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Universe
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Exploring Low-Frequency Gravitational Wave Sources: Waveforms, Detection and Sciences
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Exploring Low-Frequency Gravitational Wave Sources: Waveforms, Detection and Sciences

A special issue of Universe (ISSN 2218-1997). This special issue belongs to the section "Gravitation".

Deadline for manuscript submissions: 31 December 2025 | Viewed by 1855

Special Issue Editors

Prof. Dr. Wenbiao Han

E-Mail Website
Guest Editor
Shanghai Astronomical Observatory, CAS, Shanghai 200030, China
Interests: gravitational waves; tests of theories of gravity; machine learning; black hole physics
Special Issues, Collections and Topics in MDPI journals
Prof. Dr. Ziren Luo

E-Mail Website
Guest Editor
Institute of Mechanics, Chinese Academy of Sciences, Beijing 100190, China
Interests: gravitational waves; space-borne laser interferometry; metrology; precise measurement
Special Issues, Collections and Topics in MDPI journals
Dr. Shucheng Yang

E-Mail Website
Guest Editor
Shanghai Astronomical Observatory, Chineses Academy of Sciences, Shanghai, China
Interests: gravitational wave astronomy

Special Issue Information

Dear Colleagues,

Gravitational wave astronomy has developed significantly since the first detection of gravitational waves in 2015. Various detection methods will realize multi-wavelength observation, including ground-based or space-borne interferometers and pulsar timing arrays. In particular, the latter two will open a low-frequency window for observing gravitational waves, that is, Hz. They will enable the study of gravitational wave physics in the unexplored parameter space of strain and frequency, and then allow for an in-depth understanding of gravitational waves.

In this Special Issue, we will focus on low-frequency gravitational wave sources, waveform templates, data analysis, pipeline software development, and gravitational wave astronomy and physics such as astrophysical environments, tests of theories of gravity, cosmology, and black hole physics.

We welcome contributions on theories, simulations, and data analysis.

Prof. Dr. Wenbiao Han
Prof. Dr. Ziren Luo
Dr. Shucheng Yang
Guest Editors

Manuscript Submission Information

Manuscripts should be submitted online at www.mdpi.com by registering and logging in to this website. Once you are registered, click here to go to the submission form. Manuscripts can be submitted until the deadline. All submissions that pass pre-check are peer-reviewed. Accepted papers will be published continuously in the journal (as soon as accepted) and will be listed together on the special issue website. Research articles, review articles as well as short communications are invited. For planned papers, a title and short abstract (about 100 words) can be sent to the Editorial Office for announcement on this website.

Submitted manuscripts should not have been published previously, nor be under consideration for publication elsewhere (except conference proceedings papers). All manuscripts are thoroughly refereed through a single-blind peer-review process. A guide for authors and other relevant information for submission of manuscripts is available on the Instructions for Authors page. Universe is an international peer-reviewed open access monthly journal published by MDPI.

Please visit the Instructions for Authors page before submitting a manuscript. Submitted papers should be well formatted and use good English. Authors may use MDPI's English editing service prior to publication or during author revisions.

Keywords

  • gravitational waves
  • black holes
  • tests of theories of gravity
  • machine learning
  • data analysis

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Published Papers (3 papers)

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12 pages, 784 KiB  
Article
Thermal Profile of Accretion Disk Around Black Hole in 4D Einstein–Gauss–Bonnet Gravity
by Odilbek Kholmuminov, Bakhtiyor Narzilloev and Bobomurat Ahmedov
Universe 2025, 11(2), 38; https://doi.org/10.3390/universe11020038 - 26 Jan 2025
Viewed by 344
Abstract
In this study, we investigate the properties of a thin accretion disk around a static spherically symmetric black hole in 4D Einstein–Gauss–Bonnet gravity, with an additional coupling constant, α, appearing in the spacetime metric. Using the Novikov–Thorne accretion disk model, we examine [...] Read more.
In this study, we investigate the properties of a thin accretion disk around a static spherically symmetric black hole in 4D Einstein–Gauss–Bonnet gravity, with an additional coupling constant, α, appearing in the spacetime metric. Using the Novikov–Thorne accretion disk model, we examine the thermal properties of the disk, finding that increasing α reduces the energy, angular momentum, and effective potential of a test particle orbiting the black hole. We demonstrate that α can mimic the spin of a Kerr black hole in general relativity up to a≃ 0.23 M for the maximum value of α. Our analysis of the thermal radiation flux shows that larger α values increase the flux and shift its maximum towards the central black hole, while far from the black hole, the solution recovers the Schwarzschild limit. The impact of α on the radiative efficiency of the disk is weak but can slightly alter it. Assuming black-body radiation, we observe that the disk’s temperature peaks near its inner edge and is higher for larger α values. Lastly, the electromagnetic spectra reveal that the disk’s luminosity is lower in Einstein–Gauss–Bonnet gravity compared to general relativity, with the peak luminosity shifting toward higher frequencies, corresponding to the soft X-ray band as α increases. Full article
(This article belongs to the Special Issue Exploring Low-Frequency Gravitational Wave Sources: Waveforms, Detection and Sciences)
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22 pages, 3351 KiB  
Article
Distinguishing Compact Objects in Extreme-Mass-Ratio Inspirals by Gravitational Waves
by Lujia Xu, Shucheng Yang, Wenbiao Han, Xingyu Zhong, Rundong Tang and Yuanhao Zhang
Universe 2025, 11(1), 18; https://doi.org/10.3390/universe11010018 - 13 Jan 2025
Viewed by 472
Abstract
Extreme-mass-ratio inspirals (EMRIs) are promising gravitational-wave (GW) sources for space-based GW detectors. EMRI signals typically have long durations, ranging from several months to several years, necessitating highly accurate GW signal templates for detection. In most waveform models, compact objects in EMRIs are treated [...] Read more.
Extreme-mass-ratio inspirals (EMRIs) are promising gravitational-wave (GW) sources for space-based GW detectors. EMRI signals typically have long durations, ranging from several months to several years, necessitating highly accurate GW signal templates for detection. In most waveform models, compact objects in EMRIs are treated as test particles without accounting for their spin, mass quadrupole, or tidal deformation. In this study, we simulate GW signals from EMRIs by incorporating the spin and mass quadrupole moments of the compact objects. We evaluate the accuracy of parameter estimation for these simulated waveforms using the Fisher Information Matrix (FIM) and find that the spin, tidal-induced quadruple, and spin-induced quadruple can all be measured with precision ranging from 10−2 to 10−1, particularly for a mass ratio of ∼10−4. Assuming the “true” GW signals originate from an extended body inspiraling into a supermassive black hole, we compute the signal-to-noise ratio (SNR) and Bayes factors between a test-particle waveform template and our model, which includes the spin and quadrupole of the compact object. Our results show that the spin of compact objects can produce detectable deviations in the waveforms across all object types, while tidal-induced quadrupoles are only significant for white dwarfs, especially in cases approaching an intermediate-mass ratio. Spin-induced quadrupoles, however, have negligible effects on the waveforms. Therefore, our findings suggest that it is possible to distinguish primordial black holes from white dwarfs, and, under certain conditions, neutron stars can also be differentiated from primordial black holes. Full article
(This article belongs to the Special Issue Exploring Low-Frequency Gravitational Wave Sources: Waveforms, Detection and Sciences)
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15 pages, 4625 KiB  
Article
Frequency Shift of Electromagnetic Radiation Around Charged Hayward Black Hole
by Bakhodirkhon Saidov, Bakhtiyor Narzilloev, Ahmadjon Abdujabbarov, Malika Khudoyberdieva and Bobomurat Ahmedov
Universe 2024, 10(12), 454; https://doi.org/10.3390/universe10120454 (registering DOI) - 12 Dec 2024
Viewed by 611
Abstract
In this work, we investigate spacetime and photon dynamics around a charged Hayward black hole, focusing on the effects of electric charge Q and the length factor l. Our analysis shows that the maximum charge for black hole existence decreases as l [...] Read more.
In this work, we investigate spacetime and photon dynamics around a charged Hayward black hole, focusing on the effects of electric charge Q and the length factor l. Our analysis shows that the maximum charge for black hole existence decreases as l increases, vanishing at l/M≃0.77. The black hole has both inner and outer horizons, with the outer horizon shrinking and the inner horizon expanding as spacetime parameters increase. The spacetime curvature, measured by the Kretschmann scalar, is most pronounced when both parameters are small, resembling the Schwarzschild black hole. The electric charge strongly influences the curvature and photon sphere size, while the effect of the length factor is less significant. Additionally, the gravitational redshift of photons is more sensitive to the electric charge of the compact object than the length factor, diminishing as Q increases and with greater radial distance from the black hole. Overall, while both spacetime parameters affect black hole properties, the electric charge has a slightly stronger impact, especially on gravitational redshift and photon behavior. Full article
(This article belongs to the Special Issue Exploring Low-Frequency Gravitational Wave Sources: Waveforms, Detection and Sciences)
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