DOCSLIB.ORG

Properties of Matter

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Properties of Matter Properties of Matter What is matter? Matter is anything that takes up space!!! What are the three states of matter??? The three states of matter are solids, liquids, and gases! States of Matter Gases, liquids and solids are all made up of microscopic particles, but the behaviors of these particles differ in the three phases. The following figure illustrates the microscopic differences. Microscopic view of a Microscopic view of a Microscopic view of a gas. liquid. solid. Note that: Particles in a: o gas are well separated with no regular arrangement. o liquid are close together with no regular arrangement. o solid are tightly packed, usually in a regular pattern. Particles in a: o gas vibrate and move freely at high speeds. o liquid vibrate, move about, and slide past each other. o solid vibrate (jiggle) but generally do not move from place to place. Liquids and solids are often referred to as condensed phases because the particles are very close together. The following table summarizes properties of gases, liquids, and solids and identifies the microscopic behavior responsible for each property. Some Characteristics of Gases, Liquids and Solids and the Microscopic Explanation for the Behavior gas liquid solid assumes the shape and assumes the shape of retains a fixed volume volume of its the part of the and shape container container which it rigid - particles locked particles can move past occupies into place one another particles can move/slide past one another compressible not easily not easily lots of free space compressible compressible between particles little free space little free space between particles between particles flows easily flows easily does not flow easily particles can move past particles can rigid - particles cannot one another move/slide past one move/slide past one another another In shortly speak: Solid state Solids have three main properties: 1. It has a definite shape. 2. It has a definite mass. 3. It has a definite volume. This means that a solid will always look the same, take up the same amount of space, and have the same amount of molecules in it. Liquid state Liquids have three main properties: 1. It does not have a definite shape. 2. It has a definite mass. 3. It has a definite volume. This means that liquids will always take up the same amount of space and have the same amount of molecules in it. However, because it does not have a definite shape, it takes the shape of its container. Gas state Gases have three main properties: 1. It does not have a definite shape. 2. It does not have a definite mass. 3. It does not have a definite volume. This means that a gas does not always take up the same amount of space, nor does it weigh the same all the time. Like liquids, gases take the shape of their containers. However, they will fill the space they are given. That is why they don't always take up the same amount of space!! properties of matter There are four different properties of matter. They are weight, volume, mass, and density. Mass The most important one is mass. Mass is the amount of matter in an object and it never changes unless matter is taken out of the object. Mass also has a direct relationship with inertia. Inertia is the resistance of motion of an object. If an object has a greater mass, then it has a greater inertia. Also, you can find mass by measuring it on a triple beam balance. (Q)Does the man on top of Mount Everest have a greater or lesser mass then he would in Death Valley? Volume Volume is another general property of matter. Anything that takes up space has volume. In fact, volume is the amount of space an object takes up. You can find a straight-edged object's volume by measuring the Length x Width x Height. For irregular shaped objects, you'd probably want to use a graduated cylinder. Liters and milliliters are used to measure the volume of liquids, while cubic centimeters are used to measure solids. (Q)If the cube is 5cm long, 5cm wide, and 5cm tall; what is the volume of the object? Density The third general property of matter is density. Density is very important because it enables you to compare different objects. For instance, water has a density of 1 gram/cc and wood is 0.8 grams/cc. Therefore, wood will float in water because it's density is less than that of water. The equation for density is Density=Mass/Volume. Also, if you split an object in half, it will still have the exact same density. (Q)If the mass of the car is 2000kg, and the volume is 1000cc, then what is the density? (A)The density would be 2kg/cc. Don't forget, density equals mass divided by volume. Weight Weight is the fourth general property of matter. It is defined as the measure of force of attraction between objects due to gravity. Gravity is what keeps you and me on the ground. In fact, gravity exists between you and your computer. You are attracted to it by gravity. You don't feel the attraction because the computer's mass is so small. The earth, on the other hand has a very large mass. That's why you are attracted to the ground. Weight, unlike mass, changes with location. The farther you are from the center of the Earth, the less you weigh. The metric unit for weight is the Newton, even though in America the most common unit is the pound. The equation for weight is Weight=Mass x Acceleration due to gravity, but I personally think the easiest one is for every kilogram of mass, there's 9.8 Newton of weight. (Q)If the mass of buck is 125kg, then what is the weight in newtons on Earth? (A)It would weigh 1,225N. This is because there's 9.8 newtons on Earth for every one kilogram. PROPERTIES OF MATTER - CHEMICAL AND PHYSICAL Physical properties - depends only upon matter itself, the identity of the substance does not change. Physical properties can be measured using physical senses. Examples: color, mass, size, density, magnetic, melting point, boiling point, texture, shape. Chemical properties - those things that describe the events which occur when two materials react with each other. Examples: Was heat, light, sound, or some other form of energy generated? Did a reaction take place at all (if not, the materials are non-reactive - which is a chemical property)? Were gases formed? Was it endothermic or exothermic? The chemical properties of an element are determined by the number of valence electrons it has. Example: a rusting nail 4 Fe + 3 O2 --------> 2 Fe2O3 iron oxygen iron(III) oxide New substance formed which has its own set of physical and chemical properties, but, can be broken back down into the elements which formed it. Intensive Versus Extensive Properties Physical properties of matter are categorized as either Intensive or Extensive: o Intensive - Properties that do not depend on the amount of the matter present. Color . Odor . Luster - How shiny a substance is. Malleability - The ability of a substance to be beaten into thin sheets. Ductility - The ability of a substance to be drawn into thin wires. Conductivity - The ability of a substance to allow the flow of energy or electricity. Hardness - How easily a substance can be scratched. Melting/Freezing Point - The temperature at which the solid and liquid phases of a substance are in equilibrium at atmospheric pressure. Boiling Point - The temperature at which the vapor pressure of a liquid is equal to the pressure on the liquid (generally atmospheric pressure). Density - The mass of a substance divided by its volume o Extensive - Properties that do depend on the amount of matter present. Mass - A measurement of the amount of matter in a object (grams). Weight - A measurement of the gravitational force of attraction of the earth acting on an object. Volume - A measurement of the amount of space a substance occupies. Length CHANGES IN MATTER - PHYSICAL AND CHEMICAL Physical change: change in physical properties - a change in shape, size, or state without a change in actual composition. - it involves changes in one or more physical properties of a substance but not in the identifying chemical properties or molecular composition of the substance. - Example: breaking a rock, melting ice, evaporation, freezing water. Chemical change: Change in which a substance becomes another substance with different properties. - Example: souring of milk, silver tarnishing, electrolysis of water - an energy change always accompanies a chemical change - loss or gain of heat, light, or some other form of energy. Physical Changes . Changes in matter that do not alter the identity of the matter itself. For example: 1. Size 2. Shape 3. State - solid liquid gas 4. Dilutions Chemical Changes 3. Changes that do alter the identity of a substance. 4. For example: 1. Iron rusting 4 Fe(s) + 3 O2(g) 2 Fe2O3 � 3 H2O 2. Wood burning 3. Copper turning to brass KINETIC THEORY OF MATTER To understand the different states in which matter can exist, we need to understand something called the Kinetic Molecular Theory of Matter. Kinetic Molecular Theory has many parts, but we will introduce just a few here. One of the basic concepts of the theory states that atoms and molecules possess an energy of motion that we perceive as temperature. In other words, atoms and molecules are constantly moving, and we measure the energy of these movements as the temperature of the substance.
Load more

Recommended publications
  • Neutron Stars and Strange Matter Bnl—39402 De37 006746 J
    NEUTRON STARS AND STRANGE MATTER BNL—39402 DE37 006746 J. Cooperstein* Brookhaven National Laboratory, Upton NY 11973 and SUNY at Stony Brook NY 11794 We investigate the likelihood that quark matter with strangeness of order unity resides in neutron stars. In the strong coupling regime near Po this is found to be unlikely. Considering higher densities where perturbative expansions are used, we find a lower bound to be at 7p0 for the transition density. This is higher than the inferred density of observed neutron stars, and thus the transition to quark matter is precluded. I. Introduction We will deal with the question: does bulk strange matter exist in nature? For this we will draw upon our recent investigation of this subject done in collaboration with Hans Bethe and Gerry Brown1. Strange matter is usually taken to mean deconfined i .lark matter with strangeness of order unity. If such material exists in the universe today, the core of neutron stars is the oi?ly reasonable place to search for it in the bulk. Observationally the problem is difficult. We know that all well measured neutron stars have masses in the range 1.4 ~ M/MQ ~ 1.6, so we have at least a lower limit to the maximum mass. As far as an upper limit is concerned one might be tempted to believe it is not much higher than the above range for two reasons. First there is the fact that Type II supernovae calculations always tend to leave behind a mass at the lower end of the above range, since this is about the iron core mass of the presupernova star, and the explosion should sweep out almost all of the overlying burning shells.
    [Show full text]
  • Arxiv:Astro-Ph/9702189V1 21 Feb 1997 90.Tetertclpeitosaecmae Ihtebo the with Compared Al
    Differences in the Cooling Behavior of Strange Quark Matter Stars and Neutron Stars Christoph Schaab1, Bernd Hermann, Fridolin Weber and Manfred K. Weigel Institut f¨ur theoretische Physik, Ludwig-Maximilians Universit¨at M¨unchen, Theresienstr. 37, D-80333 M¨unchen, Germany ABSTRACT The general statement that hypothetical strange (quark matter) stars cool more rapidly than neutron stars is investigated in greater detail. It is found that the direct Urca process could be forbidden not only in neutron stars but also in strange stars. In this case, strange stars are slowly cooling, and their surface temperatures are more or less indistinguishable from those of slowly cooling neutron stars. Furthermore the case of enhanced cooling is reinvestigated. It shows that strange stars cool significantly more rapidly than neutron stars within the first ∼ 30 years after birth. This feature could become particularly interesting if continued observation of SN 1987A would reveal the temperature of the possibly existing pulsar at its center. Subject headings: stars: evolution – stars: neutron 1. Introduction The theoretical possibility that strange quark matter – made up of roughly equal numbers of up, down and strange quarks – may be more stable than atomic nuclei (specifically iron, which is arXiv:astro-ph/9702189v1 21 Feb 1997 the most stable atomic nucleus) constitutes one of the most startling predictions of modern physics (see Bodmer 1971, Witten 1984, Terazawa 1989), which, if true, would have implications of greatest importance for laboratory physics, cosmology, the early universe, its evolution to the present day, and massive astrophysical objects (cf. Madsen & Haensel 1991). Unfortunately it seems unlikely that lattice QCD calculations will be accurate enough in the foreseeable future to give a definitive prediction on the absolute stability of strange matter, so that one is presently left with experiments and astrophysical studies (cf.
    [Show full text]
  • Strange Quark Matter in Neutron Stars
    Strange quark matter in neutron stars Prof. Mark Alford Washington University in St. Louis SQM 2013 Schematic QCD phase diagram T heavy ion collider QGP non−CFL hadronic = color− superconducting gas liq CFL quark matter nuclear compact star µ superfluid /supercond M. Alford, K. Rajagopal, T. Sch¨afer, A. Schmitt, arXiv:0709.4635 (RMP review) A. Schmitt, arXiv:1001.3294 (Springer Lecture Notes) Quark matter in compact stars Conventional scenario Strange Matter Hypothesis Bodmer 1971; Witten 1984; Farhi, Jaffe 1984 Neutron/hybrid star Strange star nuclear crust nuclear crust neutron NM star SQM SQM strangelet NM crust hybrid star SQM SQM Two scenarios for quark matter Conventional scenario Strange Matter Hypothesis Vac!NM!QM Vac!QM p QM NM p QM NM pcrit vac vac µ µcrit µ 310 MeV 310MeV µsqm Nuclear!quark matter transition Vacuum!quark matter transition at high pressure, (µcrit, pcrit) at µ = µsqm, p = 0. Strange quark matter (SQM) is the favored phase down to p = 0. Stars under the Strange Matter Hypothesis nuclear crust SQM SQM strangelet crust SQM Strangelet crust At zero pressure, if its surface tension is low enough, strange matter, like nuclear matter, will undergo charge separation and evaporation in to charged droplets. neutral −2 vacuum σcrit . 10 MeVfm e e Crust thickness neutral e e ∆R . 1 km SQM Alford, Eby, arXiv:0808.0671 neutral SQM Jaikumar, Reddy, Steiner, nucl-th/0507055 Charge separation: a generic feature charge−separated dΩ phase charge density ρ = Ω = dµe p neutral neutral vacuum SQM Neutral quark matter and µe neutral vacuum can coexist at zero pressure.
    [Show full text]
  • Strangelets and Strange Quark Matter
    View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by CERN Document Server 1 LBNL-40988 Strangelets and Strange Quark Matter J¨urgen Schaffner-Bielicha ∗ aNuclear Science Division, Lawrence Berkeley National Laboratory, University of California, Berkeley, CA 94720 I summarize the properties of finite lumps of strange quark matter (strangelets) with emphasis on the two scenarios of producing strange matter in relativistic heavy ion col- lisions. As an outlook, I discuss the possibility of short-lived strange composites and charmed matter. 1. INTRODUCTION – PRODUCING STRANGE MATTER IN THE LAB- ORATORY As it has been discussed widely during this conference, strangeness opens a new dimen- sions to nuclear physics. Insofar, systems with strangeness number S = −1, −2 have been discussed. Here we want to examine the unknown domain of finite nuclear systems with S<−2. There have been speculations about the existence of finite systems of strange quark matter (strangelets) and strange hadronic matter. Here we will focus on the former objects and recent progress in this field [1] as the latter ones were discussed at the last hypernuclear meeting in detail [2]. How can one produce such strangeness-rich systems? Hadron beams enable only to explore systems up to S = −2. Nevertheless, relativistic truly heavy-ion collisions constitute a prolific source of strangeness as dozens of hyperons are produced on a single central event. In principle, strangelets can be produced via two different scenarios: by a coalescence of hyperons or by a distillation of a quark-gluon plasma. The coalescence model for strangelet production in heavy-ion collisions has been put forward by Carl Dover [3].
    [Show full text]
  • The Physics and Astrophysics of Strange Matter
    The Physics and Astrophysics of Strange Matter 1. INTRODUCTION It is generally believed that if a nucleus or collection of nuclei is subjected to a high enough pressure, a transition to quark matter occurs. 1 Above a critical pressure, Pn individual nucleon bound­ aries dissolve and a system with baryon number A is best described as 3A quarks and not as A nucleons. The quarks are still confined to the system as a whole but they are no longer parts of three quark units. In this quark matter phase, quarks have very different wave functions than they do in nuclei, and hadrons, as we know them, do not exist. The scale of the strong interactions, A, is roughly mproton/3 or 300 MeV. On this scale the up and down quark masses are neg­ ligible and it is reasonable to assume that the transition pressure, Pc, is characterized by A. If we think of a system under a pressure just above Pc as a Fermi gas of 3A quarks (assume A is large), then the chemical potentials of the quarks are of order A. The mass of the strange quark, m, is not well determined but is usually taken to be between 50 Me V and 300 Me V. I will assume that m is com­ fortably below the chemical potentials of the quarks just considered. In this case, weak interactions such as u + d ~ u + s or u ~ s + e+ + v will convert up and down quarks to strange quarks. The system will lower its energy (more precisely its Gibbs po­ tential) by distributing its quarks in three Fermi seas instead of Comments Nucl.
    [Show full text]
  • Strange Matter in Compact Stars
    EPJ Web of Conferences 171, 08001 (2018) https://doi.org/10.1051/epjconf/201817108001 SQM 2017 Strange matter in compact stars Thomas Klähn1,2, and David B. Blaschke2,3,4, 1Department of Physics and Astronomy, California State University Long Beach, California 90840, U.S.A 2Institute of Theoretical Physics, University of Wrocław, pl. M. Borna 9, 50-204 Wroclaw, Poland 3Bogoliubov Laboratory of Theoretical Physics JINR Dubna, Joliot-Curie str. 6, 141980 Dubna, Russia 4National Research Nuclear University (MEPhI), Kashirskoe Shosse 31, 115409 Moscow, Russia Abstract. We discuss possible scenarios for the existence of strange matter in compact stars. The appearance of hyperons leads to a hyperon puzzle in ab-initio approaches based on effective baryon-baryon potentials but is not a severe problem in relativistic mean field models. In general, the puzzle can be resolved in a natural way if hadronic matter gets stiffened at supersaturation densities, an effect based on the quark Pauli quenching be- tween hadrons. We explain the conflict between the necessity to implement dynamical chiral symmetry breaking into a model description and the conditions for the appear- ance of absolutely stable strange quark matter that require both, approximately massless- ness of quarks and a mechanism of confinement. The role of strangeness in compact stars (hadronic or quark matter realizations) remains unsettled. It is not excluded that strangeness plays no role in compact stars at all. To answer the question whether the case of absolutely stable strange quark matter can be excluded on theoretical grounds requires an understanding of dense matter that we have not yet reached.
    [Show full text]
  • “Unmatter,” As a New Form of Matter, and Its Related “Un-Particle,” “Un-Atom,” “Un-Molecule”
    “Unmatter,” as a new form of matter, and its related “un-particle,” “un-atom,” “un-molecule” Florentin Smarandache has introduced the notion of “unmatter” and related concepts such as “unparticle,” “unatom,” “unmolecule” in a manuscript from 1980 according to the CERN web site, and he uploaded articles about unmatter starting with year 2004 to the CERN site and published them in various journals in 2004, 2005, 2006. In short, unmatter is formed by matter and antimatter that bind together. The building blocks (most elementary particles known today) are 6 quarks and 6 leptons; their 12 antiparticles also exist. Then unmatter will be formed by at least a building block and at least an antibuilding block which can bind together. Keywords: unmatter, unparticle, unatom, unmolecule Abstract. As shown, experiments registered unmatter: a new kind of matter whose atoms include both nucleons and anti-nucleons, while their life span was very short, no more than 10-20 sec. Stable states of unmatter can be built on quarks and anti-quarks: applying the unmatter principle here it is obtained a quantum chromodynamics formula that gives many combinations of unmatter built on quarks and anti-quarks. In the last time, before the apparition of my articles defining “matter, antimatter, and unmatter”, and Dr. S. Chubb’s pertinent comment on unmatter, new development has been made to the unmatter topic in the sense that experiments verifying unmatter have been found.. 1. Definition of Unmatter. In short, unmatter is formed by matter and antimatter that bind together. The building blocks (most elementary particles known today) are 6 quarks and 6 leptons; their 12 antiparticles also exist.
    [Show full text]
  • Does Cygnus X-3 Contain a Strange Neutron Star?
    eep underground proton-decay charge must be zero; otherwise the direc- a sufficiently long lifetime, of order a year detectors in the Soudan iron mine tionality and timing of the signal would be in its rest frame, that it not decay en route D in Minnesota and under the Mont destroyed by galactic magnetic fields. from the source. (Lorentz dilation in- Blanc have recorded very energetic muons Secondly, the mass of the primary must be creases the observed lifetime of a rapidly coming from the direction of Cygnus X-3 less than its energy by a factor of about 104; moving particle by the ratio of its energy with its 4.79-hour periodicity. These ob- otherwise differences in travel times of to its mass.) The known neutral particles servations, if confirmed, present a very primaries with different energies would with such properties are photons, neu- challenging puzzle. What is the primary wash out the periodicity of the primaries trinos, and neutrons, but arguments cosmic-ray particle that produces the and hence that of the muons. (A 1OO-GeV- presented in the main text appear to rule muons at the earth, and how is such a mass particle, for example, would arrive these out. Briefly, the reported flux of particle produced in Cygnus X-3? One of about 1 hour sooner if it had an energy of muons is too high to be attributed to the more coherent explanations is that the 12 TeV than if it had an energy of 10 TeV gamma rays (high-energy photons), the primaries originate as exotic hadrons (1 GeV = 109 eV and 1 TeV = 1012 eV).) observed dependence of the muon flux on (strongly interacting particles, not yet To produce muons with sufficient energy zenith angle rules out neutrinos, and neu- made in laboratories) chipped off the neu- to penetrate the overlying rock and reach trons would decay in flight unless their tron star in Cygnus X-3, a star itself made the great depths of the detectors (equiva- energy was unacceptably large.
    [Show full text]
  • Astrophysical Relevance of Strange Quarks
    Available online a t www.scholarsresearchlibrary.com Scholars Research Library Archives of Physics Research, 2010, 1 (3):89-110 (http://scholarsresearchlibrary.com/archive.html) ISSN 0976-0970 CODEN (USA): APRRC7 Astrophysical relevance of Strange Quarks Navjot Hothi† and Shuchi Bisht * Department of Physics, Kumaun University, Nainital, Uttrakhand, India ______________________________________________________________________________ ABSTRACT In this contribution, peculiarities in the nature of strange quarks in relevance to astrophysics are investigated. The absolute stability of strange quark matter is a viable possibility and immensely affects physics at the astrophysical scale. Relativistic heavy-ion reactions offer a stage to produce this exotic state of matter and we have discussed the enhanced production of strange particles during these reactions within the framework of quark-gluon plasma (QGP) along with its observable implications. The role of strangeness for compact star phenomenology is explored. Emphasis is laid upon the possibility of existence of a third family of strange quark stars and its study help in revealing a number of unexplored features of the cosmos. Bag model parameters have been used to determine some integral parameters for a sequence of strange stars with crust and strange dwarfs constructed out of strange quark matter crust. A comparative analysis is performed between the strange and neutron stars and the strange and white dwarfs based upon these intrinsic parameters and paramount differences are observed. PACS numbers: 12.38.Mh, 25.75.Nq, 14.65.-q, 97.60.Jd, 26.60.-c Keywords: strangeness, strange stars, quark-gluon plasma, deconfinement. ______________________________________________________________________________ INTRODUCTION The last few years witnessed the inclusion of strangeness as another degree of freedom in astrophysical systems.
    [Show full text]
  • Engineering with Quark Matter Beams of '"U and Zospb Nuclei
    ~N~AT_U~R~E~v_o_L_._33_7_2_FE_B_R_u_A_R_Y_I9_H_9 ________________ NEVVSAN0VI8NS------------------------------------~~~5 Nuclear physics quark nuggets has been used by Brugger et al. \ who have adapted Rutherford scat­ tering, bombarding material samples with Engineering with quark matter beams of '"U and zospb nuclei. Any back­ scattering of the beams by angles greater Charles Alcock than 90° indicates the presence of scatter­ ing centres (the nuggets) more massive THE possibility that small drops of 'quark these collapsed stars, but some argue that than the projectile nuclei. matter' might be stable was first put strange matter is. For his proposal, Brugger et al. applied this elegant tech­ forward by Witten'. More detailed cal­ Madsen adduces the conclusion of Alpar' nique to various natural samples (includ­ culations by Farhi and Jaffe' showed that that the radio pulsars which exhibit glitches ing a meteorite) and derive upper limits to the hypothesis was certainly plausible; (abrupt, very small period reductions the abundance of quark nuggets: 1 per 1010 also these authors named stable quark followed by a few months of relaxation) for nuggets with A=l03 down to 1 per 1014 matter 'strange matter' because of the must be made of neutron matter, not at A=10'. The technique is less readily important role played by strange quarks, a stange matter. This conclusion rests on the applied for higher atomic number because name which has stuck. The strange-matter success of neutron-star models for the the electrostatic potential of the nuggets is hypothesis has several interesting con­ glitch phenomenon and the absence of a not a simple Coulomb form.
    [Show full text]
  • Teacher's Guide
    TEACHER’S GUIDE TABLE OF CONTENTS Letter to Teachers ................................................................................................................................. 3 Matrix of Activity Curriculum Connections .............................................................................................. 4 The Exhibits of STRANGE MATTER .............................................................................................................. 7 What is Materials Science? ........................................................................................................................ 8 ACTIVITIES MY MATTER / The Investigator’s Challenge Teacher’s Notes ....................................................................................................................... 10 Student Activity ....................................................................................................................... 14 MAGNETIC MATTER / The Astronaut’s Challenge Teacher’s Notes ....................................................................................................................... 17 Student Activity ....................................................................................................................... 21 SLIMY MATTER / The Toy Designer’s Challenge Teacher’s Notes ...................................................................................................... 25 Student Activity ...................................................................................................... 31
    [Show full text]
  • Relativistic Simulations of Compact Object Mergers for Nucleonic Matter and Strange Quark Matter
    Technische Universit¨at M¨unchen Physik Department Max-Planck-Institut f¨ur Astrophysik Relativistic simulations of compact object mergers for nucleonic matter and strange quark matter Andreas Ottmar Bauswein Vollst¨andiger Abdruck der von der Fakult¨at f¨ur Physik der Technische Universit¨at M¨unchen zur Erlangung des akademischen Grades eines Doktors der Naturwissenschaften (Dr. rer. nat.) genehmigten Dissertation. Vorsitzender: Univ.-Prof. Dr. R. Kr¨ucken Pr¨ufer der Dissertation: 1. Priv.-Doz. Dr. H.-Th. Janka 2. Univ.-Prof. Dr. W. Weise Die Dissertation wurde am 25.11.2009 bei der Technischen Universit¨at M¨unchen eingereicht und durch die Fakult¨at f¨ur Physik am 29.01.2010 angenommen. Diese Arbeit ist meinen Eltern Maria und Ottmar gewidmet. 3 Contents 1. Introduction 7 1.1. Physicalcontext................................ 7 1.2. Observational consequences . ... 9 1.2.1. Gravitational-wavesignals . .. 9 1.2.2. Gamma-raybursts .. .. .. 10 1.2.3. Nucleosynthesis aspects . 11 1.2.4. Signaturesofstrangequarkmatter . .. 11 1.3. Modelingcompactstarmergers . .. 12 1.4. Neutronstar-blackholemergers . .... 14 1.5. Goalsandoutlineofthethesis. ... 15 1.6. Conventionsandnotations . .. 16 2. Physical model and numerical implementation 17 2.1. Relativistic smooth particle hydrodynamics and the conformal flatness approximation................................. 17 2.1.1. Initialdata .............................. 22 2.2. Simulating neutron star-black hole mergers . ........ 22 2.2.1. Black holes in numerical relativity . .... 23 2.2.2. Puncture black hole in the conformal flatness approach...... 25 2.2.3. Further aspects of simulating black holes . ..... 29 3. Equation of state of high-density matter 33 3.1. Nuclearequationsofstate . .. 33 3.2. Strangequarkmatterequationsofstate . ..... 35 3.3. Thermodynamical properties and stellar structure .
    [Show full text]