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Signatures from the observed jet power and the radiative efficiency for rotating black holes in loop quantum gravity 环量子引力中旋转黑洞的观测喷流功率和辐射效率特征
Pub Date : 2024-09-11 DOI: arxiv-2409.06950
Zhengwei Cheng, Songbai Chen, Jiliang Jing
We study the radiative efficiency and the jet power in the spacetime of therotating black hole in loop quantum gravity (LQG), which has an extra LQGparameter. It is shown that with the increase of the LQG parameter, theconversion efficiency decreases for the slowly rotating black hole, butincreases for the rapidly rotating black hole, the jet power increases fordifferent black hole spins. With the observed data from the well-known sourcesA0620-00, H1743-322, XTE J1550-564, GRS1124-683, GRO J1655-40, and GRS1915+105,we make some constraints on the black hole spin parameter and the LQGparameter. The presence of the LQG parameter broadens the allowed range of theblack hole spin parameter for sources A0620-00, H1743-322, XTE J1550-564 andGRO J1655-40. However, for the source GRS 1915+105, there is no overlap betweenobservational constrain parameter regions, which implies that the rotating LQGblack hole cannot simultaneously account for the observed jet power and theradiative efficiency as in other black hole spacetimes.
我们研究了环量子引力(LQG)中旋转黑洞时空中的辐射效率和喷流功率。结果表明,随着LQG参数的增加,慢速旋转黑洞的转换效率会降低,而快速旋转黑洞的转换效率会增加,不同黑洞自旋时的喷流功率也会增加。我们利用来自著名黑洞源A0620-00、H1743-322、XTE J1550-564、GRS1124-683、GRO J1655-40和GRS1915+105的观测数据,对黑洞自旋参数和LQG参数做了一些约束。LQG参数的存在扩大了A0620-00、H1743-322、XTE J1550-564和GRO J1655-40等源的黑洞自旋参数的允许范围。然而,对于源GRS 1915+105,观测约束参数区域之间没有重叠,这意味着旋转LQG黑洞不能像其他黑洞空间一样同时解释观测到的喷流功率和辐射效率。
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引用次数: 0
Unique Imprint of Black Hole Spin on the Polarization of Near-Horizon Images 黑洞自旋对近地平线图像偏振的独特影响
Pub Date : 2024-09-11 DOI: arxiv-2409.07248
Yehui Hou, Jiewei Huang, Yosuke Mizuno, Minyong Guo, Bin Chen
Extracting information about the gravitational background from black holeimages is both important and challenging. In this study, we use a physicallymotivated plasma model, typically applied to stationary, axisymmetricspacetimes, to demonstrate that in a rotating black hole spacetime, thepolarizations of emitted light near the event horizon depend solely on thespacetime geometry, independent of the plasma flow geometry. We confirm thatthe frame-dragging effect of a rotating black hole governs the observedpolarization structure in the near-horizon image. This finding indicates aunique imprint of the black hole spin on the polarization of the near-horizonimage. We anticipate that refined observations of near-horizon emissions by thenext-generation Event Horizon Telescope will enable us to determine the blackhole spin in a straightforward manner.
从黑洞图像中提取引力背景信息既重要又具有挑战性。在这项研究中,我们使用了通常应用于静止、轴对称时空的物理等离子体模型,证明在旋转黑洞时空中,事件视界附近发射光的极化完全取决于时空几何,而与等离子体流几何无关。我们证实,旋转黑洞的拖帧效应控制着近视界图像中观测到的极化结构。这一发现表明了黑洞自旋对近地平线图像偏振的独特影响。我们预计下一代事件地平线望远镜对近地平线辐射的精细观测将使我们能够直接确定黑洞自旋。
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引用次数: 0
Einstein-Klein-Gordon system via Cauchy-characteristic evolution: Computation of memory and ringdown tail 通过考奇特征演化的爱因斯坦-克莱因-戈登系统:记忆和环落尾的计算
Pub Date : 2024-09-10 DOI: arxiv-2409.06141
Sizheng Ma, Kyle C. Nelli, Jordan Moxon, Mark A. Scheel, Nils Deppe, Lawrence E. Kidder, William Throwe, Nils L. Vu
Cauchy-characteristic evolution (CCE) is a powerful method for accuratelyextracting gravitational waves at future null infinity. In this work, we extendthe previously implemented CCE system within the numerical relativity codeSpECTRE by incorporating a scalar field. This allows the system to capturefeatures of beyond-general-relativity theories. We derive scalar contributionsto the equations of motion, Weyl scalar computations, Bianchi identities, andbalance laws at future null infinity. Our algorithm, tested across variousscenarios, accurately reveals memory effects induced by both scalar and tensorfields and captures Price's power-law tail ($u^{-l-2}$) in scalar fields atfuture null infinity, in contrast to the $t^{-2l-3}$ tail at future timelikeinfinity.
考奇特征演化(CCE)是在未来空无穷远处精确提取引力波的一种强大方法。在这项工作中,我们在数值相对论代码SpECTRE中扩展了先前实现的CCE系统,加入了一个标量场。这使得该系统能够捕捉到超越广义相对论的特征。我们推导了标量对运动方程的贡献、韦尔标量计算、比安奇等式以及未来空无穷远时的平衡定律。我们的算法在各种情况下都进行了测试,准确地揭示了标量场和张量场引起的记忆效应,并捕捉到了未来空无穷大时标量场中的普赖斯幂律尾部($u^{-l-2}$),而在未来类时间无穷大时则捕捉到了$t^{-2l-3}$尾部。
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引用次数: 0
Hierarchical Bayesian inference on an analytical model of the LISA massive black hole binary population LISA 大质量黑洞双星群分析模型的分层贝叶斯推论
Pub Date : 2024-09-10 DOI: arxiv-2409.06527
Vivienne Langen, Nicola Tamanini, Sylvain Marsat, Elisa Bortolas
Massive black hole binary (MBHB) mergers will be detectable in large numbersby the Lisa Interferometer Space Antenna (LISA), which will thus provide newinsights on how they form via repeated dark matter (DM) halo and galaxymergers. Here we present a simple analytical model to generate a population ofMBHB mergers based on a theoretical prescription that connects them to DM halomergers. The high flexibility of our approach allows us to explore the broadand uncertain range of MBH seeding and growth mechanisms, as well as thedifferent effects behind the interplay between MBH and galactic astrophysics.Such a flexibility is fundamental for the successful implementation andoptimisation of the hierarchical Bayesian parameter estimation approach thathere we apply to the MBHB population of LISA for the first time. Our inferredpopulation hyper-parameters are chosen as proxies to characterise the MBH--DMhalo mass scaling relation, the occupation fraction of MBHs in DM halos and thedelay between halo and MBHB mergers. We find that LISA will provide tightconstraints at the lower-end of the MBH-halo scaling relation, wellcomplementing EM observations which are biased towards large masses.Furthermore, our results suggest that LISA will constrain some features of theMBH occupation fraction at high redshift, as well as merger time delays of theorder of a few hundreds of Myr, opening the possibility to constrain dynamicalevolution time scales such as the dynamical friction. The analysis presentedhere constitutes a first attempt at developing a hierarchical Bayesianinference approach to the LISA MBHB population, opening the way for severalfurther improvements and investigations.
大质量黑洞双星(MBHB)合并将通过丽莎干涉仪空间天线(LISA)被大量探测到,这将为我们提供关于它们如何通过重复的暗物质(DM)光环和星系合并形成的新见解。在这里,我们提出了一个简单的分析模型,根据将MBHB合并与DM光环合并联系起来的理论处方,生成MBHB合并群。这种灵活性是成功实施和优化分层贝叶斯参数估计方法的基础,我们在这里首次将这种方法应用于 LISA 的 MBHB 群体。我们推断出的种群超参数被选作描述MBH--DM光环质量比例关系、DM光环中MBH的占据比例以及光环和MBHB合并之间的延迟的代理参数。我们发现,LISA 将在 MBH-halo 缩放关系的低端提供严格的约束,很好地补充了偏向于大质量的电磁观测。此外,我们的结果表明,LISA 将约束高红移下 MBH 占有率的某些特征,以及合并时间延迟到几百 Myr 的数量级,从而为约束动力学演变时间尺度(如动力学摩擦)提供了可能性。这里介绍的分析是针对 LISA MBHB 群体开发分层贝叶斯推断方法的首次尝试,为进一步的改进和研究开辟了道路。
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引用次数: 0
Wave Metrics in the Cotton and Conformal Killing Gravity Theories 棉花和共形杀伤引力理论中的波尺度
Pub Date : 2024-09-10 DOI: arxiv-2409.06257
Metin Gürses, Yaghoub Heydarzade, Çetin Şentürk
We study wave metrics in the context of Cotton Gravity and Conformal KillingGravity. First, we consider pp-wave metrics with flat and non-flat wavesurfaces and show that they are exact solutions to the field equations of thesetheories. More explicitly, the field equations reduce to an inhomogeneousLaplace and Helmholtz differential equations, depending on the curvature of thetwo-dimensional geometry of the wave surfaces. An interesting point here isthat the ones with non-flat wave surfaces are not present in classical GR,which manifests a crucial distinction between these theories and GR. Moreover,we investigate Kerr-Schild-Kundt metrics in the context of these theories andshow that, from among these metrics, only the AdS wave metrics solve the fieldequations of these theories. However, AdS spherical and dS hyperbolic wavemetrics do not solve the field equations of these theories, which is incontrast to the classical GR. In the case of AdS wave metrics, the fieldequations of these theories reduce to an inhomogeneous Klein-Gordon equation.We give all the necessary and sufficient conditions for the metric function $V$to solve these field equations. Lastly, we address the colliding gravitationalplane waves problem only in Cotton gravity due to the complexity of the fieldequations in Conformal Killing Gravity.
我们在科顿引力(Cotton Gravity)和共形基灵引力(Conformal KillingGravity)的背景下研究波度量。首先,我们考虑了具有平坦和非平坦波面的pp波度量,并证明它们是setheories场方程的精确解。更明确地说,场方程简化为非均质拉普拉斯微分方程和亥姆霍兹微分方程,这取决于波面二维几何的曲率。这里有趣的一点是,经典 GR 中不存在非平面波面,这体现了这些理论与 GR 的重要区别。此外,我们还研究了这些理论背景下的克尔-希尔德-昆特度量,结果表明,在这些度量中,只有AdS波度量解决了这些理论的场方程。然而,AdS球面波度量和dS双曲面波度量并不能求解这些理论的场方程,这与经典GR是不一致的。我们给出了求解这些场方程的度量函数 $V$ 的所有必要条件和充分条件。最后,由于共形基林引力中场方程的复杂性,我们只在科顿引力中讨论引力面波对撞问题。
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引用次数: 0
Influence of scalar field in massive particle motion in JNW spacetime 标量场对 JNW 时空中大质量粒子运动的影响
Pub Date : 2024-09-10 DOI: arxiv-2409.06225
Bobur Turimov, Akbar Davlataliev, Ahmadjon Abdujabbarov, Bobomurat Ahmedov
In this paper, we investigated the motion of massive particles in thepresence of scalar and gravitational fields, particularly focusing on theJanis-Newman-Winicour (JNW) naked singularity solution. It is shown that theinnermost stable circular orbit (ISCO) radius strongly depends on scalarcoupling parameter. Additionally, we explored the radiation reaction effects onparticle dynamics, incorporating a reaction term into the motion equations.Numerical simulations indicated minimal impact on particle trajectories fromradiation reaction. We also examined the oscillatory motion of particles aroundcompact objects in the JNW spacetime, focusing on radial and verticaloscillations. Our analysis indicated that the scalar field's coupling parameterand the spacetime deformation parameter $n$ significantly alter the fundamentalfrequencies of these oscillations. Furthermore, we studied quasi-periodicoscillations (QPOs) in X-ray binaries, using the relativistic precession (RP)model to analyze upper and lower frequency relationships. Our results indicatedthat increasing parameters ($n$ and $g_s$) shifts the frequency ratio of 3:2QPOs closer to the naked singularity, with $n$ decreasing and $g_s$ increasingboth frequencies. Finally, we analyzed QPO data from selected four X-ray binarysystems using Markov Chain Monte Carlo (MCMC) analysis to constrain JNWparameters. Our findings provided insights into the mass, coupling anddeformation parameter for each system, enhancing our understanding of compactobject dynamics in strong gravitational fields.
在本文中,我们研究了大质量粒子在标量场和引力场作用下的运动,尤其侧重于詹尼斯-纽曼-维尼柯(JNW)裸奇点解。研究表明,最稳定圆形轨道(ISCO)半径与标量耦合参数密切相关。此外,我们还探索了辐射反应对粒子动力学的影响,在运动方程中加入了反应项。我们还研究了 JNW 时空中粒子围绕紧凑物体的振荡运动,重点是径向和垂直振荡。我们的分析表明,标量场的耦合参数和时空变形参数 $n$ 显著改变了这些振荡的基频。此外,我们还研究了X射线双星中的准周期振荡(QPOs),利用相对论前冲(RP)模型分析了上下频率关系。结果表明,参数($n$和$g_s$)的增大会使3:2QPO的频率比更接近裸奇点,$n$减小,$g_s$增大。最后,我们利用马尔可夫链蒙特卡洛(MCMC)分析方法分析了所选的四个X射线双系统的QPO数据,以约束JNW参数。我们的研究结果提供了对每个系统的质量、耦合和变形参数的见解,增强了我们对强引力场中紧凑天体动力学的理解。
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引用次数: 0
Non-Canonical Dark Energy Parameter Evolution in a Canonical Quintessence Cosmology 经典五元宇宙学中的非经典暗能量参数演化
Pub Date : 2024-09-10 DOI: arxiv-2409.06792
Rodger I. Thompson
This study considers the specific case of a flat, minimally coupled togravity, quintessence cosmology with a dark energy quartic polynomial potentialthat has the same mathematical form as the Higgs potential. Previous work onthis case determined that the scalar field is given by a simple expression ofthe Lambert W function in terms of the easily observable scale factor. Thisexpression provides analytic equations for the evolution of cosmological darkenergy parameters as a function of the scale factor for all points on theLambert W function principal branch. The Lambert W function is zero at a scalefactor of zero that marks the big bang. The evolutionary equations beyond thebig bang describe a canonical universe that is similar to {Lambda}CDM, makingit an excellent dynamical template to compare with observational data. Theportion of the W function principal before the big bang extends to the infinitepre-bang past. It describes a noncanonical universe with an initially very lowmass density that contracts by rolling down the dark energy potential to asingularity, big bang, at the scale factor zero point. This provides a naturalorigin for the big bang. It also raises the possibility that the universeexisted before the big bang and is far older, and that it was once far largerthan its current size. The recent increasing interest in the possibility of adynamical universe instead of {Lambda}CDM makes the exploration of the natureof such universes particularly relevant.
本研究考虑的是一种平坦的、与引力最小耦合的五元宇宙学,其暗能量四元多项式势的数学形式与希格斯势相同。以前关于这种情况的研究确定,标量场是由易于观测的尺度因子的朗伯 W 函数的简单表达式给出的。这个表达式为宇宙学暗能量参数的演化提供了解析方程,它是兰伯特 W 函数主支上所有点的尺度因子的函数。兰伯特 W 函数在大爆炸尺度因子为零时为零。大爆炸之后的演化方程描述了一个与{Lambda}CDM相似的典型宇宙,使其成为与观测数据进行比较的绝佳动力学模板。大爆炸之前的W函数本构部分一直延伸到大爆炸之前的无限远的过去。它描述了一个非正则宇宙,其初始质量密度非常低,在尺度因子零点时,暗能量势能向下滚动,从而收缩为奇点,即大爆炸。这为大爆炸提供了一个自然起源。这也提出了一种可能性,即宇宙在大爆炸之前就已经存在,而且要古老得多,它曾经比现在的大小要大得多。最近,人们对{Lambda}CDM之外的ynamical宇宙的可能性越来越感兴趣,这使得探索这种宇宙的性质变得尤为重要。
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引用次数: 0
Schwarzschild Lensing From Geodesic Deviation 从大地偏差看施瓦兹柴尔德透镜
Pub Date : 2024-09-10 DOI: arxiv-2409.06281
Zhao Li, Xiao Guo, Tan Liu, Tao Zhu, Wen Zhao
We revisit the gravitational lensing of light or gravitational waves bySchwarzschild black hole in geometric optics. Instead of a single masslessparticle, we investigate the collective behavior of a congruence oflight/gravitational rays, described by the geodesic deviation equation (GDE).By projecting on the Newman-Penrose tetrad, GDE is decoupled, and we find ananalytical Dyson-like series solution in the weak deflection and thin lenslimits. Based on such a solution, we study the evolution of cross-sectionalarea and axis ratio. Finally, we reproduce the magnification and axis ratio ofthe lensing images up to the second order of weak deflection approximation andimprove some missing corrections in previous works.
我们在几何光学中重新探讨了施瓦兹柴尔德黑洞对光或引力波的引力透镜作用。通过在纽曼-彭罗斯四面体上的投影,GDE 被解耦,我们找到了在弱偏转和薄透镜极限下的戴森样解析级数解。在此基础上,我们研究了横截面积和轴比的演变。最后,我们在弱偏转近似的二阶以内重现了透镜图像的放大率和轴比,并改进了之前工作中一些缺失的修正。
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引用次数: 0
Black hole - neutron star binaries with high spins and large mass asymmetries: II. Properties of dynamical simulations 具有高自旋和大质量不对称的黑洞-中子星双星:II.动力学模拟的特性
Pub Date : 2024-09-10 DOI: arxiv-2409.06777
Konrad Topolski, Samuel Tootle, Luciano Rezzolla
Black hole (BH) - neutron star (NS) binary mergers are not only strongsources of gravitational waves (GWs), but they are also candidates for jointdetections in the GW and electromagnetic (EM) spectra. However, the possibleemergence of an EM signal from these binaries is determined by a complexcombination of the equation of state (EOS), the BH spin, and the mass ratio. Inthis second paper in a series, we present a systematic exploration of thepossible space of binary parameters in terms of the mass ratio and BH spin soas to construct a complete description of the dynamical processes accompanyinga BHNS binary merger. This second work relies not only on the initial datapresented in the companion paper I, but also on the predictions viaquasi-equilibrium (QE) sequences on the outcome of the binary. In this way, andfor the first time, we are able to relate the predictions of QE analyses withthe results of accurate general-relativistic magnetohydrodynamic simulations.In addition to a careful investigation of the evolution of the BH mass and spinas a result of the merger, the total remnant rest-mass of the resultingaccretion disk and its properties, and of the corresponding post-merger GWemission, special attention is paid to the conditions that lead to tidaldisruption. Leveraging QE calculations, we are able to verify the reliabilityof stringent predictions about the occurrence or not of a plunge and to measurethe `strength' of the tidal disruption when it takes place. Finally, using anovel contraction of the Riemann tensor in a tetrad comoving with the fluidintroduced in paper I, we are able to point out the onset of the instability totidal disruption. This new diagnostic can be employed not only to determine theoccurrence of the disruption, but also to characterize it in terms of thebinary parameters.
黑洞(BH)-中子星(NS)双星合并不仅是引力波(GW)的强大来源,而且也是引力波和电磁波(EM)光谱联合探测的候选者。然而,这些双星可能产生的电磁信号是由状态方程(EOS)、BH自旋和质量比的综合组合决定的。在本系列的第二篇论文中,我们从质量比和BH自旋的角度,对双星参数的可能空间进行了系统的探索,从而构建出伴随BHNS双星合并的动力学过程的完整描述。这第二项工作不仅依赖于论文 I 中提供的初始数据,还依赖于通过准平衡(QE)序列对双星结果的预测。除了仔细研究合并后 BH 质量和自旋的演化、所产生的增殖盘的总剩余静止质量及其性质,以及相应的合并后 GW 发射之外,我们还特别关注了导致潮汐破坏的条件。利用 QE 计算,我们能够验证关于发生或不发生暴跌的严格预测的可靠性,并测量潮汐扰动发生时的 "强度"。最后,利用与论文 I 中引入的流体相向的四面体中黎曼张量的水平收缩,我们能够指出潮汐扰动不稳定性的开始。这种新的诊断方法不仅可以用来确定破坏的发生,还可以根据二元参数来描述破坏的特征。
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引用次数: 0
Cosmic Acceleration from topological considerations III: Lie group 从拓扑考虑宇宙加速 III:列群
Pub Date : 2024-09-10 DOI: arxiv-2409.06893
I. A. Sarmiento Alvarado, Maribel Hernández Márquez, Tonatiuh Matos
Recent observations on the large-scale structure of the universe indicatethat the cosmological constant cannot be the definitive answer to the nature ofdark energy. Therefore, it is a good time to propose alternatives to understandthe late-accelerated expansion of the universe. In this work we study thepossibility that the acceleration of space-time is due to the topology of theuniverse. We assume that the topology of the universe is a principal fiberbundle whose base space is our 4-dimensional spacetime and the fiber is an$N$-dimensional Lie group that evolves with time. For the base space weconsider a homogeneous and isotropic spacetime, we find that the base space iscurrently accelerating for $1 < N$ compact semi-simple Lie groups whosescale-factors are equal and for $1 < N$ non-Abelian Lie groups whosescale-factors are different and as long as its structure constants satisfy someconditions. However when we study the evolution of the density parameters thesediffer from the evolution within the $Lambda$CDM model, this led us to thinkin the possibility of use a different group as fiber in order to obtain theright evolution of the density parameters. We conclude that it is possible thatthe accelerated expansion of the universe is due to consider a differenttopology of the universe as a principal fiber bundle.
最近对宇宙大尺度结构的观测表明,宇宙常数并不能成为暗能量性质的最终答案。因此,现在是提出替代方案来理解宇宙晚期加速膨胀的好时机。在这项工作中,我们研究了时空加速是由于宇宙拓扑造成的这一可能性。我们假设宇宙的拓扑结构是一个主纤维束,其基底空间是我们的四维时空,纤维是一个随时间演化的 N 维李群。我们认为基底空间是均质和各向同性的时空,我们发现,只要基底空间的结构常数满足某些条件,那么对于1<N$的紧凑半简单李群(其阶跃因子是相等的)和1<N$的非阿贝尔李群(其阶跃因子是不同的),基底空间目前是加速的。然而,当我们研究密度参数的演化时,它们与$Lambda$CDM模型中的演化有所不同,这促使我们思考是否有可能使用不同的群作为纤维,以获得密度参数的正确演化。我们的结论是,宇宙的加速膨胀有可能是由于考虑了不同的宇宙拓扑结构作为主纤维束。
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引用次数: 0
期刊
arXiv - PHYS - General Relativity and Quantum Cosmology
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