Physical Review D最新文献

{"title":"Phenomenological model of gravitational self-force enhanced tides in inspiraling binary neutron stars","authors":"Natalie Williams, Patricia Schmidt, Geraint Pratten","doi":"10.1103/physrevd.110.104013","DOIUrl":"https://doi.org/10.1103/physrevd.110.104013","url":null,"abstract":"Gravitational waves from inspiraling binary neutron stars provide unique access to ultradense nuclear matter and offer the ability to constrain the currently unknown neutron star equation-of-state through tidal measurements. This, however, requires the availability of accurate and efficient tidal waveform models. In this paper we present <span>p</span>henom<span>gsf</span>, a new phenomenological tidal phase model for the inspiral of neutron stars in the frequency domain, which captures the gravitational self-force informed tidal contributions of the time-domain effective-one-body model <span>teobr</span>esum<span>s</span>. <span>p</span>henom<span>gsf</span> is highly faithful and computationally efficient, and by choosing a modular approach, it can be used in conjunction with <i>any</i> frequency-domain binary black hole waveform model to generate the complete phase for a binary neutron star inspiral. <span>p</span>henom<span>gsf</span> is valid for neutron star binaries with unequal masses and mass ratios between 1 and 3, and dimensionless tidal deformabilities up to 5000. Furthermore, <span>p</span>henom<span>gsf</span> does not assume universal relations or parametrized equations of state, hence allowing for exotic matter analyses and beyond standard model physics investigations. We demonstrate the efficacy and accuracy of our model through comparisons against <span>teobr</span>esum<span>s</span>, numerical relativity waveforms and full Bayesian inference, including a reanalysis of the binary neutron star observation GW170817.","PeriodicalId":20167,"journal":{"name":"Physical Review D","volume":"69 1","pages":""},"PeriodicalIF":5.0,"publicationDate":"2024-11-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142597274","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Muon𝑔−2and lepton flavor violation in supersymmetric GUTs","authors":"Mario E. Gómez, Smaragda Lola, Qaisar Shafi, Cem Salih Ün","doi":"10.1103/physrevd.110.095003","DOIUrl":"https://doi.org/10.1103/physrevd.110.095003","url":null,"abstract":"We present a class of supersymmetric (SUSY) GUT models that can explain the apparent discrepancy between the SM predictions and experimental values of muon &lt;mjx-container ctxtmenu_counter=\"43\" ctxtmenu_oldtabindex=\"1\" jax=\"CHTML\" overflow=\"linebreak\" role=\"tree\" sre-explorer- style=\"font-size: 100.7%;\" tabindex=\"0\"&gt;&lt;mjx-math data-semantic-structure=\"(3 0 1 2)\"&gt;&lt;mjx-mrow data-semantic-children=\"0,2\" data-semantic-content=\"1\" data-semantic- data-semantic-owns=\"0 1 2\" data-semantic-role=\"subtraction\" data-semantic-speech=\"g minus 2\" data-semantic-type=\"infixop\"&gt;&lt;mjx-mi data-semantic-annotation=\"clearspeak:simple\" data-semantic-font=\"italic\" data-semantic- data-semantic-parent=\"3\" data-semantic-role=\"latinletter\" data-semantic-type=\"identifier\"&gt;&lt;mjx-c&gt;𝑔&lt;/mjx-c&gt;&lt;/mjx-mi&gt;&lt;mjx-mo data-semantic- data-semantic-operator=\"infixop,−\" data-semantic-parent=\"3\" data-semantic-role=\"subtraction\" data-semantic-type=\"operator\" space=\"3\"&gt;&lt;mjx-c&gt;−&lt;/mjx-c&gt;&lt;/mjx-mo&gt;&lt;mjx-mn data-semantic-annotation=\"clearspeak:simple\" data-semantic-font=\"normal\" data-semantic- data-semantic-parent=\"3\" data-semantic-role=\"integer\" data-semantic-type=\"number\" space=\"3\"&gt;&lt;mjx-c&gt;2&lt;/mjx-c&gt;&lt;/mjx-mn&gt;&lt;/mjx-mrow&gt;&lt;/mjx-math&gt;&lt;/mjx-container&gt; while providing testable signals for lepton flavor violation in charged lepton decays. Moreover, these models predict LSP neutralino abundance that is compatible with the Planck dark matter bounds. We find that scenarios in the framework of &lt;mjx-container ctxtmenu_counter=\"44\" ctxtmenu_oldtabindex=\"1\" jax=\"CHTML\" overflow=\"linebreak\" role=\"tree\" sre-explorer- style=\"font-size: 100.7%;\" tabindex=\"0\"&gt;&lt;mjx-math breakable=\"true\" data-semantic-children=\"28,31,35\" data-semantic-content=\"7,15\" data-semantic- data-semantic-owns=\"28 7 31 15 35\" data-semantic-role=\"multiplication\" data-semantic-speech=\"upper S upper U left parenthesis 4 right parenthesis Subscript c times upper S upper U left parenthesis 2 right parenthesis Subscript upper L times upper S upper U left parenthesis 2 right parenthesis Subscript upper R\" data-semantic-structure=\"(32 (28 0 26 1 27 (6 (23 2 3 4) 5)) 7 (31 8 29 9 30 (14 (24 10 11 12) 13)) 15 (35 16 33 17 34 (22 (25 18 19 20) 21)))\" data-semantic-type=\"infixop\"&gt;&lt;mjx-mrow data-semantic-added=\"true\" data-semantic-annotation=\"clearspeak:unit\" data-semantic-children=\"0,1,6\" data-semantic-content=\"26,27\" data-semantic- data-semantic-owns=\"0 26 1 27 6\" data-semantic-parent=\"32\" data-semantic-role=\"implicit\" data-semantic-type=\"infixop\"&gt;&lt;mjx-mi data-semantic-annotation=\"clearspeak:simple\" data-semantic-font=\"italic\" data-semantic- data-semantic-parent=\"28\" data-semantic-role=\"latinletter\" data-semantic-type=\"identifier\"&gt;&lt;mjx-c&gt;𝑆&lt;/mjx-c&gt;&lt;/mjx-mi&gt;&lt;mjx-mo data-semantic-added=\"true\" data-semantic- data-semantic-operator=\"infixop,⁢\" data-semantic-parent=\"28\" data-semantic-role=\"multiplication\" data-semantic-type=\"operator\"&gt;&lt;mjx-c&gt;⁢&lt;/mjx-c&gt;&lt;/mjx-mo&gt;&lt;mjx-mi data-semantic-annotation=\"clearspeak:simple\" data-semantic-font=\"italic\" data-semantic- data-semanti","PeriodicalId":20167,"journal":{"name":"Physical Review D","volume":"95 1","pages":""},"PeriodicalIF":5.0,"publicationDate":"2024-11-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142597275","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Dilatonic dynamics of baryonic crystals, branes, and spheres","authors":"Jahmall Bersini, Alessandra D’Alise, Francesco Sannino, Matías Torres","doi":"10.1103/physrevd.110.094008","DOIUrl":"https://doi.org/10.1103/physrevd.110.094008","url":null,"abstract":"We systematically analyze the impact of dilatonic dynamics on Skyrme spheres, crystals, and branes. The effects of the dilatonic model parameters, encompassing different underlying near-conformal dynamics, on the macroscopic properties of skyrmions such as their mass and radius are discussed. For spheres and crystals we identify special values of the ratio of the decay constants for which the second order differential equations reduce to a solvable first order system. Additionally, in the case of the crystals, the dilaton presence spatially separates the baryon and isospin charge distributions. For branes, we show how the dilaton smooths out their configurations. Our results are expected to have wide implications from the study of near-conformal dynamics stemming from QCD-like theories to phenomenological investigations of nuclear matter in extreme regimes.","PeriodicalId":20167,"journal":{"name":"Physical Review D","volume":"38 1","pages":""},"PeriodicalIF":5.0,"publicationDate":"2024-11-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142598157","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Investigating cosmic histories with a stiff era through gravitational waves","authors":"Hannah Duval, Sachiko Kuroyanagi, Alberto Mariotti, Alba Romero-Rodríguez, Mairi Sakellariadou","doi":"10.1103/physrevd.110.103503","DOIUrl":"https://doi.org/10.1103/physrevd.110.103503","url":null,"abstract":"We investigate the potential of gravitational-wave background searches to constrain cosmic histories characterized by a stiff equation of state, preceded by a period of matter domination. Such a scenario leads to a characteristic peak in the primordial gravitational-wave spectrum originating from cosmological inflation. Assuming instant transitions between distinct epochs, which allows for an analytical treatment of the gravitational-wave spectrum, we perform a Bayesian inference analysis to derive constraints from the first three observing runs of the LIGO-Virgo-KAGRA Collaboration. Additionally, we consider a smooth transition, employing an axionlike particle physics model, and highlight the differences compared to the instant transition approximation. Finally, we forecast detection prospects for such a cosmic history through future gravitational-wave experiments.","PeriodicalId":20167,"journal":{"name":"Physical Review D","volume":"196 1","pages":""},"PeriodicalIF":5.0,"publicationDate":"2024-11-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142594368","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"QCD corrections at subleading power for inclusive nonleptonic𝑏→𝑐⁢¯𝑢⁢𝑑decays","authors":"Thomas Mannel, Daniel Moreno, Alexei A. Pivovarov","doi":"10.1103/physrevd.110.094011","DOIUrl":"https://doi.org/10.1103/physrevd.110.094011","url":null,"abstract":"In this paper we compute the next-to-leading order (NLO) QCD corrections for the inclusive nonleptonic decay rates of <mjx-container ctxtmenu_counter=\"31\" ctxtmenu_oldtabindex=\"1\" jax=\"CHTML\" overflow=\"linebreak\" role=\"tree\" sre-explorer- style=\"font-size: 100.7%;\" tabindex=\"0\"><mjx-math data-semantic-structure=\"0\"><mjx-mi data-semantic-annotation=\"clearspeak:simple\" data-semantic-font=\"italic\" data-semantic- data-semantic-role=\"latinletter\" data-semantic-speech=\"upper B\" data-semantic-type=\"identifier\"><mjx-c>𝐵</mjx-c></mjx-mi></mjx-math></mjx-container> hadrons at subleading power of the heavy quark expansion. In particular, we discuss the coefficient of the chromomagnetic moment parameter <mjx-container ctxtmenu_counter=\"32\" ctxtmenu_oldtabindex=\"1\" jax=\"CHTML\" overflow=\"linebreak\" role=\"tree\" sre-explorer- style=\"font-size: 100.7%;\" tabindex=\"0\"><mjx-math data-semantic-structure=\"(2 0 1)\"><mjx-msub data-semantic-children=\"0,1\" data-semantic- data-semantic-owns=\"0 1\" data-semantic-role=\"greekletter\" data-semantic-speech=\"mu Subscript upper G\" data-semantic-type=\"subscript\"><mjx-mi data-semantic-annotation=\"clearspeak:simple\" data-semantic-font=\"italic\" data-semantic- data-semantic-parent=\"2\" data-semantic-role=\"greekletter\" data-semantic-type=\"identifier\"><mjx-c>𝜇</mjx-c></mjx-mi><mjx-script style=\"vertical-align: -0.15em;\"><mjx-mi data-semantic-annotation=\"clearspeak:simple\" data-semantic-font=\"italic\" data-semantic- data-semantic-parent=\"2\" data-semantic-role=\"latinletter\" data-semantic-type=\"identifier\" size=\"s\"><mjx-c>𝐺</mjx-c></mjx-mi></mjx-script></mjx-msub></mjx-math></mjx-container>, which has a large uncertainty at leading order due to its dependence on the renormalization scale. We find that the renormalization-scale dependence of this coefficient is significantly reduced, thereby reducing the theoretical uncertainty of the coefficient and, consequently, the rates. The sign of the coefficient becomes stable, and we estimate that the NLO corrections will increase the decay rates by around 2%.","PeriodicalId":20167,"journal":{"name":"Physical Review D","volume":"2 1","pages":""},"PeriodicalIF":5.0,"publicationDate":"2024-11-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142597276","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Specific heats for quantum BTZ black holes in extended thermodynamics","authors":"Clifford V. Johnson, Roberto Nazario","doi":"10.1103/physrevd.110.106004","DOIUrl":"https://doi.org/10.1103/physrevd.110.106004","url":null,"abstract":"It was shown recently that extended black hole thermodynamics, where the cosmological constant is a dynamical variable, giving rise to a pressure &lt;mjx-container ctxtmenu_counter=\"48\" ctxtmenu_oldtabindex=\"1\" jax=\"CHTML\" overflow=\"linebreak\" role=\"tree\" sre-explorer- style=\"font-size: 100.7%;\" tabindex=\"0\"&gt;&lt;mjx-math data-semantic-structure=\"0\"&gt;&lt;mjx-mi data-semantic-annotation=\"clearspeak:simple\" data-semantic-font=\"italic\" data-semantic- data-semantic-role=\"latinletter\" data-semantic-speech=\"p\" data-semantic-type=\"identifier\"&gt;&lt;mjx-c&gt;𝑝&lt;/mjx-c&gt;&lt;/mjx-mi&gt;&lt;/mjx-math&gt;&lt;/mjx-container&gt; and its conjugate volume &lt;mjx-container ctxtmenu_counter=\"49\" ctxtmenu_oldtabindex=\"1\" jax=\"CHTML\" overflow=\"linebreak\" role=\"tree\" sre-explorer- style=\"font-size: 100.7%;\" tabindex=\"0\"&gt;&lt;mjx-math data-semantic-structure=\"0\"&gt;&lt;mjx-mi data-semantic-annotation=\"clearspeak:simple\" data-semantic-font=\"italic\" data-semantic- data-semantic-role=\"latinletter\" data-semantic-speech=\"upper V\" data-semantic-type=\"identifier\"&gt;&lt;mjx-c&gt;𝑉&lt;/mjx-c&gt;&lt;/mjx-mi&gt;&lt;/mjx-math&gt;&lt;/mjx-container&gt;, can be given a natural setting in the context of braneworld models. We study the specific heat capacities &lt;mjx-container ctxtmenu_counter=\"50\" ctxtmenu_oldtabindex=\"1\" jax=\"CHTML\" overflow=\"linebreak\" role=\"tree\" sre-explorer- style=\"font-size: 100.7%;\" tabindex=\"0\"&gt;&lt;mjx-math data-semantic-annotation=\"clearspeak:simple\" data-semantic-children=\"2,6\" data-semantic-content=\"7,0\" data-semantic- data-semantic-owns=\"2 7 6\" data-semantic-role=\"simple function\" data-semantic-speech=\"upper C Subscript p Baseline left parenthesis upper T right parenthesis\" data-semantic-structure=\"(8 (2 0 1) 7 (6 3 4 5))\" data-semantic-type=\"appl\"&gt;&lt;mjx-msub data-semantic-children=\"0,1\" data-semantic- data-semantic-owns=\"0 1\" data-semantic-parent=\"8\" data-semantic-role=\"simple function\" data-semantic-type=\"subscript\"&gt;&lt;mjx-mi data-semantic-annotation=\"clearspeak:simple\" data-semantic-font=\"italic\" data-semantic- data-semantic-operator=\"appl\" data-semantic-parent=\"2\" data-semantic-role=\"simple function\" data-semantic-type=\"identifier\"&gt;&lt;mjx-c&gt;𝐶&lt;/mjx-c&gt;&lt;/mjx-mi&gt;&lt;mjx-script style=\"vertical-align: -0.15em; margin-left: -0.018em;\"&gt;&lt;mjx-mi data-semantic-annotation=\"clearspeak:simple\" data-semantic-font=\"italic\" data-semantic- data-semantic-parent=\"2\" data-semantic-role=\"latinletter\" data-semantic-type=\"identifier\" size=\"s\"&gt;&lt;mjx-c&gt;𝑝&lt;/mjx-c&gt;&lt;/mjx-mi&gt;&lt;/mjx-script&gt;&lt;/mjx-msub&gt;&lt;mjx-mo data-semantic-added=\"true\" data-semantic- data-semantic-operator=\"appl\" data-semantic-parent=\"8\" data-semantic-role=\"application\" data-semantic-type=\"punctuation\"&gt;&lt;mjx-c&gt;⁡&lt;/mjx-c&gt;&lt;/mjx-mo&gt;&lt;mjx-mrow data-semantic-added=\"true\" data-semantic-children=\"4\" data-semantic-content=\"3,5\" data-semantic- data-semantic-owns=\"3 4 5\" data-semantic-parent=\"8\" data-semantic-role=\"leftright\" data-semantic-type=\"fenced\"&gt;&lt;mjx-mo data-semantic- data-semantic-operator=\"fenced\" data-semantic-parent=\"6\" data-semantic-role=\"open\" data-semantic-type=\"fence\" style=\"vertical-align: -0.02em;\"&gt;&lt;mjx","PeriodicalId":20167,"journal":{"name":"Physical Review D","volume":"41 1","pages":""},"PeriodicalIF":5.0,"publicationDate":"2024-11-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142594365","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Measuring the circular polarization of gravitational waves with pulsar timing arrays","authors":"N. M. Jiménez Cruz, Ameek Malhotra, Gianmassimo Tasinato, Ivonne Zavala","doi":"10.1103/physrevd.110.103505","DOIUrl":"https://doi.org/10.1103/physrevd.110.103505","url":null,"abstract":"The circular polarization of the stochastic gravitational wave background (SGWB) is a key observable for characterizing the origin of the signal detected by Pulsar Timing Array (PTA) collaborations. Both the astrophysical and the cosmological SGWB can have a sizeable amount of circular polarization, due to Poisson fluctuations in the source properties for the former, and to parity violating processes in the early universe for the latter. Its measurement is challenging since PTA are blind to the circular polarization monopole, forcing us to turn to anisotropies for detection. We study the sensitivity of current and future PTA datasets to circular polarization anisotropies, focusing on realistic modelling of intrinsic and kinematic anisotropies for astrophysical and cosmological scenarios respectively. Our results indicate that the expected level of circular polarization for the astrophysical SGWB should be within the reach of near future datasets, while for cosmological SGWB circular polarization is a viable target for more advanced SKA-type experiments.","PeriodicalId":20167,"journal":{"name":"Physical Review D","volume":"2 1","pages":""},"PeriodicalIF":5.0,"publicationDate":"2024-11-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142594366","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Resonant conversion of gravitational waves in neutron star magnetospheres","authors":"Jamie I. McDonald, Sebastian A. R. Ellis","doi":"10.1103/physrevd.110.103003","DOIUrl":"https://doi.org/10.1103/physrevd.110.103003","url":null,"abstract":"High-frequency gravitational waves are the subject of rapidly growing interest in the theoretical and experimental community. In this work we calculate the resonant conversion of gravitational waves into photons in the magnetospheres of neutron stars via the inverse Gertsenshtein mechanism. The resonance occurs in regions where the vacuum birefringence effects cancel the classical plasma contribution to the photon dispersion relation, leading to a massless photon in the medium which becomes kinematically matched to the graviton. We set limits on the amplitude of a possible stochastic background of gravitational waves using X-ray and IR flux measurements of neutron stars. Using Chandra (2–8 keV) and NuSTAR (3–79 keV) observations of RX J1856.6-3754, we set strain limits &lt;mjx-container ctxtmenu_counter=\"28\" ctxtmenu_oldtabindex=\"1\" jax=\"CHTML\" overflow=\"linebreak\" role=\"tree\" sre-explorer- style=\"font-size: 100.7%;\" tabindex=\"0\"&gt;&lt;mjx-math breakable=\"true\" data-semantic-children=\"4,17\" data-semantic-content=\"5\" data-semantic- data-semantic-owns=\"4 5 17\" data-semantic-role=\"equality\" data-semantic-speech=\"h Subscript c Superscript limit Baseline asymptotically equals 10 Superscript negative 26 Baseline en dash 10 Superscript negative 24\" data-semantic-structure=\"(18 (4 (3 0 1) 2) 5 (17 (10 6 (9 7 8)) 11 (16 12 (15 13 14))))\" data-semantic-type=\"relseq\"&gt;&lt;mjx-msubsup data-semantic-children=\"0,1,2\" data-semantic-collapsed=\"(4 (3 0 1) 2)\" data-semantic- data-semantic-owns=\"0 1 2\" data-semantic-parent=\"18\" data-semantic-role=\"latinletter\" data-semantic-type=\"subsup\"&gt;&lt;mjx-mi data-semantic-annotation=\"clearspeak:simple\" data-semantic-font=\"italic\" data-semantic- data-semantic-parent=\"4\" data-semantic-role=\"latinletter\" data-semantic-type=\"identifier\"&gt;&lt;mjx-c&gt;ℎ&lt;/mjx-c&gt;&lt;/mjx-mi&gt;&lt;mjx-script style=\"vertical-align: -0.247em; margin-left: 0px;\"&gt;&lt;mjx-mi data-semantic-font=\"normal\" data-semantic- data-semantic-parent=\"4\" data-semantic-role=\"limit function\" data-semantic-type=\"function\" size=\"s\"&gt;&lt;mjx-c noic=\"true\" style=\"padding-top: 0.706em;\"&gt;l&lt;/mjx-c&gt;&lt;mjx-c noic=\"true\" style=\"padding-top: 0.706em;\"&gt;i&lt;/mjx-c&gt;&lt;mjx-c style=\"padding-top: 0.706em;\"&gt;m&lt;/mjx-c&gt;&lt;/mjx-mi&gt;&lt;mjx-spacer style=\"margin-top: 0.271em;\"&gt;&lt;/mjx-spacer&gt;&lt;mjx-mi data-semantic-annotation=\"clearspeak:simple\" data-semantic-font=\"italic\" data-semantic- data-semantic-parent=\"4\" data-semantic-role=\"latinletter\" data-semantic-type=\"identifier\" size=\"s\"&gt;&lt;mjx-c&gt;𝑐&lt;/mjx-c&gt;&lt;/mjx-mi&gt;&lt;/mjx-script&gt;&lt;/mjx-msubsup&gt;&lt;mjx-break size=\"4\"&gt;&lt;/mjx-break&gt;&lt;mjx-mo data-semantic- data-semantic-operator=\"relseq,≃\" data-semantic-parent=\"18\" data-semantic-role=\"equality\" data-semantic-type=\"relation\"&gt;&lt;mjx-c&gt;≃&lt;/mjx-c&gt;&lt;/mjx-mo&gt;&lt;mjx-mrow data-semantic-added=\"true\" data-semantic-children=\"10,16\" data-semantic-content=\"11\" data-semantic- data-semantic-owns=\"10 11 16\" data-semantic-parent=\"18\" data-semantic-role=\"dash\" data-semantic-type=\"infixop\" space=\"4\"&gt;&lt;mjx-msup data-semantic-children=\"6,9\" data-semantic- data-semantic-owns=\"6 9\" data-se","PeriodicalId":20167,"journal":{"name":"Physical Review D","volume":"3 1","pages":""},"PeriodicalIF":5.0,"publicationDate":"2024-11-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142594369","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Slowly rotating anisotropic neutron stars with a parametrized equation of state","authors":"L. M. Becerra, E. A. Becerra-Vergara, F. D. Lora-Clavijo","doi":"10.1103/physrevd.110.103004","DOIUrl":"https://doi.org/10.1103/physrevd.110.103004","url":null,"abstract":"In this work, we study the impact of anisotropy on slowly rotating neutron stars by extending the Hartle–Thorne formalism in general relativity to include anisotropy in pressure up to second order in the angular velocity. We assess the presence of anisotropy within the star by employing a quasi-local relationship. Our results show that the ratio between the gravitational mass of the fastest anisotropic rotating configurations and the corresponding nonrotating ones ranges from 1.12 to 1.25, consistent with recent findings. We develop universal relations for the moment of inertia, binding energy, and quadrupole moment of the rotating stars. These relations are tested against various equations of state, which were modeled by a piecewise polytropic function with continuous sound speed.","PeriodicalId":20167,"journal":{"name":"Physical Review D","volume":"17 1","pages":""},"PeriodicalIF":5.0,"publicationDate":"2024-11-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142594549","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Different origins of running in the 2Dℂ⁢ℙ⁡(1)model","authors":"Kasra Kiaee, Alexander Monin","doi":"10.1103/physrevd.110.096007","DOIUrl":"https://doi.org/10.1103/physrevd.110.096007","url":null,"abstract":"We revisit the computation of the beta function in the two-dimensional <mjx-container ctxtmenu_counter=\"5\" ctxtmenu_oldtabindex=\"1\" jax=\"CHTML\" overflow=\"linebreak\" role=\"tree\" sre-explorer- style=\"font-size: 100.7%;\" tabindex=\"0\"><mjx-math data-semantic-structure=\"(6 0 5 (4 1 2 3))\"><mjx-mrow data-semantic-annotation=\"clearspeak:simple\" data-semantic-children=\"0,4\" data-semantic-content=\"5,0\" data-semantic- data-semantic-owns=\"0 5 4\" data-semantic-role=\"simple function\" data-semantic-speech=\"double struck upper C upper P left parenthesis 1 right parenthesis\" data-semantic-type=\"appl\"><mjx-mi data-semantic-annotation=\"clearspeak:simple\" data-semantic-font=\"double-struck\" data-semantic- data-semantic-operator=\"appl\" data-semantic-parent=\"6\" data-semantic-role=\"simple function\" data-semantic-type=\"identifier\"><mjx-c noic=\"true\" style=\"padding-top: 0.669em;\">ℂ</mjx-c><mjx-c style=\"padding-top: 0.669em;\">ℙ</mjx-c></mjx-mi><mjx-mo data-semantic-added=\"true\" data-semantic- data-semantic-operator=\"appl\" data-semantic-parent=\"6\" data-semantic-role=\"application\" data-semantic-type=\"punctuation\"><mjx-c>⁡</mjx-c></mjx-mo><mjx-mrow data-semantic-added=\"true\" data-semantic-children=\"2\" data-semantic-content=\"1,3\" data-semantic- data-semantic-owns=\"1 2 3\" data-semantic-parent=\"6\" data-semantic-role=\"leftright\" data-semantic-type=\"fenced\"><mjx-mo data-semantic- data-semantic-operator=\"fenced\" data-semantic-parent=\"4\" data-semantic-role=\"open\" data-semantic-type=\"fence\" style=\"vertical-align: -0.02em;\"><mjx-c>(</mjx-c></mjx-mo><mjx-mn data-semantic-annotation=\"clearspeak:simple\" data-semantic-font=\"normal\" data-semantic- data-semantic-parent=\"4\" data-semantic-role=\"integer\" data-semantic-type=\"number\"><mjx-c>1</mjx-c></mjx-mn><mjx-mo data-semantic- data-semantic-operator=\"fenced\" data-semantic-parent=\"4\" data-semantic-role=\"close\" data-semantic-type=\"fence\" style=\"vertical-align: -0.02em;\"><mjx-c>)</mjx-c></mjx-mo></mjx-mrow></mjx-mrow></mjx-math></mjx-container> sigma model. We show that in different schemes, different diagrams are responsible for the running, such as momentum-independent tadpoles or even UV-finite bubble diagrams. We also comment on the relation between the beta functions and the energy dependence of scattering amplitudes.","PeriodicalId":20167,"journal":{"name":"Physical Review D","volume":"70 1","pages":""},"PeriodicalIF":5.0,"publicationDate":"2024-11-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142597249","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}