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4 <title>Classical and Quantum Gravity - latest papers</title>
5 <link>http://iopscience.iop.org/journal/rss/0264-9381</link>
6 <description>Latest articles for Classical and Quantum Gravity</description>
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23 <title>IOPscience</title>
24 <url>http://iopscience.iop.org/image/iopscience-rss.gif</url>
25 <link>http://iopscience.iop.org/journal/rss/0264-9381</link>
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27 <item rdf:about="http://iopscience.iop.org/article/10.1088/1361-6382/acb9cd">
28 <title>Curvature and dynamical spacetimes: can we peer into the quantum regime?</title>
29 <link>http://iopscience.iop.org/article/10.1088/1361-6382/acb9cd</link>
30 <description>Stationary compact astrophysical objects such as black holes and neutron stars behave as classical systems from the gravitational point of view. Their (observable) curvature is everywhere ‘small’. Here we investigate whether mergers of such objects, or other strongly dynamical spacetimes such as collapsing configurations, may probe the strong-curvature regime of general relativity. Our results indicate that dynamical black hole spacetimes always result in a modest increase in the Kretschmann scalar, relative to the stationary state. In contrast, we find that the Kretschmann scalar can dynamically increase by orders of magnitude, during the gravitational collapse of scalar fields, and that the (normalized) peak curvature does not correspond to that of the critical solution. Nevertheless, without fine tuning of initial data, this increase lies far below that needed to render quantum-gravity corrections important.</description>
31 <dc:creator>Vitor Cardoso, David Hilditch, Krinio Marouda, José Natário and Ulrich Sperhake</dc:creator>
32 <dc:date>2023-02-23T00:00:00Z</dc:date>
33 <dc:source>Classical and Quantum Gravity</dc:source>
34 <iop:authors>Vitor Cardoso <em>et al</em></iop:authors>
35 <iop:citation>Vitor Cardoso <em>et al</em> 2023 <em>Classical and Quantum Gravity</em> <b>40</b> 065008</iop:citation>
36 <iop:pdf>https://iopscience.iop.org/article/10.1088/1361-6382/acb9cd/pdf</iop:pdf>
37 <prism:coverDisplayDate>23/February/2023</prism:coverDisplayDate>
38 <prism:number>6</prism:number>
39 <prism:volume>40</prism:volume>
40 <prism:publicationName>Classical and Quantum Gravity</prism:publicationName>
41 <prism:startingPage>065008</prism:startingPage>
42 <prism:doi>10.1088/1361-6382/acb9cd</prism:doi>
43 </item>
44 <item rdf:about="http://iopscience.iop.org/article/10.1088/1361-6382/acbadc">
45 <title>The analysis of the far-field phase and the tilt-to-length error contribution in space-based laser interferometry</title>
46 <link>http://iopscience.iop.org/article/10.1088/1361-6382/acbadc</link>
47 <description>The arm length of the space-based interferometer for gravitational wave detection is 108–109
48 , and picometer precision is required. The wavefront error in the far-field coupled with the pointing jitter is a major noise source, which raises higher requirements of the wavefront quality of the telescope. By extending the analytical solutions of the far-field phase to 21 Zernike aberrations, this paper demonstrates that the far-field phase could be regarded as the sum of the effects of the individual aberrations and a phase plane with its slope related to the wavefront RMS. For individual aberrations, only low-order aberrations have a significant effect on the far-field phase, but high-order aberrations will contribute to the coupling terms which is shown as a phase slope. So there is a definite corresponding relationship between the aberrations and the far-field phase, and it can be easily illustrated graphically. Based on the analytical solutions of the far-field phase, we proposed to consider the tilt-to-length (TTL) error together with the far-field phase. The TTL error is also one of the main noise sources in space-based laser interferometry, which presents big difficulties in the optical system. We found that TTL error could be added to the far-field phase as a piston term during pointing, which then help to bring the stationary point closer to the z-axis and reduce the phase noise detected at the stationary point. By considering the TTL together with the far-field phase, the requirement of the telescope could be λ/25 wavefront RMS (λ = 1064 ). And there will be a large tolerance range for the TTL error, so it is only necessary to evaluate the TTL error and limit it to a suitable range, not to eliminate it.</description>
49 <dc:creator>Qing Xiao, Huizong Duan, Min Ming, Jingyi Zhang, Fan Zhu, Yuwei Jiang and Hsien-Chi Yeh</dc:creator>
50 <dc:date>2023-02-23T00:00:00Z</dc:date>
51 <dc:source>Classical and Quantum Gravity</dc:source>
52 <iop:authors>Qing Xiao <em>et al</em></iop:authors>
53 <iop:citation>Qing Xiao <em>et al</em> 2023 <em>Classical and Quantum Gravity</em> <b>40</b> 065009</iop:citation>
54 <iop:pdf>https://iopscience.iop.org/article/10.1088/1361-6382/acbadc/pdf</iop:pdf>
55 <prism:coverDisplayDate>23/February/2023</prism:coverDisplayDate>
56 <prism:number>6</prism:number>
57 <prism:volume>40</prism:volume>
58 <prism:publicationName>Classical and Quantum Gravity</prism:publicationName>
59 <prism:startingPage>065009</prism:startingPage>
60 <prism:doi>10.1088/1361-6382/acbadc</prism:doi>
61 </item>
62 <item rdf:about="http://iopscience.iop.org/article/10.1088/1361-6382/acbc04">
63 <title>Multicritical phase transitions in multiply rotating black holes</title>
64 <link>http://iopscience.iop.org/article/10.1088/1361-6382/acbc04</link>
65 <description>We show that multi-critical points in which more than three phases coalesce are present in multiply rotating Kerr-anti de Sitter black holes in d-dimensions. We explicitly present a quadruple point for a triply rotating black hole in d = 8 and a quintuple point for a quadruply rotating black hole in d = 10. The maximal number of distinct phases n is one larger than the maximal number of independent rotations, and we outline a method for obtaining the associated n-tuple point. Situations also exist where more than three phases merge at sub-maximal multi-critical points. Our results show that multi-critical points in black hole thermodynamics are more common than previously thought, with systems potentially supporting many phases as long as a sufficient number of thermodynamic variables are present.</description>
66 <dc:creator>Jerry Wu and Robert B Mann</dc:creator>
67 <dc:date>2023-02-22T00:00:00Z</dc:date>
68 <dc:source>Classical and Quantum Gravity</dc:source>
69 <iop:authors>Jerry Wu and Robert B Mann</iop:authors>
70 <iop:citation>Jerry Wu and Robert B Mann 2023 <em>Classical and Quantum Gravity</em> <b>40</b> 06LT01</iop:citation>
71 <iop:pdf>https://iopscience.iop.org/article/10.1088/1361-6382/acbc04/pdf</iop:pdf>
72 <prism:coverDisplayDate>22/February/2023</prism:coverDisplayDate>
73 <prism:number>6</prism:number>
74 <prism:volume>40</prism:volume>
75 <prism:publicationName>Classical and Quantum Gravity</prism:publicationName>
76 <prism:startingPage>06LT01</prism:startingPage>
77 <prism:doi>10.1088/1361-6382/acbc04</prism:doi>
78 </item>
79 <item rdf:about="http://iopscience.iop.org/article/10.1088/1361-6382/acbadb">
80 <title>The impact of
81
82 f(G,T)
83
84 gravity on the evolution of cavity in the cluster of stars</title>
85 <link>http://iopscience.iop.org/article/10.1088/1361-6382/acbadb</link>
86 <description>This paper investigates the evolution of cavities for the cluster of stars in the context of extended Gauss–Bonnet gravity. We assume a spherically symmetric geometry along with locally anisotropic fluid distribution. It is assumed that the proper radial distance among neighboring stellar components stays unchanged during purely areal evolution stage. We provide some analytical solutions by using general formulism in gravitation theory. The thick-shells cavities at one or both boundary surfaces are found to satisfy the Darmois conditions. Moreover, we also investigate the physical behavior of cavity models by considering the stellar , and . We conclude that the dark matter has a strong impact on the evolution of cavities in the cluster of stars.</description>
87 <dc:creator>Rubab Manzoor, M Awais Sadiq and Imdad Hussain</dc:creator>
88 <dc:date>2023-02-21T00:00:00Z</dc:date>
89 <dc:source>Classical and Quantum Gravity</dc:source>
90 <iop:authors>Rubab Manzoor <em>et al</em></iop:authors>
91 <iop:citation>Rubab Manzoor <em>et al</em> 2023 <em>Classical and Quantum Gravity</em> <b>40</b> 065007</iop:citation>
92 <iop:pdf>https://iopscience.iop.org/article/10.1088/1361-6382/acbadb/pdf</iop:pdf>
93 <prism:coverDisplayDate>21/February/2023</prism:coverDisplayDate>
94 <prism:number>6</prism:number>
95 <prism:volume>40</prism:volume>
96 <prism:publicationName>Classical and Quantum Gravity</prism:publicationName>
97 <prism:startingPage>065007</prism:startingPage>
98 <prism:doi>10.1088/1361-6382/acbadb</prism:doi>
99 </item>
100 <item rdf:about="http://iopscience.iop.org/article/10.1088/1361-6382/acbade">
101 <title>Deflection in higher dimensional spacetime and asymptotically non-flat spacetimes</title>
102 <link>http://iopscience.iop.org/article/10.1088/1361-6382/acbade</link>
103 <description>Using a perturbative technique, in this work we study the deflection of null and timelike signals in the extended Einstein–Maxwell spacetime, the Born–Infeld gravity and the charged Ellis–Bronnikov (CEB) spacetime in the weak field limit. The deflection angles are found to take a (quasi-)series form of the impact parameter, and automatically takes into account the finite distance effect of the source and observer. The method is also applied to find the deflections in CEB spacetime with arbitrary dimension. It’s shown that to the leading non-trivial order, the deflection in some n-dimensional spacetimes is of the order . We then extended the method to spacetimes that are asymptotically non-flat and studied the deflection in a nonlinear electrodynamical scalar theory. The deflection angle in such asymptotically non-flat spacetimes at the trivial order is found to be not π anymore. In all these cases, the perturbative deflection angles are shown to agree with numerical results extremely well. The effects of some nontrivial spacetime parameters as well as the signal velocity on the deflection angles are analyzed.</description>
104 <dc:creator>Jinhong He, Qianchuan Wang, Qiyue Hu, Li Feng and Junji Jia</dc:creator>
105 <dc:date>2023-02-21T00:00:00Z</dc:date>
106 <dc:source>Classical and Quantum Gravity</dc:source>
107 <iop:authors>Jinhong He <em>et al</em></iop:authors>
108 <iop:citation>Jinhong He <em>et al</em> 2023 <em>Classical and Quantum Gravity</em> <b>40</b> 065006</iop:citation>
109 <iop:pdf>https://iopscience.iop.org/article/10.1088/1361-6382/acbade/pdf</iop:pdf>
110 <prism:coverDisplayDate>21/February/2023</prism:coverDisplayDate>
111 <prism:number>6</prism:number>
112 <prism:volume>40</prism:volume>
113 <prism:publicationName>Classical and Quantum Gravity</prism:publicationName>
114 <prism:startingPage>065006</prism:startingPage>
115 <prism:doi>10.1088/1361-6382/acbade</prism:doi>
116 </item>
117 <item rdf:about="http://iopscience.iop.org/article/10.1088/1361-6382/acb633">
118 <title>Data quality up to the third observing run of advanced LIGO: Gravity Spy glitch classifications</title>
119 <link>http://iopscience.iop.org/article/10.1088/1361-6382/acb633</link>
120 <description>Understanding the noise in gravitational-wave detectors is central to detecting and interpreting gravitational-wave signals. Glitches are transient, non-Gaussian noise features that can have a range of environmental and instrumental origins. The Gravity Spy project uses a machine-learning algorithm to classify glitches based upon their time–frequency morphology. The resulting set of classified glitches can be used as input to detector-characterisation investigations of how to mitigate glitches, or data-analysis studies of how to ameliorate the impact of glitches. Here we present the results of the Gravity Spy analysis of data up to the end of the third observing run of advanced laser interferometric gravitational-wave observatory (LIGO). We classify 233981 glitches from LIGO Hanford and 379805 glitches from LIGO Livingston into morphological classes. We find that the distribution of glitches differs between the two LIGO sites. This highlights the potential need for studies of data quality to be individually tailored to each gravitational-wave observatory.</description>
121 <dc:creator>J Glanzer, S Banagiri, S B Coughlin, S Soni, M Zevin, C P L Berry, O Patane, S Bahaadini, N Rohani, K Crowston, V Kalogera, C Østerlund, L Trouille and A Katsaggelos</dc:creator>
122 <dc:date>2023-02-20T00:00:00Z</dc:date>
123 <dc:source>Classical and Quantum Gravity</dc:source>
124 <iop:authors>J Glanzer <em>et al</em></iop:authors>
125 <iop:citation>J Glanzer <em>et al</em> 2023 <em>Classical and Quantum Gravity</em> <b>40</b> 065004</iop:citation>
126 <iop:pdf>https://iopscience.iop.org/article/10.1088/1361-6382/acb633/pdf</iop:pdf>
127 <prism:coverDisplayDate>20/February/2023</prism:coverDisplayDate>
128 <prism:number>6</prism:number>
129 <prism:volume>40</prism:volume>
130 <prism:publicationName>Classical and Quantum Gravity</prism:publicationName>
131 <prism:startingPage>065004</prism:startingPage>
132 <prism:doi>10.1088/1361-6382/acb633</prism:doi>
133 </item>
134 <item rdf:about="http://iopscience.iop.org/article/10.1088/1361-6382/acb9cc">
135 <title>On the algebraic approach to GUP in anisotropic space</title>
136 <link>http://iopscience.iop.org/article/10.1088/1361-6382/acb9cc</link>
137 <description>Motivated by current searches for signals of Lorentz symmetry violation in nature and recent investigations on generalized uncertainty principle (GUP) models in anisotropic space, in this paper we identify GUP models satisfying two criteria: (i) invariance of commutators under canonical transformations, and (ii) physical independence of position and momentum on the ordering of auxiliary operators in their definitions. Compliance of these criteria is fundamental if one wishes to unambiguously describe GUP using an algebraic approach and, surprisingly, neither is trivially satisfied when GUP is assumed within anisotropic space. As a consequence, we use these criteria to place important restrictions on what or how GUP models may be approached algebraically.</description>
138 <dc:creator>André Herkenhoff Gomes</dc:creator>
139 <dc:date>2023-02-17T00:00:00Z</dc:date>
140 <dc:source>Classical and Quantum Gravity</dc:source>
141 <iop:authors>André Herkenhoff Gomes</iop:authors>
142 <iop:citation>André Herkenhoff Gomes 2023 <em>Classical and Quantum Gravity</em> <b>40</b> 065005</iop:citation>
143 <iop:pdf>https://iopscience.iop.org/article/10.1088/1361-6382/acb9cc/pdf</iop:pdf>
144 <prism:coverDisplayDate>17/February/2023</prism:coverDisplayDate>
145 <prism:number>6</prism:number>
146 <prism:volume>40</prism:volume>
147 <prism:publicationName>Classical and Quantum Gravity</prism:publicationName>
148 <prism:startingPage>065005</prism:startingPage>
149 <prism:doi>10.1088/1361-6382/acb9cc</prism:doi>
150 </item>
151 <item rdf:about="http://iopscience.iop.org/article/10.1088/1361-6382/acace4">
152 <title>The gravitational afterglow of boson stars</title>
153 <link>http://iopscience.iop.org/article/10.1088/1361-6382/acace4</link>
154 <description>In this work we study the long-lived post-merger gravitational wave signature of a boson-star binary coalescence. We use full numerical relativity to simulate the post-merger and track the gravitational afterglow over an extended period of time. We implement recent innovations for the binary initial data, which significantly reduce spurious initial excitations of the scalar field profiles, as well as a measure for the angular momentum that allows us to track the total momentum of the spatial volume, including the curvature contribution. Crucially, we find the afterglow to last much longer than the spin-down timescale. This prolonged gravitational wave afterglow provides a characteristic signal that may distinguish it from other astrophysical sources.</description>
155 <dc:creator>Robin Croft, Thomas Helfer, Bo-Xuan Ge, Miren Radia, Tamara Evstafyeva, Eugene A Lim, Ulrich Sperhake and Katy Clough</dc:creator>
156 <dc:date>2023-02-15T00:00:00Z</dc:date>
157 <dc:source>Classical and Quantum Gravity</dc:source>
158 <iop:authors>Robin Croft <em>et al</em></iop:authors>
159 <iop:citation>Robin Croft <em>et al</em> 2023 <em>Classical and Quantum Gravity</em> <b>40</b> 065001</iop:citation>
160 <iop:pdf>https://iopscience.iop.org/article/10.1088/1361-6382/acace4/pdf</iop:pdf>
161 <prism:coverDisplayDate>15/February/2023</prism:coverDisplayDate>
162 <prism:number>6</prism:number>
163 <prism:volume>40</prism:volume>
164 <prism:publicationName>Classical and Quantum Gravity</prism:publicationName>
165 <prism:startingPage>065001</prism:startingPage>
166 <prism:doi>10.1088/1361-6382/acace4</prism:doi>
167 </item>
168 <item rdf:about="http://iopscience.iop.org/article/10.1088/1361-6382/acb5df">
169 <title>Boundary conditions for AdS2 dilaton gravity</title>
170 <link>http://iopscience.iop.org/article/10.1088/1361-6382/acb5df</link>
171 <description>We study a bi-parametric family of dilaton gravity models with constant and negative curvature. This family includes the Jackiw–Teitelboim gravity and the Liouville gravity model induced by a bosonic string. Furthermore, this family is conformally equivalent to the hyperbolic dilaton models. We propose boundary conditions in the Fefferman–Graham and in the Eddington–Finkelstein gauge. We check the consistency of the asymptotic conditions by computing the entropy of their black hole solution.</description>
172 <dc:creator>Carlos Valcárcel</dc:creator>
173 <dc:date>2023-02-15T00:00:00Z</dc:date>
174 <dc:source>Classical and Quantum Gravity</dc:source>
175 <iop:authors>Carlos Valcárcel</iop:authors>
176 <iop:citation>Carlos Valcárcel 2023 <em>Classical and Quantum Gravity</em> <b>40</b> 065003</iop:citation>
177 <iop:pdf>https://iopscience.iop.org/article/10.1088/1361-6382/acb5df/pdf</iop:pdf>
178 <prism:coverDisplayDate>15/February/2023</prism:coverDisplayDate>
179 <prism:number>6</prism:number>
180 <prism:volume>40</prism:volume>
181 <prism:publicationName>Classical and Quantum Gravity</prism:publicationName>
182 <prism:startingPage>065003</prism:startingPage>
183 <prism:doi>10.1088/1361-6382/acb5df</prism:doi>
184 </item>
185 <item rdf:about="http://iopscience.iop.org/article/10.1088/1361-6382/acb884">
186 <title>Pole inflation and primordial black holes formation in Starobinsky-like supergravity</title>
187 <link>http://iopscience.iop.org/article/10.1088/1361-6382/acb884</link>
188 <description>We extend the Cecotti–Kallosh model of Starobinsky inflation in supergravity by adding a holomorphic function to the superpotential in order to generate a large peak in the power spectrum of scalar (curvature) perturbations. In our approach, the singular non-canonical kinetic terms are largely responsible for inflation (as an attractor solution), whereas the superpotential is engineered to generate a production of PBH. We study the cases with (a) a linear holomorphic function, (b) a quadratic holomorphic function, and (c) an exponential holomorphic function, as regards the dependence of inflation and PBH production upon parameters of those functions and initial conditions, as well as verify viability of inflation with our superpotentials. We find that an efficient production of PBH consistent with cosmic microwave background measurements is only possible in the second (b) case. We calculate the masses of the produced PBH and find that they are below the Hawking (black hole) evaporation limit, so that they cannot be part of the current dark matter in our Universe.</description>
189 <dc:creator>Shuntaro Aoki, Ryotaro Ishikawa and Sergei V Ketov</dc:creator>
190 <dc:date>2023-02-15T00:00:00Z</dc:date>
191 <dc:source>Classical and Quantum Gravity</dc:source>
192 <iop:authors>Shuntaro Aoki <em>et al</em></iop:authors>
193 <iop:citation>Shuntaro Aoki <em>et al</em> 2023 <em>Classical and Quantum Gravity</em> <b>40</b> 065002</iop:citation>
194 <iop:pdf>https://iopscience.iop.org/article/10.1088/1361-6382/acb884/pdf</iop:pdf>
195 <prism:coverDisplayDate>15/February/2023</prism:coverDisplayDate>
196 <prism:number>6</prism:number>
197 <prism:volume>40</prism:volume>
198 <prism:publicationName>Classical and Quantum Gravity</prism:publicationName>
199 <prism:startingPage>065002</prism:startingPage>
200 <prism:doi>10.1088/1361-6382/acb884</prism:doi>
201 </item>
202