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Table Of Integrals Series And Products

본 연구는 현존하는 여덟 개의 〈뿔피리를 부는 제빵사〉 작품이 산발적으로 우연히 등장한 것이 아닌 서로 유기적인 영향관계를 주고 받으며 생산된 하나의 도상으로 살펴보았다. “뿔피리를 부는 제빵사” 그림에 대한 현재까지의 연구는 대부분 그림에 나타나 있는 다양한 빵들을 성만찬을 의미하는 종교적 상징으로 해석하고 있다. 이에 반해 본 연구는 “뿔피리를 부는 제빵사” 도상이 유독 17세기 중후반 네덜란드에서 생산된 사실에 주목하고, 그 이유를 동시대 네덜란드인들의 일상에 직접적인 영향을 주었던 빵의 생산 및 공급 그리고 유통과정에서 찾고자 한다. 여기에는 빵이 당대 네덜란드인들의 식생활 뿐 아니라 그들의 경제생활 더나아가 국가경제 전체에 어떤 중요한 역할을 했는지에 대한 연구가 선행되어야 한다. 주로 풍속화의 전통으로 해석되었던 “뿔피리를 부는 제빵사” 그림은 본 연구에서 풍속화와 초상화 두 장르가 혼합한 도상으로 다루어졌으며, 이제까지의 연구에서 미흡했던 초상화로서의 가능성이 적극적으로 제기되었다. 제빵사의 초상화 또는 화가의 자화상으로 생산된 〈뿔피리를 부는 제빵사〉의 시대적 배경에는 제빵사의 경제적 여유와 사회적 지위상승 그리고 제빵사를 영혼의 양식을 공급하는 고귀한 직업으로 승화시킨 칼비니즘의 영향이 있다. 제빵사들이 부를 축적할 수 있었던 배경에는 국가가 나서서 빵의 생산과 공급을 철저하게 관리해준 덕분이었다. 17세기 네덜란드의 제빵사들은 길드에 속해야만 빵을 팔 수 있었고 각 제빵사들의 빵 만드는 법은 외부인들에게 절대로 공개되지 않았다. 동시에 당시 네덜란드인들은 세금을 내지 않고는 빵을 먹기가 힘들었다. 이런 이유로 개인의 집에 오븐을 설치하는 것은 금지되었고, 빵은 꼭 관헌들에게 세금을 내는 합법적인 제빵사에게서만 살 수 있었다. 이렇게 17세기 네덜란드는 직업으로서 빵 굽는 사람을 보호하는 동시에 단속하기 위해 매우 엄격한 규정을 제정하였다. 17세기 네덜란드인들에게 빵은 그들의 식생활 뿐 아니라 그들의 다양한 직업과도 관련이 있었으며 빵의 생산과 유통과정에 개입한 국가의 권위와 통제를 상징하기도 한다. 빵의 생산과 유통에 붙는 세금은 국가의 경제를 지탱하고 발전시키는데 중요한 재원이었으며, 동시에 국민들을 엄격하게 관리함으로써 국가의 질서를 세우기 위한 효과적인 방편이었다. 빵가격은 변동이 심한 곡물가격과 빵의 크기에 따라서 엄격하게 결정되었다. 네덜란드정부는 평상시에 빵의 공식적인 무게와 가격을 고정시켰는데, 이는 다른 음식에서는 찾아볼 수 없는 유일한 관리방식이었다. 따라서 동시대 네덜란드인들에게 빵은 국가의 적극적인 개입과 관리체계를 통해서만 그들의 입에 넣을 수 있는 음식이었다. 이러한 맥락에서 볼 때, 본 연구에서 다룬 〈뿔피리를 부는 제빵사〉 그림에서 풍성하게 차려진 다양한 빵은 경제적인 풍요와 정치적인 안정을 의미한다. 여러 가지 다양한 음식 중에서도 빵이 이러한 의미를 가장 효과적으로 전달한다는 점에서 〈뿔피리를 부는 제빵사〉 그림에서 빵은 당시 네덜란드의 물질적 풍요뿐만 아니라 국가의 번영과 안녕을 의미한다고 볼 수 있다.

17세기 네덜란드 미술에 나타난 빵의 사회사

Traversable wormholes, tunnel-like structures introduced by Morris and Thorne [Am. J. Phys. 56 (1988) 395], have a significant role in connection of two different spacetimes or two different parts of the same spacetime. The characteristics of these wormholes depend upon the redshift and shape functions which are defined in terms of radial coordinate. In literature, several shape functions are defined and wormholes are studied in f(R) gravity with respect to these shape functions [F. S. N. Lobo and M. A. Oliveira, Phys. Rev. D 80 (2009) 104012; H. Saiedi and B. N. Esfahani, Mod. Phys. Lett. A 26 (2011) 1211; S. Bahamonde, M. Jamil, P. Pavlovic and M. Sossich, Phys. Rev. D 94 (2016) 044041]. In this paper, two shape functions (i) b(r) = r0log(r+1) log(r0+1) and (ii) b(r) = r0( r r0 )γ, 0 < γ < 1, are considered. The first shape function is newly defined, however, the second one is collected from the literature [M. Cataldo, L. Liempi and P. Rodriguez, Eur. Phys. J. C 77 (2017) 748]. The wormholes are investi...

Traversable wormholes and energy conditions with two different shape functions in f(R) gravity

Teleparallel gravity has significantly increased in popularity in recent decades, bringing attention to Einstein's other theory of gravity. In this Review, we relate this form of geometry to the broader metric-affine approach to forming gravitational theories where we describe a systematic way of constructing consistent teleparallel theories that respect certain physical conditions such as local Lorentz invariance. We first use teleparallel gravity to formulate a teleparallel equivalent of general relativity which is dynamically equivalent to general relativity but which may have different behaviors for other scenarios, such as quantum gravity. After setting this foundation, we describe the plethora of modified teleparallel theories of gravity that have been proposed in the literature. In the second part of the Review, we first survey works in teleparallel astrophysics literature where we focus on the open questions in this regime of physics. We then discuss the cosmological consequences for the various formulations of teleparallel gravity. We do this at background level by exploring works using various approaches ranging from dynamical systems to Noether symmetries, and more. Naturally, we then discuss perturbation theory, firstly by giving a concise approach in which this can be applied in teleparallel gravity theories and then apply it to a number of important theories in the literature. Finally, we examine works in observational and precision cosmology across the plethora of proposal theories. This is done using some of the latest observations and is used to tackle cosmological tensions which may be alleviated in teleparallel cosmology. We also introduce a number of recent works in the application of machine learning to gravity, we do this through deep learning and Gaussian processes, together with discussions about other approaches in the literature.

Teleparallel Gravity: From Theory to Cosmology

Morris \& Thorne \cite{morris1} proposed geometrical objects called traversable wormholes that act as bridges in connecting two spacetimes or two different points of the same spacetime. The geometrical properties of these wormholes depend upon the choice of the shape function. In literature, these are studied in modified gravities for different types of shape functions. In this paper, the traversable wormholes having shape function $b(r)=\frac{r_0\tanh(r)}{\tanh(r_0)}$ are explored in $f(R)$ gravity with $f(R)=R+\alpha R^m-\beta R^{-n}$, where $\alpha$, $\beta$, $m$ and $n$ are real constants. For different values of constants in function $f(R)$, the analysis is done in various cases. In each case, the energy conditions, equation of state parameter and anisotropic parameter are determined.

Non violation of energy conditions in wormholes modelling

We present the reconstruction method of $f(R)$ gravity for the homogeneous and anisotropic Bianchi-I spacetime, which was previously formulated only for homogeneous and isotropic Friedmann-Lemaitre-Robertson-Walker spacetime. We argue in this paper that for anisotropic spacetimes, the total anisotropy behaves as an independent metric degree of freedom (d.o.f.) on top of the average scale factor in $f(R)$ gravity. This is not like general relativity, where specifying the form of the average scale factor as a function of time also specifies the total anisotropy as a function of time uniquely. We link this peculiar fact to an interesting intertwining between the definition of Ricci scalar for anisotropic metric and anisotropy evolution equation in $f(R)$ gravity. Consequently, specifying an anisotropic solution of $f(R)$ gravity implies specifying both the average scale factor and the total anisotropy as functions of time. The reconstruction method hence formulated is applied to two scenarios where anisotropy suppression is important, namely, a quasi-de-Sitter expansion as required in inflation, and a power law contraction as required in ekpyrotic bounce models.

Reconstruction method of f ( R ) gravity for isotropic and anisotropic spacetimes

We investigate the dynamics of $f(R)$ gravity in Jordan and Einstein frames. First, we perform a phase-space singularities analysis in both frames. We show that, typically, anisotropic singularities are absent in the Einstein frame, whereas they may appear in the Jordan frame. We conciliate this apparent inconsistency by showing that the necessary conditions for the existence of the Einstein frame are namely the same ones assuring the absence of the anisotropic singularities in the Jordan frame. In other words, we show that, at least in the context of Bianchi I cosmologies, the Einstein frame is available only when the original formulation in the Jordan frame is free of anisotropic singularities. Furthermore, we present a novel dynamical system formulation for anisotropic cosmologies in which both frames, provided they exist, will be manifestly equivalent from the dynamical point of view, even though they fail to be diffeomorphic in general. Our results could not only help the construction of viable (free of anisotropic singularities) $f(R)$ cosmological models but also contribute to the still active debate on the physical interpretation of the two frames.

Dynamical equivalence of f (R ) gravity in Jordan and Einstein frames

In this work, we present some cosmologically relevant solutions using the spatially flat Friedmann-Lemaitre-Robertson-Walker (FLRW) spacetime in metric f ( R ) gravity where the form of the gravitational Lagrangian is given by 1 α e α R . In the low curvature limit this theory reduces to ordinary Einstein-Hilbert Lagrangian together with a cosmological constant term. Precisely because of this cosmological constant term this theory of gravity is able to support nonsingular bouncing solutions in both matter and vacuum background. Since for this theory of gravity f ′ and f ″ is always positive, this is free of both ghost instability and tachyonic instability. Moreover, because of the existence of the cosmological constant term, this gravity theory also admits a de-Sitter solution. Lastly we hint towards the possibility of a new type of cosmological solution that is possible only in higher derivative theories of gravity like this one.

https://www.mdpi.com/2218-1997/4/10/105/pdf

Cosmological Bounce and Some Other Solutions in Exponential Gravity

We present a dynamical analysis in terms of new expansion-normalized variables for homogeneous and anisotropic Bianchi-I spacetimes in $f(R)$ gravity in the presence of anisotropic matter. With a suitable choice of the evolution parameter, the Einstein's equations are reduced to an autonomous five-dimensional system of ordinary differential equations for the new variables. Further restrictions lead to considerable simplifications. For instance, we show that for a large class of functions $f(R)$, which includes several cases commonly considered in the literature, all the fixed points are polynomial roots, and hence they can be determined with good accuracy and classified for stability. Moreover, typically for these cases, any fixed point corresponding to isotropic solutions in the presence of anisotropic matter will be unstable. The assumption of a perfect fluid as source and the vacuum cases imply some dimensional reductions and even more simplifications. In particular, we find that the vacuum solutions of $f(R)={R}^{1+\ensuremath{\delta}}$, with $\ensuremath{\delta}$ a constant, are governed by an effective bidimensional phase space which can be analytically constructed, leading to an exactly soluble dynamics. Finally, we demonstrate that several results already reported in the literature can be reobtained in a more direct and easy way by exploring our dynamical formulation.

Dynamical properties of Bianchi-I spacetimes in f (R) gravity

As our understanding of the past in a bouncing universe is limited, it becomes difficult to propose a cosmological model which can give some understanding of the causal structure of the bouncing universe. In this article we address the issue related to the particle horizon problem in the bouncing universe models. It is shown that in many models the particle horizon does not exist, and consequently the horizon problem is trivially solved. In some cases a bouncing universe can have a particle horizon and we specify the conditions for its existence. In the absence of a particle horizon the Hubble surface specifies the causal structure of a bouncing universe. We specify the complex relationship between the Hubble surface and the particle horizon when the particle horizon exists. The article also address the issue related to the event horizon in a bouncing universe. A toy example of a bouncing universe is first presented where we specify the conditions which dictate the presence of a particle horizon. Next we specify the causal structures of three widely used bouncing models. The first case is related to quintom matter bounce model, the second one is loop quantum cosmology based bounce model and lastly $f(R)$ gravity induced bounce model. We present a brief discussion on the horizon problem in bouncing cosmologies. We point out that the causal structure of the various bounce models fit our general theoretical predictions.

Saikat Chakraborty

Papers

Reconstruction method of f ( R ) gravity for isotropic and anisotropic spacetimes

Dynamical equivalence of f (R ) gravity in Jordan and Einstein frames

Cosmological Bounce and Some Other Solutions in Exponential Gravity

Dynamical properties of Bianchi-I spacetimes in f (R) gravity

Causal horizons in a bouncing universe