Classical and Quantum Gravity最新文献_第7页

Measuring the boson mass of fuzzy dark matter with stellar proper motions 用恒星正确运动测量模糊暗物质的玻色子质量

IF 3.5 3区物理与天体物理

Classical and Quantum Gravity Pub Date : 2025-03-26 DOI: 10.1088/1361-6382/adc17f

Gabriel d’Andrade Furlanetto, Riccardo Della Monica and Ivan De Martino

{"title":"Measuring the boson mass of fuzzy dark matter with stellar proper motions","authors":"Gabriel d’Andrade Furlanetto, Riccardo Della Monica and Ivan De Martino","doi":"10.1088/1361-6382/adc17f","DOIUrl":"https://doi.org/10.1088/1361-6382/adc17f","url":null,"abstract":"Fuzzy dark matter (FDM) is among the most suitable candidates to replace WIMPs and to resolve the puzzling mystery of dark matter (DM). A galactic DM halo made of these ultralight bosonic particles leads to the formation of a solitonic core surrounded by quantum interference patterns that, on average, reproduce a Navarro-Frenk-White-like mass density profile in the outskirts of the halo. The structure of such a core is determined once the boson mass and the total mass of the halo are set. We investigated the capability of future astrometric Theia-like missions to detect the properties of such a halo within the FDM model, namely the boson mass and the core radius. To this aim, we built mock catalogs containing three-dimensional positions and velocities of stars within a target dwarf galaxy. We exploited these catalogs using a Markov Chain Monte Carlo algorithm and found that measuring the proper motion of at least 2000 stars within the target galaxy, with uncertainty km s−1 on the velocity components, will constrain the boson mass and the core radius with 3% accuracy. Furthermore, the transition between the solitonic core and the outermost NFW-like density profile could be detected with an uncertainty of 7%. Such results would not only help to confirm the existence of FDM, but they would also be useful for alleviating the current tension between galactic and cosmological estimations of the boson mass, or demonstrating the need for multiple particles with a broad mass spectrum as naturally arise String Axiverse.","PeriodicalId":10282,"journal":{"name":"Classical and Quantum Gravity","volume":"29 1","pages":""},"PeriodicalIF":3.5,"publicationDate":"2025-03-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143703295","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"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}

引用次数: 0

New edge modes and corner charges for first-order symmetries of 4D gravity 四维引力一阶对称性的新边模和角荷

IF 3.5 3区物理与天体物理

Classical and Quantum Gravity Pub Date : 2025-03-25 DOI: 10.1088/1361-6382/adbfee

Simon Langenscheidt and Daniele Oriti

引用次数: 0

Are dark matter and dark energy omnipresent? 暗物质和暗能量是否无所不在？

IF 3.5 3区物理与天体物理

Classical and Quantum Gravity Pub Date : 2025-03-21 DOI: 10.1088/1361-6382/adbed1

Richard Lieu

{"title":"Are dark matter and dark energy omnipresent?","authors":"Richard Lieu","doi":"10.1088/1361-6382/adbed1","DOIUrl":"https://doi.org/10.1088/1361-6382/adbed1","url":null,"abstract":"A set of temporal singularities (transients) in the mass-energy density and pressure, bearing a specific mathematical structure which represents a new solution to the continuity equation (i.e. conservation of mass-energy) and satisfying the strong energy condition, is proposed to account for the expansion history of a homogeneous Universe, and the formation and binding of large scale structures as a continuum approximation of their cumulative effects. These singularities are unobservable because they occur rarely in time and are unresolvably fast, and that could be the reason why dark matter and dark energy have not been found. Implication on inflationary cosmology is discussed. The origin of these temporal singularities is unknown, safe to say that the same is true of the moment of the Big Bang itself. This work complements a recent paper, where a topological defect in the form of a spatial, spherical shell of density singularity giving rise to a 1/r attractive force (to test particles of positive mass) but zero integrated mass over a large volume of space, was proposed to solve the dark matter problem in bound structures but not cosmic expansion. The idea also involved a negative density, which is not present in the current model.","PeriodicalId":10282,"journal":{"name":"Classical and Quantum Gravity","volume":"56 1","pages":""},"PeriodicalIF":3.5,"publicationDate":"2025-03-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143665868","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"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}

引用次数: 0

Boson stars in non-minimal gravity 非最小引力中的玻色子星

IF 3.5 3区物理与天体物理

Classical and Quantum Gravity Pub Date : 2025-03-21 DOI: 10.1088/1361-6382/adbed3

Sanjeev Kumar, Susheel Arora, Usha Kulshreshtha and Daya Shankar Kulshreshtha

{"title":"Boson stars in non-minimal gravity","authors":"Sanjeev Kumar, Susheel Arora, Usha Kulshreshtha and Daya Shankar Kulshreshtha","doi":"10.1088/1361-6382/adbed3","DOIUrl":"https://doi.org/10.1088/1361-6382/adbed3","url":null,"abstract":"We study the boson star solutions in a theory involving a complex scalar field in a conical scalar field potential: in the presence of non-minimal gravity given by the term: in the action, where ξ is a constant parameter that couples the complex scalar field Φ with the Ricci scalar R and is treated, in our work, as a free parameter. The theory has one more free parameter denoted by (where ω is the frequency of the complex scalar field). Here G is the Newton’s gravitational constant, λ is a constant used in the definition of the scalar field potential. We find that the acceptable boson star solutions exist in this theory that involves non-minimal gravity as above. For obtaining the acceptable boson star solutions, we obtain the domain of existence of our free parameters ξ and α for which the boson star solutions exist and then study the various properties of the boson star solutions. In our studies, as we trace the evolution of our solutions along the relevant path, emanating from the solutions corresponding to the absence of gravitational field, we observe a steady increase in mass with radius. Employing principles from catastrophe theory, we find that this trajectory remains stable until it reaches the maximum mass value. This leads to the characteristic spiraling behavior of the mass-radius curve, a well-known feature in compact star models signaling the onset of instability.","PeriodicalId":10282,"journal":{"name":"Classical and Quantum Gravity","volume":"214 1","pages":""},"PeriodicalIF":3.5,"publicationDate":"2025-03-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143665870","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"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}

引用次数: 0

A sensitivity curve approach to tuning a pulsar timing array in the detection era 探测时代脉冲星定时阵列调谐的灵敏度曲线方法

IF 3.5 3区物理与天体物理

Classical and Quantum Gravity Pub Date : 2025-03-21 DOI: 10.1088/1361-6382/adbbab

Jeremy G Baier, Jeffrey S Hazboun and Joseph D Romano

{"title":"A sensitivity curve approach to tuning a pulsar timing array in the detection era","authors":"Jeremy G Baier, Jeffrey S Hazboun and Joseph D Romano","doi":"10.1088/1361-6382/adbbab","DOIUrl":"https://doi.org/10.1088/1361-6382/adbbab","url":null,"abstract":"As pulsar timing arrays (PTAs) transition into the detection era of the stochastic gravitational wave background (GWB), it is important for PTA collaborations to review and possibly revise their observing campaigns. The detection of a ‘single source’ would be a boon for gravitational astrophysics, as such a source would emit gravitational waves for millions of years in the PTA frequency band. Here we present generic methods for studying the effects of various observational strategies, taking advantage of detector sensitivity curves, i.e. noise-averaged, frequency-domain detection statistics. The statistical basis for these methods is presented along with myriad examples of how to tune a detector towards single, deterministic signals or a stochastic background. We demonstrate that trading observations of the worst pulsars for high cadence campaigns on the best pulsars increases sensitivity to single sources at high frequencies while hedging losses in GWB and single source sensitivity at low frequencies. We also find that sky-targeted observing campaigns yield minimal sensitivity improvements compared with other PTA tuning options. Lastly, we show the importance of the uncorrelated half of the GWB, i.e. the pulsar-term, as an increasingly prominent sources of noise and show the impact of this emerging noise source on various PTA configurations.","PeriodicalId":10282,"journal":{"name":"Classical and Quantum Gravity","volume":"22 1","pages":""},"PeriodicalIF":3.5,"publicationDate":"2025-03-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143665902","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"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}

引用次数: 0

Experiment demonstration of tilt-to-length coupling suppression by beam-alignment-mechanism 用波束对准机制抑制倾斜-长度耦合的实验论证

IF 3.5 3区物理与天体物理

Classical and Quantum Gravity Pub Date : 2025-03-21 DOI: 10.1088/1361-6382/adbed2

Peng Qiu, Xiang Lin, Yurong Liang, Hao Yan, Haixing Miao and Zebing Zhou

{"title":"Experiment demonstration of tilt-to-length coupling suppression by beam-alignment-mechanism","authors":"Peng Qiu, Xiang Lin, Yurong Liang, Hao Yan, Haixing Miao and Zebing Zhou","doi":"10.1088/1361-6382/adbed2","DOIUrl":"https://doi.org/10.1088/1361-6382/adbed2","url":null,"abstract":"Tilt-to-length (TTL) noise, caused by angular jitter and misalignment, is a major noise source in the inter-satellite interferometer for gravitational wave detection. However, the required level of axis alignment of the optical components is beyond the current state of the art. A set of optical parallel plates, called beam alignment mechanism (BAM), is proposed by LISA to compensate for the alignment error. In this paper, we show a prototype design of the BAM and demonstrate its performance in a ground-based optical system. We derive the BAM theoretical model, which agrees well with the numerical simulation. Experimental results reveal that the BAM can achieve lateral displacement compensation of the optical axis with a resolution of 1 µm across a range of about 0.5 mm. Furthermore, the TTL coefficient is reduced from about 0.3 mm rad−1 to about 5 µm rad−1, satisfying the preliminary requirements for LISA and TianQin. These findings confirm the efficacy of the BAM in suppressing TTL noise, offering a promising solution for space-based gravitational wave detection.","PeriodicalId":10282,"journal":{"name":"Classical and Quantum Gravity","volume":"29 1","pages":""},"PeriodicalIF":3.5,"publicationDate":"2025-03-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143665869","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"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}

引用次数: 0

Can quasars, triggered by mergers, account for NANOGrav’s stochastic gravitational wave background? 由合并引发的类星体能解释nanogravity的随机引力波背景吗？

IF 3.5 3区物理与天体物理

Classical and Quantum Gravity Pub Date : 2025-03-20 DOI: 10.1088/1361-6382/adbda6

Ágnes Kis-Tóth, Zoltán Haiman and Zsolt Frei

{"title":"Can quasars, triggered by mergers, account for NANOGrav’s stochastic gravitational wave background?","authors":"Ágnes Kis-Tóth, Zoltán Haiman and Zsolt Frei","doi":"10.1088/1361-6382/adbda6","DOIUrl":"https://doi.org/10.1088/1361-6382/adbda6","url":null,"abstract":"The stochastic gravitational wave (GW) background recently discovered by several pulsar timing array experiments is consistent with arising from a population of coalescing super-massive black hole binaries. The amplitude of the background is somewhat higher than expected in most previous population models or from the local mass density observations. Such binaries are expected to be produced in galaxy mergers, which are also thought to trigger bright quasar activity. Under the assumptions that (i) a fraction of all quasars are associated with mergers, (ii) the typical quasar lifetime is , and (iii) adopting Eddington ratios for the luminosity of quasars, we compute the GW background associated directly with the empirically measured quasar luminosity function. This approach bypasses the need to model the cosmological evolution of black holes or galaxy mergers from simulations or semi-analytical models. We find the amplitude matching the value measured by NANOGrav. Our results are consistent with most quasars being associated with black hole binaries and being the sources of the GW background, and imply a joint constraint on , and the typical mass ratio . The signal in this case would be dominated by relatively distant sources at , at the peak of quasar activity. Similarly to other models, our results remain in tension with the local super-massive black hole mass density.","PeriodicalId":10282,"journal":{"name":"Classical and Quantum Gravity","volume":"56 1","pages":""},"PeriodicalIF":3.5,"publicationDate":"2025-03-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143661266","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"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}

引用次数: 0

Unique Carrollian manifolds emerging from Einstein spacetimes 爱因斯坦时空中出现的独特的卡罗流形

IF 3.5 3区物理与天体物理

Classical and Quantum Gravity Pub Date : 2025-03-19 DOI: 10.1088/1361-6382/adbb4e

Samuel Blitz, David McNutt and Pawel Nurowski

引用次数: 0

A MIMO system identification approach for the longitudinal control of the filter cavity of the advanced virgo gravitational-wave detector 先进处女座引力波探测器滤光腔纵向控制的MIMO系统辨识方法

IF 3.5 3区物理与天体物理

Classical and Quantum Gravity Pub Date : 2025-03-18 DOI: 10.1088/1361-6382/adb82b

E N Tapia San Martín, Y Guo, M Vardaro, Y Zhao, E Capocasa, R Flaminio and M Tacca

{"title":"A MIMO system identification approach for the longitudinal control of the filter cavity of the advanced virgo gravitational-wave detector","authors":"E N Tapia San Martín, Y Guo, M Vardaro, Y Zhao, E Capocasa, R Flaminio and M Tacca","doi":"10.1088/1361-6382/adb82b","DOIUrl":"https://doi.org/10.1088/1361-6382/adb82b","url":null,"abstract":"The sensitivity of the second generation ground-based gravitational-wave detectors is mostly limited by quantum noise (QN). The injection of frequency-dependent squeezed vacuum states into the output port of the interferometer has been shown to reduce QN across the entire detector bandwidth. Frequency dependent squeezed states are generated by reflecting a frequency independent squeezed states off a detuned optical cavity: the phase response of the cavity rotates the squeeze angle as a function of frequency. The precision of the longitudinal control of the such cavity, known as filter cavity, is one of the key parameters affecting the QN suppression factor. The target longitudinal control precision was achieved by simultaneously acting on both the cavity length and the frequency of the squeezing main laser. In this scenario, the analysis of this system requires a Multiple-Input Multiple-Output (MIMO) system model. In this work, we demonstrate that a MIMO model is required and show that a MIMO system identification technique is effective to characterize the system and improve its robustness. Ultimately we show that these techniques allow the design of robust filters that can keep the cavity residual length fluctuations below 1 pm, allowing for a QN reduction of 4.5 dB at high frequencies and 2 dB at low frequencies in the Advanced Virgo interferometer.","PeriodicalId":10282,"journal":{"name":"Classical and Quantum Gravity","volume":"183 1","pages":""},"PeriodicalIF":3.5,"publicationDate":"2025-03-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143641080","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"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}

引用次数: 0

Parametric solutions to the Kerr separatrix 克尔分离矩阵的参数解

IF 3.5 3区物理与天体物理

Classical and Quantum Gravity Pub Date : 2025-03-17 DOI: 10.1088/1361-6382/adba36

Tammy Ng and Edward Teo

引用次数: 0