Problem of Time and Background Independence: Classical Version's
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The Homological Kنhler-De Rham Differential Mechanism Part I
Hindawi Publishing Corporation Advances in Mathematical Physics Volume 2011, Article ID 191083, 14 pages doi:10.1155/2011/191083 Research Article The Homological Kahler-De¨ Rham Differential Mechanism part I: Application in General Theory of Relativity Anastasios Mallios and Elias Zafiris Department of Mathematics, National and Kapodistrian University of Athens, Panepistimioupolis, 15784 Athens, Greece Correspondence should be addressed to Elias Zafiris, ezafi[email protected] Received 7 March 2011; Accepted 12 April 2011 Academic Editor: Shao-Ming Fei Copyright q 2011 A. Mallios and E. Zafiris. This is an open access article distributed under the Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. The mechanism of differential geometric calculus is based on the fundamental notion of a connection on a module over a commutative and unital algebra of scalars defined together with the associated de Rham complex. In this communication, we demonstrate that the dynamical mechanism of physical fields can be formulated by purely algebraic means, in terms of the homological Kahler-De¨ Rham differential schema, constructed by connection inducing functors and their associated curvatures, independently of any background substratum. In this context, we show explicitly that the application of this mechanism in General Relativity, instantiating the case of gravitational dynamics, is related with the absolute representability of the theory in the field of real numbers, a byproduct of which is the fixed background manifold construct of this theory. Furthermore, the background independence of the homological differential mechanism is of particular importance for the formulation of dynamics in quantum theory, where the adherence to a fixed manifold substratum is problematic due to singularities or other topological defects. -
Loop Quantum Gravity Alejandro Perez, Centre De Physique Théorique and Université Aix-Marseille II • Campus De Luminy, Case 907 • 13288 Marseille • France
features Loop quantum gravity Alejandro Perez, Centre de Physique Théorique and Université Aix-Marseille II • Campus de Luminy, case 907 • 13288 Marseille • France. he revolution brought by Einstein’s theory of gravity lies more the notion of particle, Fourier modes, vacuum, Poincaré invariance Tin the discovery of the principle of general covariance than in are essential tools that can only be constructed on a given space- the form of the dynamical equations of general relativity. General time geometry.This is a strong limitation when it comes to quantum covariance brings the relational character of nature into our descrip- gravity since the very notion of space-time geometry is most likely tion of physics as an essential ingredient for the understanding of not defined in the deep quantum regime. Secondly, quantum field the gravitational force. In general relativity the gravitational field is theory is plagued by singularities too (UV divergences) coming encoded in the dynamical geometry of space-time, implying a from the contribution of arbitrary high energy quantum processes. strong form of universality that precludes the existence of any non- This limitation of standard QFT’s is expected to disappear once the dynamical reference system—or non-dynamical background—on quantum fluctuations of the gravitational field, involving the dynam- top of which things occur. This leaves no room for the old view ical treatment of spacetime geometry, are appropriately taken into where fields evolve on a rigid preestablished space-time geometry account. But because of its intrinsically background dependent (e.g. Minkowski space-time): to understand gravity one must definition, standard QFT cannot be used to shed light on this issue. -
Who's Afraid of Background Independence?
D. RICKLES WHO’S AFRAID OF BACKGROUND INDEPENDENCE? ABSTRACT: Background independence is generally considered to be ‘the mark of distinction’ of gen- eral relativity. However, there is still confusion over exactly what background independence is and how, if at all, it serves to distinguish general relativity from other theories. There is also some con- fusion over the philosophical implications of background independence, stemming in part from the definitional problems. In this paper I attempt to make some headway on both issues. In each case I argue that a proper account of the observables of such theories goes a long way in clarifying mat- ters. Further, I argue, against common claims to the contrary, that the fact that these observables are relational has no bearing on the debate between substantivalists and relationalists, though I do think it recommends a structuralist ontology, as I shall endeavour to explain. 1 INTRODUCTION Everybody says they want background independence, and then when they see it they are scared to death by how strange it is ... Background independence is a big conceptual jump. You cannot get it for cheap... ([Rovelli, 2003], p. 1521) In his ‘Who’s Afraid of Absolute Space?’ [1970], John Earman defended New- ton’s postulation of absolute, substantival space at a time when it was very un- fashionable to do so, relationalism being all the rage. Later, in his World Enough and Space-Time, he argued for a tertium quid, fitting neither substantivalism nor relationalism, substantivalism succumbing to the hole argument and relational- ism offering “more promissory notes than completed theories” ([Earman, 1989], p. -
Arxiv:1911.01307V1 [Gr-Qc] 4 Nov 2019 What ‘True Names’ This Article Refers to These By
Lie Theory suffices to understand, and Locally Resolve, the Problem of Time Edward Anderson Abstract The Lie claw digraph controls Background Independence and thus the Problem of Time and indeed the Fundamental Nature of Physical Law. This has been established in the realms of Flat and Differential Geometry with varying amounts of extra mathematical structure. This Lie claw digraph has Generator Closure at its centre (Lie brackets), Relationalism at its root (implemented by Lie derivatives), and, as its leaves, Assignment of Observables (zero commutants under Lie brackets) and Constructability from Less Structure Assumed (working if generator Deformation leads to Lie brackets algebraic Rigidity). This centre is enabled by automorphisms and powered by the Generalized Lie Algorithm extension of the Dirac Algorithm (itself sufficing for the canonical subcase, for which generators are constraints). The Problem of Time’s facet ordering problem is resolved. 1 dr.e.anderson.maths.physics *at* protonmail.com 1 Introduction Over 50 years ago, Wheeler, DeWitt and Dirac [6, 4] found a number of conceptual problems with combining General Relativity (GR) and Quantum Mechanics (QM). Kuchař and Isham [11] subsequently classified attempted resolutions of these problems; see [14] for a summary. They moreover observed that attempting to extend one of these Problem of Time facet’s resolution to include a second facet has a strong tendency to interfere with the first resolution (nonlinearity). The Author next identified [15, 20] each facet’s nature in a theory-independent manner. This is in the form of clashes between background-dependent (including conventional QM) and background-independent Physics (including GR). -
Chapter 9: the 'Emergence' of Spacetime in String Theory
Chapter 9: The `emergence' of spacetime in string theory Nick Huggett and Christian W¨uthrich∗ May 21, 2020 Contents 1 Deriving general relativity 2 2 Whence spacetime? 9 3 Whence where? 12 3.1 The worldsheet interpretation . 13 3.2 T-duality and scattering . 14 3.3 Scattering and local topology . 18 4 Whence the metric? 20 4.1 `Background independence' . 21 4.2 Is there a Minkowski background? . 24 4.3 Why split the full metric? . 27 4.4 T-duality . 29 5 Quantum field theoretic considerations 29 5.1 The graviton concept . 30 5.2 Graviton coherent states . 32 5.3 GR from QFT . 34 ∗This is a chapter of the planned monograph Out of Nowhere: The Emergence of Spacetime in Quantum Theories of Gravity, co-authored by Nick Huggett and Christian W¨uthrich and under contract with Oxford University Press. More information at www.beyondspacetime.net. The primary author of this chapter is Nick Huggett ([email protected]). This work was sup- ported financially by the ACLS and the John Templeton Foundation (the views expressed are those of the authors not necessarily those of the sponsors). We want to thank Tushar Menon and James Read for exceptionally careful comments on a draft this chapter. We are also grateful to Niels Linnemann for some helpful feedback. 1 6 Conclusions 35 This chapter builds on the results of the previous two to investigate the extent to which spacetime might be said to `emerge' in perturbative string the- ory. Our starting point is the string theoretic derivation of general relativity explained in depth in the previous chapter, and reviewed in x1 below (so that the philosophical conclusions of this chapter can be understood by those who are less concerned with formal detail, and so skip the previous one). -
A Semifilter Approach to Selection Principles II: Τ
A semifilter approach to selection principles II: τ ∗-covers Lyubomyr Zdomskyy September 3, 2018 Abstract Developing the ideas of [23] we show that every Menger topological space ∗ has the property Sfin(O, T ) provided (u < g), and every space with the ∗ + ℵ0 property Sfin(O, T ) is Hurewicz provided (Depth ([ω] ) ≤ b). Combin- ing this with the results proven in cited literature, we settle all questions whether (it is consistent that) the properties P and Q [do not] coincide, P Q ∗ where and run over Sfin(O, Γ), Sfin(O, T), Sfin(O, T ), Sfin(O, Ω), and Sfin(O, O). Introduction Following [15] we say that a topological space X has the property Sfin(A, B), ω where A and B are collections of covers of X, if for every sequence (un)n∈ω ∈ A there exists a sequence (vn)n∈ω, where each vn is a finite subset of un, such that {∪vn : n ∈ ω}∈B. Throughout this paper “cover” means “open cover” and A is equal to the family O of all open covers of X. Concerning B, we shall also consider the collections Γ, T, T⋆, T∗, and Ω of all open γ-, τ-, τ ⋆, τ ∗-, and ω-covers of X. For technical reasons we shall use the collection Λ of countable large covers. The most natural way to define these types of covers uses the Marczewski “dictionary” map introduced in [13]. Given an indexed family u = {Un : n ∈ ω} of subsets of a set X and element x ∈ X, we define the Marczewski map µu : X → P(ω) arXiv:math/0510484v1 [math.GN] 22 Oct 2005 letting µu(x)= {n ∈ ω : x ∈ Un} (µu(x) is nothing else but Is(x, u) in notations ∗ of [23]). -
Arxiv:1905.10287V2 [Math.GN] 1 Jul 2019 .Bnnig,M Ave 1,M Aa 1]–[8,W Ut ..Miller A.W
Selectors for dense subsets of function spaces Lev Bukovsk´y, Alexander V. Osipov Institute of Mathematics, Faculty of Science, P.J. Saf´arikˇ University, Jesenn´a5, 040 01 Koˇsice, Slovakia Krasovskii Institute of Mathematics and Mechanics, Ural Federal University, and Ural State University of Economics, Yekaterinburg, Russia Abstract ⋆ Let USCp(X) be the topological space of real upper semicontinuous bounded functions defined on X with the subspace topology of the product topology on X R. Φ˜ ↑, Ψ˜ ↑ are the sets of all upper sequentially dense, upper dense or pointwise ⋆ dense subsets of USCp(X), respectively. We prove several equivalent assertions ⋆ ˜ ↑ ˜ ↑ to that that USCp(X) satisfies the selection principles S1(Φ , Ψ ), including a condition on the topological space X. ⋆ We prove similar results for the topological space Cp(X) of continuous bounded functions. ↑ ↑ Similar results hold true for the selection principles Sfin(Φ˜ , Ψ˜ ). Keywords: Upper semicontinuous function, dense subset, sequentially dense subset, upper dense set, upper sequentially dense set, pointwise dense subset, covering propery S1, selection principle S1. 2010 MSC: 54C35, 54C20, 54D55. 1. Introduction We shall study the relationship between selection properties of covers of ⋆ a topological space X and selection properties of dense subsets of the set USCp(X) of all bounded upper semicontinuous functions on X and the set of all bounded ∗ continuous functions Cp (X) on X with the topology of pointwise convergence. arXiv:1905.10287v2 [math.GN] 1 Jul 2019 Similar problems were studied by M. Scheepers [21, 22], J. Haleˇs[7], A. Bella, M. Bonanzinga, M. Matveev [1], M. Sakai [16] – [18], W. -
String Field Theory, Nucl
1 String field theory W. TAYLOR MIT, Stanford University SU-ITP-06/14 MIT-CTP-3747 hep-th/0605202 Abstract This elementary introduction to string field theory highlights the fea- tures and the limitations of this approach to quantum gravity as it is currently understood. String field theory is a formulation of string the- ory as a field theory in space-time with an infinite number of massive fields. Although existing constructions of string field theory require ex- panding around a fixed choice of space-time background, the theory is in principle background-independent, in the sense that different back- grounds can be realized as different field configurations in the theory. String field theory is the only string formalism developed so far which, in principle, has the potential to systematically address questions involv- ing multiple asymptotically distinct string backgrounds. Thus, although it is not yet well defined as a quantum theory, string field theory may eventually be helpful for understanding questions related to cosmology arXiv:hep-th/0605202v2 28 Jun 2006 in string theory. 1.1 Introduction In the early days of the subject, string theory was understood only as a perturbative theory. The theory arose from the study of S-matrices and was conceived of as a new class of theory describing perturbative interactions of massless particles including the gravitational quanta, as well as an infinite family of massive particles associated with excited string states. In string theory, instead of the one-dimensional world line 1 2 W. Taylor of a pointlike particle tracing out a path through space-time, a two- dimensional surface describes the trajectory of an oscillating loop of string, which appears pointlike only to an observer much larger than the string. -
Denumerable Cellular Families in Hausdorff Spaces and Towers Of
Denumerable cellular families in Hausdorff spaces and towers of Boolean algebras in ZF Kyriakos Keremedis, Eliza Wajch Department of Mathematics, University of the Aegean Karlovassi, Samos 83200, Greece [email protected] Institute of Mathematics Faculty of Exact and Natural Sciences Siedlce University of Natural Sciences and Humanities ul. 3 Maja 54, 08-110 Siedlce, Poland [email protected] Orcid: 0000-0003-1864-2303 January 6, 2020 Abstract A denumerable cellular family of a topological space X is an in- finitely countable collection of pairwise disjoint non-empty open sets of X. It is proved that the following statements are equivalent in ZF: arXiv:2001.00619v1 [math.GN] 2 Jan 2020 (i) For every infinite set X, [X]<ω has a denumerable subset. (ii) Every infinite 0-dimensional Hausdorff space admits a denu- merable cellular family. It is also proved that (i) implies the following: (iii) Every infinite Hausdorff Baire space has a denumerable cellular family. Among other results, the following theorems are also proved in ZF: (iv) Every countable collection of non-empty subsets of R has a choice function iff, for every infinite second-countable Hausdorff space 1 X, it holds that every base of X contains a denumerable cellular family of X. (v) If every Cantor cube is pseudocompact, then every non-empty countable collection of non-empty finite sets has a choice function. (vi) If all Cantor cubes are countably paracompact, then (i) holds. Moreover, among other forms independent of ZF, a partial Kinna- Wagner selection principle for families expressible as countable unions of finite families of finite sets is introduced. -
Loop Quantum Gravity
QUANTUM GRAVITY Loop gravity combines general relativity and quantum theory but it leaves no room for space as we know it – only networks of loops that turn space–time into spinfoam Loop quantum gravity Carlo Rovelli GENERAL relativity and quantum the- ture – as a sort of “stage” on which mat- ory have profoundly changed our view ter moves independently. This way of of the world. Furthermore, both theo- understanding space is not, however, as ries have been verified to extraordinary old as you might think; it was introduced accuracy in the last several decades. by Isaac Newton in the 17th century. Loop quantum gravity takes this novel Indeed, the dominant view of space that view of the world seriously,by incorpo- was held from the time of Aristotle to rating the notions of space and time that of Descartes was that there is no from general relativity directly into space without matter. Space was an quantum field theory. The theory that abstraction of the fact that some parts of results is radically different from con- matter can be in touch with others. ventional quantum field theory. Not Newton introduced the idea of physi- only does it provide a precise mathemat- cal space as an independent entity ical picture of quantum space and time, because he needed it for his dynamical but it also offers a solution to long-stand- theory. In order for his second law of ing problems such as the thermodynam- motion to make any sense, acceleration ics of black holes and the physics of the must make sense. -
STAR SELECTION PRINCIPLES: a SURVEY 1. Introduction There Are
Khayyam J. Math. 1 (2015), no. 1, 82{106 STAR SELECTION PRINCIPLES: A SURVEY LJUBISAˇ D.R. KOCINACˇ Communicated by H.R. Ebrahimi Vishki Abstract. We review selected results obtained in the last fifteen years on star selection principles in topology, an important subfield of the field of selection principles theory. The results which we discuss concern also uniform structures and, in particular, topological groups and their generalizations. 1. Introduction There are many results in the literature which show that a number of topolog- ical properties can be characterized by using the method of stars. In particular it is the case with many covering properties of topological spaces. The method of stars has been used to study the problem of metrization of topological spaces, and for definitions of several important classical topological notions. More infor- mation on star covering properties can be found in [17], [45]. We use here such a method in investigation of selection principles for topological and uniform spaces. Although Selection Principles Theory is a field of mathematics having a rich his- tory going back to the papers by Borel, Menger, Hurewicz, Rothberger, Seirpi´nski in 1920{1930's, a systematic investigation in this area rapidly increased and attracted a big number of mathematicians in the last two-three decades after Scheeper's paper [54]. Nowadays, this theory has deep connections with many branches of mathematics such as Set theory and General topology, Game theory, Ramsey theory, Function spaces and hyperspaces, Cardinal invariants, Dimension theory, Uniform structures, Topological groups and relatives, Karamata theory. Researchers working in this area have organized four international mathemati- cal forums called \Workshop on Coverings, Selections and Games in Topology". -
Non-Standard Solutions to the Euler System of Isentropic Gas Dynamics
NON-STANDARD SOLUTIONS TO THE EULER SYSTEM OF ISENTROPIC GAS DYNAMICS Dissertation zur Erlangung der naturwissenschaftlichen Doktorw¨urde (Dr. sc. nat.) vorgelegt der Mathematisch-naturwissenschaftlichen Fakult¨at der Universit¨atZ¨urich von ELISABETTA CHIODAROLI von Italien Promotionskomitee Prof. Dr. Camillo De Lellis (Vorsitz) Prof. Dr. Thomas Kappeler Z¨urich, 2012 Abstract This thesis aims at shining some new light on the terra incognita of multi-dimensional hyperbolic systems of conservation laws by means of techniques new for the field. Our concern focuses in particular on the isentropic compressible Euler equations of gas dynamics, the oldest but yet most prominent paradigm for this class of equations. The theory of the Cauchy problem for hyperbolic systems of conservation laws in more than one space dimension is still in its dawning and has been facing some basic issues so far: do there exist weak solutions for any initial data? how to prove well-posedness for weak solutions? which is a good space for a well-posedness theory? are entropy inequalities good selection criteria for uniqueness? Inspired by these interesting ques- tions, we obtained some new results here collected. First, we present a counterexample to the well-posedness of entropy solutions to the multi-dimensional compressible Euler equations: in our construction the entropy condition is not sufficient as a selection criteria for unique solutions. Furthermore, we show that such a non-uniqueness theorem holds also for a classical Riemann datum in two space dimensions. Our results and constructions build upon the method of convex integration developed by De Lellis-Sz´ekelyhidi [DLS09, DLS10] for the incom- pressible Euler equations and based on a revisited "h-principle".