. B Stars 4. Be stars 5. Bibliography How stars are formed Stars are composed of gas Hydrogen is the main component of stars. Stars are formed
Nuclear fusion in stars. Collapse of primordial density fluctuations into galaxies and stars, nucleosynthesis in stars
Nuclear fusion in stars Collapse of primordial density fluctuations into galaxies and stars, nucleosynthesis in stars The origin of structure in the Universe Until the time of formation of protogalaxies,
The 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
X-ray photoelectron. Ba 0.5 Sr 0.5 Co 0.8 Fe 0.2 O 3 δ and La 0.6 Sr 0.4 Co 0.2 Fe 0.8 O 3 δ before and after thermal treatment and permeation test
study on Ba 0.5 Sr 0.5 Co 0.8 Fe 0.2 O 3 δ and La 0.6 Sr 0.4 Co 0.2 Fe 0.8 O 3 δ before and after thermal treatment and permeation test Patrizia Rosa 1 1 Dipartimenti di Fisica Università degli Studi di
Name: João Fernando Alves da Silva Class: 7-4 Number: 10
Name: João Fernando Alves da Silva Class: 7-4 Number: 10 What is the constitution of the Solar System? The Solar System is constituted not only by planets, which have satellites, but also by thousands
Theory of electrons and positrons
P AUL A. M. DIRAC Theory of electrons and positrons Nobel Lecture, December 12, 1933 Matter has been found by experimental physicists to be made up of small particles of various kinds, the particles of
Medical Applications of radiation physics. Riccardo Faccini Universita di Roma La Sapienza
Medical Applications of radiation physics Riccardo Faccini Universita di Roma La Sapienza Outlook Introduction to radiation which one? how does it interact with matter? how is it generated? Diagnostics
Pablo 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,
Indiana's Academic Standards 2010 ICP Indiana's Academic Standards 2016 ICP. map) that describe the relationship acceleration, velocity and distance.
.1.1 Measure the motion of objects to understand.1.1 Develop graphical, the relationships among distance, velocity and mathematical, and pictorial acceleration. Develop deeper understanding through representations
Dinamica del Gas nelle Galassie II. Star formation
Dinamica del Gas nelle Galassie II. Star formation Overview on ISM Molecular clouds: composition and properties. Plasmas Charge neutrality, infinite conductivity; Field freezing; Euler equation with magnetic
L3: The formation of the Solar System
credit: NASA L3: The formation of the Solar System UCL Certificate of astronomy Dr. Ingo Waldmann A stable home The presence of life forms elsewhere in the Universe requires a stable environment where
Cross section, Flux, Luminosity, Scattering Rates
Cross section, Flux, Luminosity, Scattering Rates Table of Contents Paul Avery (Andrey Korytov) Sep. 9, 013 1 Introduction... 1 Cross section, flux and scattering... 1 3 Scattering length λ and λ ρ...
HR Diagram Student Guide
Name: HR Diagram Student Guide Background Information Work through the background sections on Spectral Classification, Luminosity, and the Hertzsprung-Russell Diagram. Then complete the following questions
Halliday, 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
Gravitational waves from neutron stars binaries: accuracy and tidal effects in the late inspiral S. Bernuzzi TPI-PAF FSU Jena / SFB-TR7
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 84 044012 (2011) SB, MT, &
The Universe Inside of You: Where do the atoms in your body come from?
The Universe Inside of You: Where do the atoms in your body come from? Matthew Mumpower University of Notre Dame Thursday June 27th 2013 Nucleosynthesis nu cle o syn the sis The formation of new atomic
KE A = PE MAX 1/2M v 2 = k q1 q2 /R
CHAPTER 13 NUCLEAR STRUCTURE NUCLEAR FORCE The nucleus is help firmly together by the nuclear or strong force, We can estimate the nuclear force by observing that protons residing about 1fm = 10-15m apart
PHYS 1624 University Physics I. PHYS 2644 University Physics II
PHYS 1624 Physics I An introduction to mechanics, heat, and wave motion. This is a calculus- based course for Scientists and Engineers. 4 hours (3 lecture/3 lab) Prerequisites: Credit for MATH 2413 (Calculus
Gravitation modifiée à grande distance & tests dans le système solaire 10 avril 2008
Gravitation modifiée à grande distance et tests dans le système solaire Gilles Esposito-Farèse, GRεCO, IAP et Peter Wolf, LNE-SYRTE 10 avril 2008 Gravitation modifiée à grande distance & tests dans le
Main sequence stars. Haris Ðapo. Antalya Lecture 3. 1 Akdeniz University, Antalya
Main sequence stars Haris Ðapo 1 Akdeniz University, Antalya Antalya Lecture 3. Haris Ðapo (Akdeniz University) Main sequence stars Main sequence stars 1 / 22 Outline 1 Introduction 2 Hydrogen burning
Lecture L22-2D Rigid Body Dynamics: Work and Energy
J. Peraire, S. Widnall 6.07 Dynamics Fall 008 Version.0 Lecture L - D Rigid Body Dynamics: Work and Energy In this lecture, we will revisit the principle of work and energy introduced in lecture L-3 for
The 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
Basic Nuclear Concepts
Section 7: In this section, we present a basic description of atomic nuclei, the stored energy contained within them, their occurrence and stability Basic Nuclear Concepts EARLY DISCOVERIES [see also Section
Is there chaos in Copenhagen problem?
Monografías de la Real Academia de Ciencias de Zaragoza 30, 43 50, (2006). Is there chaos in Copenhagen problem? Roberto Barrio, Fernando Blesa and Sergio Serrano GME, Universidad de Zaragoza Abstract
thermal history of the universe and big bang nucleosynthesis
thermal history of the universe and big bang nucleosynthesis Kosmologie für Nichtphysiker Markus Pössel (vertreten durch Björn Malte Schäfer) Fakultät für Physik und Astronomie, Universität Heidelberg
p-process in SNIa with multi-d models: their role in Galactic chemical evolution
in SNIa with multi-d models: their role in Galactic chemical evolution C. Travaglio INAF Observatory of Turin (Italy) R. Gallino University of Turin (Italy) F. Rӧpke, W. Hillebrandt Uni-Würzburg, MPA Munich
WIMP 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
PHYS-2010: General Physics I Course Lecture Notes Section XIII
PHYS-2010: General Physics I Course Lecture Notes Section XIII Dr. Donald G. Luttermoser East Tennessee State University Edition 2.5 Abstract These class notes are designed for use of the instructor and
Malcolm S. Longair. Galaxy Formation. With 141 Figures and 12 Tables. Springer
Malcolm S. Longair Galaxy Formation With 141 Figures and 12 Tables Springer Contents Part I Preliminaries 1. Introduction, History and Outline 3 1.1 Prehistory 3 1.2 The Theory of the Expanding Universe
From local to global relativity
Physical Interpretations of Relativity Theory XI Imperial College, LONDON, 1-15 SEPTEMBER, 8 From local to global relativity Tuomo Suntola, Finland T. Suntola, PIRT XI, London, 1-15 September, 8 On board
Objectives. PAM1014 Introduction to Radiation Physics. Constituents of Atoms. Atoms. Atoms. Atoms. Basic Atomic Theory
PAM1014 Introduction to Radiation Physics Basic Atomic Theory Objectives Introduce and Molecules The periodic Table Electronic Energy Levels Atomic excitation & de-excitation Ionisation Molecules Constituents
Symmetric planar non collinear relative equilibria for the Lennard Jones potential 3 body problem with two equal masses
Monografías de la Real Academia de Ciencias de Zaragoza. 25: 93 114, (2004). Symmetric planar non collinear relative equilibria for the Lennard Jones potential 3 body problem with two equal masses M. Corbera,
Earth Sciences -- Grades 9, 10, 11, and 12. California State Science Content Standards. Mobile Climate Science Labs
Earth Sciences -- Grades 9, 10, 11, and 12 California State Science Content Standards Covered in: Hands-on science labs, demonstrations, & activities. Investigation and Experimentation. Lesson Plans. Presented
Presentation of problem T1 (9 points): The Maribo Meteorite
Presentation of problem T1 (9 points): The Maribo Meteorite Definitions Meteoroid. A small particle (typically smaller than 1 m) from a comet or an asteroid. Meteorite: A meteoroid that impacts the ground
PoS(NIC XIII)084. Nuclear Astrophysics @ GANIL. Francois de Oliveira GANIL, Bd H. Becquerel, 14000 Caen E-mail: oliveira@ganil.fr
Nuclear Astrophysics @ GANIL Francois de Oliveira GANIL, Bd H. Becquerel, 14000 Caen E-mail: oliveira@ganil.fr GANIL is an unique facility where high quality radioactive beams are available at low and
ENERGY TRANSPORT WITHIN A STAR
M. Pettini: Structure and Evolution of Stars Lecture 8 ENERGY TRANSPORT WITHIN A STAR 8.1 Introduction Up to now, we have considered how energy is generated within the interior of stars by the processes
Dinamica dell Electron Cloud: Calcolo dei Coefficienti della Mappa
Dinamica dell Electron Cloud: Calcolo dei Coefficienti della Mappa T. Demma 1, S.Petracca 2,3, A. Stabile 2 1 LNF INFN, Frascati 2 Dipartimento di Ingegneria - Universita' del Sannio - Benevento 3 Sezione
2 ATOMIC SYSTEMATICS AND NUCLEAR STRUCTURE
2 ATOMIC SYSTEMATICS AND NUCLEAR STRUCTURE In this chapter the principles and systematics of atomic and nuclear physics are summarised briefly, in order to introduce the existence and characteristics of
Elliptical Galaxies. Houjun Mo. April 19, 2004. Basic properties of elliptical galaxies. Formation of elliptical galaxies
Elliptical Galaxies Houjun Mo April 19, 2004 Basic properties of elliptical galaxies Formation of elliptical galaxies Photometric Properties Isophotes of elliptical galaxies are usually fitted by ellipses:
Fuel Cell Activities at TU Graz
Fuel Cell Activities at TU Graz Viktor Hacker Institute of Chemical Engineering and Environmental Technology Graz University of Technology IEA Workshop TU Graz September 1 st, 2010 Content Lifetime and
Chem 1A Exam 2 Review Problems
Chem 1A Exam 2 Review Problems 1. At 0.967 atm, the height of mercury in a barometer is 0.735 m. If the mercury were replaced with water, what height of water (in meters) would be supported at this pressure?
This paper is also taken for the relevant Examination for the Associateship. For Second Year Physics Students Wednesday, 4th June 2008: 14:00 to 16:00
Imperial College London BSc/MSci EXAMINATION June 2008 This paper is also taken for the relevant Examination for the Associateship SUN, STARS, PLANETS For Second Year Physics Students Wednesday, 4th June
History of the Atom & Atomic Theory
Chapter 5 History of the Atom & Atomic Theory You re invited to a Thinking Inside the Box Conference Each group should nominate a: o Leader o Writer o Presenter You have 5 minutes to come up with observations
Structure and Properties of Atoms
PS-2.1 Compare the subatomic particles (protons, neutrons, electrons) of an atom with regard to mass, location, and charge, and explain how these particles affect the properties of an atom (including identity,
UNIVERSITA DEGLI STUDI DI ROMA LA SAPIENZA DIPARTIMENTO INGEGNERIA CHIMICA MATERIALI AMBIENTE
UNIVERSITA DEGLI STUDI DI ROMA LA SAPIENZA DIPARTIMENTO INGEGNERIA CHIMICA MATERIALI AMBIENTE REPORT ON A TEST EXECUTED ON A KDV DEPOLYMERIZATION PLANT ON JAN 19TH 2012 IN THE ORION ECOSOLUTIONS DEMONSTRATION
arxiv: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.
Spatially separated excitons in 2D and 1D
Spatially separated excitons in 2D and 1D David Abergel March 10th, 2015 D.S.L. Abergel 3/10/15 1 / 24 Outline 1 Introduction 2 Spatially separated excitons in 2D The role of disorder 3 Spatially separated
We know from the information given that we have an equal mass of each compound, but no real numbers to plug in and find moles. So what can we do?
How do we figure this out? We know that: 1) the number of oxygen atoms can be found by using Avogadro s number, if we know the moles of oxygen atoms; 2) the number of moles of oxygen atoms can be found
About the course GENERAL CHEMISTRY. Recommended literature: Chemistry: science of the matter. Responsible for the course: Dr.
About the course GENERAL CHEMISTRY University of Pécs Medical School Academic year 2009-2010. Responsible for the course: Dr. Attila AGÓCS Optional course for 2 credit points. To have grade at the and
Low-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
Gravity measurements with atom interferometry
Gravity measurements with atom interferometry Fiodor Sorrentino, 28/10/2010 Dipartimento di Fisica e Astronomia, Università di Firenze & INFN, Polo Scientifico di Sesto Fiorentino,via Sansone 1-50019 Sesto
Stellar Evolution. The Basic Scheme
Stellar Evolution The Basic Scheme Stars live for a very long time compared to human lifetimes. Even though stellar life-spans are enormous, we know how stars are born, live, and die. All stars follow
Aeration Air & Digester Gas Flow Metering Using Thermal Mass Technology. HWEA 2011 Conference Craig S. Johnson
Aeration Air & Digester Gas Flow Metering Using Thermal Mass Technology HWEA 2011 Conference Craig S. Johnson Presentation Overview Introduction Aeration Air & Digester gas challenges Gas flow metering
A n = 2 to n = 1. B n = 3 to n = 1. C n = 4 to n = 2. D n = 5 to n = 2
North arolina Testing Program EO hemistry Sample Items Goal 4 1. onsider the spectrum for the hydrogen atom. In which situation will light be produced? 3. Which color of light would a hydrogen atom emit
Amount of Substance. http://www.avogadro.co.uk/definitions/elemcompmix.htm
Page 1 of 14 Amount of Substance Key terms in this chapter are: Element Compound Mixture Atom Molecule Ion Relative Atomic Mass Avogadro constant Mole Isotope Relative Isotopic Mass Relative Molecular
Class #14/15 14/16 October 2008
Class #14/15 14/16 October 2008 Thursday, Oct 23 in class You ll be given equations and constants Bring a calculator, paper Closed book/notes Topics Stellar evolution/hr-diagram/manipulate the IMF ISM
A i A i. µ(ion) = Z i X i
Lecture 2 Review: calculation of mean atomic weight of an ionized gas (µ) Given a mass fraction X i (or abundance) for an ionic (or atomic) species with atomic weight A i, we can can calculate µ by: For
DO 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.
DYNAMICS OF GALAXIES
DYNAMICS OF GALAXIES 2. and stellar orbits Piet van der Kruit Kapteyn Astronomical Institute University of Groningen the Netherlands Winter 2008/9 and stellar orbits Contents Range of timescales Two-body
9 th Grade Physical Science Springfield Local Schools Common Course Syllabi. Course Description
9 th Grade Physical Science Springfield Local Schools Common Course Syllabi Course Description The purpose of the Physical Science course is to satisfy the Ohio Core science graduation requirement. The
Chapter NP-1. Nuclear Physics. Atomic Nature of Matter TABLE OF CONTENTS INTRODUCTION OBJECTIVES 1.0 PROPERTIES OF SUBSTANCES
Chapter NP-1 Nuclear Physics Atomic Nature of Matter TABLE OF CONTENTS INTRODUCTION OBJECTIVES 1.0 PROPERTIES OF SUBSTANCES 1.1 CHEMICAL AND PHYSICAL PROPERTIES 2.0 COMPOSITION OF ATOMS 2.1 ATOMIC STRUCTURE
WELCOME to Aurorae In the Solar System. J.E. Klemaszewski
WELCOME to Aurorae In the Solar System Aurorae in the Solar System Sponsoring Projects Galileo Europa Mission Jupiter System Data Analysis Program ACRIMSAT Supporting Projects Ulysses Project Outer Planets
ANSWER KEY : BUILD AN ATOM PART I: ATOM SCREEN Build an Atom simulation ( http://phet.colorado.edu/en/simulation/build an atom )
ANSWER KEY : PART I: ATOM SCREEN Build an Atom simulation ( http://phet.colorado.edu/en/simulation/build an atom ) 1. Explore the Build an Atom simulation with your group. As you explore, talk about what
Halliday, 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
WHERE DID ALL THE ELEMENTS COME FROM??
WHERE DID ALL THE ELEMENTS COME FROM?? In the very beginning, both space and time were created in the Big Bang. It happened 13.7 billion years ago. Afterwards, the universe was a very hot, expanding soup
Masses in Atomic Units
Nuclear Composition - the forces binding protons and neutrons in the nucleus are much stronger (binding energy of MeV) than the forces binding electrons to the atom (binding energy of ev) - the constituents
AQA Level 1/2 Certificate in Physics PAPER 1 SPECIMEN MARK SCHEME. AQA Level 1/2 Certificate in Physics Paper 1 MS
AQA Level /2 Certificate in Physics PAPER SPECIMEN MARK SCHEME AQA Level /2 Certificate in Physics Paper MS MARK SCHEME Information to Examiners. General The mark scheme for each question shows: the marks
Radioactivity III: Measurement of Half Life.
PHY 192 Half Life 1 Radioactivity III: Measurement of Half Life. Introduction This experiment will once again use the apparatus of the first experiment, this time to measure radiation intensity as a function
UNIT V. Earth and Space. Earth and the Solar System
UNIT V Earth and Space Chapter 9 Earth and the Solar System EARTH AND OTHER PLANETS A solar system contains planets, moons, and other objects that orbit around a star or the star system. The solar system
Introduction and Origin of the Earth
Page 1 of 5 EENS 1110 Tulane University Physical Geology Prof. Stephen A. Nelson Introduction and Origin of the Earth This page last updated on 30-Jul-2015 Geology, What is it? Geology is the study of
Matter. Atomic weight, Molecular weight and Mole
Matter Atomic weight, Molecular weight and Mole Atomic Mass Unit Chemists of the nineteenth century realized that, in order to measure the mass of an atomic particle, it was useless to use the standard