Journal articles: 'Coalescence de binaire compacte'

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Spera, Mario, Alessandro Alberto Trani, and Mattia Mencagli. "Compact Binary Coalescences: Astrophysical Processes and Lessons Learned." Galaxies 10, no. 4 (June 25, 2022): 76. http://dx.doi.org/10.3390/galaxies10040076.

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On 11 February 2016, the LIGO and Virgo scientific collaborations announced the first direct detection of gravitational waves, a signal caught by the LIGO interferometers on 14 September 2015, and produced by the coalescence of two stellar-mass black holes. The discovery represented the beginning of an entirely new way to investigate the Universe. The latest gravitational-wave catalog by LIGO, Virgo and KAGRA brings the total number of gravitational-wave events to 90, and the count is expected to significantly increase in the next years, when additional ground-based and space-born interferometers will be operational. From the theoretical point of view, we have only fuzzy ideas about where the detected events came from, and the answers to most of the five Ws and How for the astrophysics of compact binary coalescences are still unknown. In this work, we review our current knowledge and uncertainties on the astrophysical processes behind merging compact-object binaries. Furthermore, we discuss the astrophysical lessons learned through the latest gravitational-wave detections, paying specific attention to the theoretical challenges coming from exceptional events (e.g., GW190521 and GW190814).

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Graziani, Luca. "Hunting for Dwarf Galaxies Hosting the Formation and Coalescence of Compact Binaries." Physics 1, no. 3 (December 6, 2019): 412–29. http://dx.doi.org/10.3390/physics1030030.

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Here we introduce the latest version of the GAMESH model, capable to consistently account for the formation and evolution of compact binary systems along the cosmic assembly of a Milky Way (MW)-like galaxy, centered on a local group volume resolving a large population of dwarf satellites. After describing the galaxy assembly process and how the formation of binary systems is accounted for, we summarize some recent findings on the properties and evolution of low-metallicity dwarf galaxies hosting the birth/coalescence of stellar/compact binaries generating GW150914-like signals. Finally, we focus on the mass and orbital properties of the above compact binary candidates assessing their impact on the resulting coalescence times and on selecting suitable galaxy hosts.

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Kalogera, V. "Close Binaries with Two Compact Objects." International Astronomical Union Colloquium 177 (2000): 579–84. http://dx.doi.org/10.1017/s0252921100060668.

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AbstractThe coalescence of close binary systems with two compact objects (neutron stars and black holes) are considered to be promising sources of gravitational waves for the currently built laser interferometers. Here, I review the current Galactic coalescence estimates derived both theoretically and empirically. I discuss the uncertainties involved as well as ways of obtaining an upper limit to the coalescence rate of two neutron stars.

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Abac, A. G., R. Abbott, I. Abouelfettouh, F. Acernese, K. Ackley, S. Adhicary, N. Adhikari, et al. "Observation of Gravitational Waves from the Coalescence of a 2.5–4.5 M _⊙ Compact Object and a Neutron Star." Astrophysical Journal Letters 970, no. 2 (July 26, 2024): L34. http://dx.doi.org/10.3847/2041-8213/ad5beb.

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Abstract We report the observation of a coalescing compact binary with component masses 2.5–4.5 M ⊙ and 1.2–2.0 M ⊙ (all measurements quoted at the 90% credible level). The gravitational-wave signal GW230529_181500 was observed during the fourth observing run of the LIGO–Virgo–KAGRA detector network on 2023 May 29 by the LIGO Livingston observatory. The primary component of the source has a mass less than 5 M ⊙ at 99% credibility. We cannot definitively determine from gravitational-wave data alone whether either component of the source is a neutron star or a black hole. However, given existing estimates of the maximum neutron star mass, we find the most probable interpretation of the source to be the coalescence of a neutron star with a black hole that has a mass between the most massive neutron stars and the least massive black holes observed in the Galaxy. We provisionally estimate a merger rate density of 55 − 47 + 127 Gpc − 3 yr − 1 for compact binary coalescences with properties similar to the source of GW230529_181500; assuming that the source is a neutron star–black hole merger, GW230529_181500-like sources may make up the majority of neutron star–black hole coalescences. The discovery of this system implies an increase in the expected rate of neutron star–black hole mergers with electromagnetic counterparts and provides further evidence for compact objects existing within the purported lower mass gap.

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Rasio, Frederic A., and Stuart L. Shapiro. "Hydrodynamic Evolution of Coalescing Compact Binaries." Symposium - International Astronomical Union 165 (1996): 17–28. http://dx.doi.org/10.1017/s0074180900055522.

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In addition to their possible relevance to gamma-ray bursts, coalescing binary neutron stars have long been recognized as important sources of gravitational radiation that should become detectable with the new generation of laser interferometers such as LIGO. Hydrodynamics plays an essential role near the end of the coalescence when the two stars finally merge into a single object. The shape of the corresponding burst of gravitational waves provides a direct probe into the interior structure of a neutron star and the nuclear equation of state. The interpretation of the gravitational waveform data will require detailed theoretical models of the complicated three-dimensional hydrodynamic processes involved. Here we review the results of our recent work on this problem, using both approximate quasi-analytic methods and large-scale numerical hydrodynamics calculations on supercomputers. We also discuss briefly the coalescence of white-dwarf binaries, which are also associated with a variety of interesting astrophysical phenomena.

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WEN, LINQING, and QI CHU. "EARLY DETECTION AND LOCALIZATION OF GRAVITATIONAL WAVES FROM COMPACT BINARY COALESCENCES." International Journal of Modern Physics D 22, no. 11 (September 2013): 1360011. http://dx.doi.org/10.1142/s0218271813600110.

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With the first detection of gravitational waves expected in the next decade, increasing efforts are made toward the electromagnetic follow-up observations of gravitational wave events. In this paper, I discuss the prospect of real-time detection and source localization for gravitational waves from neutron star–neutron star binary or neutron star–black hole binary coalescences before their merger. I show that several low-latency search pipelines are already under intensive development with the aim to provide real-time detections of these events. There will also be fast responding and/or wide-field electromagnetic telescopes available to help catch the electromagnetic or particle flashes possibly occurring during or immediately after their merger. It has been shown that a few coalescence events per year can be detected by advanced LIGO-VIRGO detector network tens of seconds before their merger. However, most of these events will have poor sky direction localization for the existing gravitational-wave detector network, making it extremely challenging for follow up observations by astronomical telescopes aiming at catching events around the merger time. A larger detector network including the planned detectors in Japan and in India will play an important role in improving the angular resolution and making prompt follow up observations much more realistic. A new detector at the Southern Hemisphere AIGO will further contribute significantly to this aspect.

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Shapiro, Stuart L. "Gravitomagnetic Induction during the Coalescence of Compact Binaries." Physical Review Letters 77, no. 22 (November 25, 1996): 4487–90. http://dx.doi.org/10.1103/physrevlett.77.4487.

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Chen, Bing-Guang, Tong Liu, Yan-Qing Qi, Bao-Quan Huang, Yun-Feng Wei, Tuan Yi, Wei-Min Gu, and Li Xue. "Effects of Vertical Advection on Multimessenger Signatures of Black Hole Neutrino-dominated Accretion Flows in Compact Binary Coalescences." Astrophysical Journal 941, no. 2 (December 1, 2022): 156. http://dx.doi.org/10.3847/1538-4357/aca406.

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Abstract In the coalescence events of binary neutron star (NS) or a black hole (BH) and an NS, a BH hyperaccretion disk might be eventually formed. At very high mass accretion rates, MeV neutrinos will be emitted from this disk, which is called a neutrino-dominated accretion flow (NDAF). Neutrino annihilation in the space out of the disk is energetic enough to launch ultrarelativistic jets to power gamma-ray bursts. Moreover, vertical advection might exist in NDAFs, which can generate the magnetic buoyancy bubbles to release gamma-ray photons. In this paper, we visit the effects of the vertical advection in NDAFs on the disk structure and gamma-ray and neutrino luminosities for different accretion rates. Then we study the anisotropic emission of kilonovae and the following gravitational waves (GWs) driven by the gamma-ray photons and neutrinos from NDAFs. Comparing NDAFs without vertical advection, the neutrino luminosity and GW strains slightly decrease for the case with vertical advection, and the kilonovae will be brightened by the injected gamma-ray photons. The future joint multimessenger observations might distinguish whether the vertical advection exists in NDAFs or not after compact binary coalescences.

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Yu, Shenghua, Youjun Lu, and C. Simon Jeffery. "Orbital evolution of neutron-star–white-dwarf binaries by Roche lobe overflow and gravitational wave radiation." Monthly Notices of the Royal Astronomical Society 503, no. 2 (March 5, 2021): 2776–90. http://dx.doi.org/10.1093/mnras/stab626.

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ABSTRACT We investigate the effects of mass transfer and gravitational wave (GW) radiation on the orbital evolution of contact neutron-star–white-dwarf (NS–WD) binaries, and the detectability of these binaries by space GW detectors (e.g. Laser Interferometer Space Antenna, LISA; Taiji; Tianqin). A NS–WD binary becomes contact when the WD component fills its Roche lobe, at which the GW frequency ranges from ∼0.0023 to 0.72 Hz for WD with masses ∼0.05–1.4 M⊙. We find that some high-mass NS–WD binaries may undergo direct coalescence after unstable mass transfer. However, the majority of NS–WD binaries can avoid direct coalescence because mass transfer after contact can lead to a reversal of the orbital evolution. Our model can well interpret the orbital evolution of the ultra-compact X-ray source 4U 1820–30. For a 4-yr observation of 4U 1820–30, the expected signal-to-noise-ratio (SNR) in GW characteristic strain is ∼11.0/10.4/2.2 (LISA/Taiji/Tianqin). The evolution of GW frequencies of NS–WD binaries depends on the WD masses. NS–WD binaries with masses larger than 4U 1820–30 are expected to be detected with significantly larger SNRs. For a $(1.4+0.5) \, {\rm M}_{\odot }$ NS–WD binary close to contact, the expected SNR for a one week observation is ∼27/40/28 (LISA/Taiji/Tianqin). For NS–WD binaries with masses of $(1.4+\gtrsim 1.1) \, {\rm M}_{\odot }$, the significant change of GW frequencies and amplitudes can be measured, and thus it is possible to determine the binary evolution stage. At distances up to the edge of the Galaxy (∼100 kpc), high-mass NS–WD binaries will be still detectable with SNR ≳ 1.

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MacLeod, Morgan, Kishalay De, and Abraham Loeb. "Dusty, Self-obscured Transients from Stellar Coalescence." Astrophysical Journal 937, no. 2 (October 1, 2022): 96. http://dx.doi.org/10.3847/1538-4357/ac8c31.

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Abstract We discuss the central role that dust condensation plays in shaping the observational appearance of outflows from coalescing binary systems. As binaries begin to coalesce, they shock-heat and expel material into their surroundings. Depending on the properties of the merging system, this material can expand to the point where molecules and dust form, dramatically increasing the gas opacity. We use the existing population of luminous red novae to constrain the thermodynamics of these ejecta, then apply our findings to the progressive obscuration of merging systems in the lead up to their coalescence. Compact progenitor stars near the main sequence or in the Hertzsprung gap along with massive progenitor stars have sufficiently hot circumstellar material to remain unobscured by dust. By contrast, more extended, low-mass giants should become completely optically obscured by dust formation in the circumbinary environment. We predict that 30%–50% of stellar-coalescence transients for solar-mass stars will be dusty, infrared-luminous sources. Of these, the optical transients may selectively trace complete merger outcomes while the infrared transients trace common envelope ejection outcomes.

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Spurzem, R., P. Berczik, I. Berentzen, D. Merritt, M. Preto, and P. Amaro-Seoane. "Formation and Evolution of Black Holes in Galactic Nuclei and Star Clusters." Proceedings of the International Astronomical Union 3, S246 (September 2007): 346–50. http://dx.doi.org/10.1017/s1743921308015901.

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AbstractWe study the formation, growth, and co-evolution of single and multiple supermassive black holes (SMBHs) and compact objects like neutron stars, white dwarfs, and stellar mass black holes in galactic nuclei and star clusters, focusing on the role of stellar dynamics. In this paper we focus on one exemplary topic out of a wider range of work done, the study of orbital parameters of binary black holes in galactic nuclei (binding energy, eccentricity, relativistic coalescence) as a function of initial parameters. In some cases the classical evolution of black hole binaries in dense stellar systems drives them to surprisingly high eccentricities, which is very exciting for the emission of gravitational waves and relativistic orbit shrinkage. Such results are interesting to the emerging field of gravitational wave astronomy, in relation to a number of ground and space based instruments designed to measure gravitational waves from astrophysical sources (VIRGO, Geo600, LIGO, LISA). Our models self-consistently cover the entire range from Newtonian dynamics to the relativistic coalescence of SMBH binaries.

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Chatterjee, Chayan, Manoj Kovalam, Linqing Wen, Damon Beveridge, Foivos Diakogiannis, and Kevin Vinsen. "Rapid Localization of Gravitational Wave Sources from Compact Binary Coalescences Using Deep Learning." Astrophysical Journal 959, no. 1 (December 1, 2023): 42. http://dx.doi.org/10.3847/1538-4357/ad08b7.

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Abstract The mergers of neutron star–neutron star and neutron star–black hole binaries (NSBHs) are the most promising gravitational wave (GW) events with electromagnetic (EM) counterparts. The rapid detection, localization, and simultaneous multimessenger follow-up of these sources are of primary importance in the upcoming science runs of the LIGO-Virgo-KAGRA Collaboration. While prompt EM counterparts during binary mergers can last less than 2 s, the timescales of existing localization methods that use Bayesian techniques, vary from seconds to days. In this paper, we propose the first deep learning–based approach for rapid and accurate sky localization of all types of binary coalescences, including neutron star–neutron star and NSBHs for the first time. Specifically, we train and test a normalizing flow model on matched-filtering output from GW searches to obtain sky direction posteriors in around 1 s using a single P100 GPU, which is several orders of magnitude faster than full Bayesian techniques.

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Romero-Shaw, I. M., C. Talbot, S. Biscoveanu, V. D’Emilio, G. Ashton, C. P. L. Berry, S. Coughlin, et al. "Bayesian inference for compact binary coalescences with bilby: validation and application to the first LIGO–Virgo gravitational-wave transient catalogue." Monthly Notices of the Royal Astronomical Society 499, no. 3 (September 21, 2020): 3295–319. http://dx.doi.org/10.1093/mnras/staa2850.

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ABSTRACT Gravitational waves provide a unique tool for observational astronomy. While the first LIGO–Virgo catalogue of gravitational-wave transients (GWTC-1) contains 11 signals from black hole and neutron star binaries, the number of observations is increasing rapidly as detector sensitivity improves. To extract information from the observed signals, it is imperative to have fast, flexible, and scalable inference techniques. In a previous paper, we introduced bilby: a modular and user-friendly Bayesian inference library adapted to address the needs of gravitational-wave inference. In this work, we demonstrate that bilby produces reliable results for simulated gravitational-wave signals from compact binary mergers, and verify that it accurately reproduces results reported for the 11 GWTC-1 signals. Additionally, we provide configuration and output files for all analyses to allow for easy reproduction, modification, and future use. This work establishes that bilby is primed and ready to analyse the rapidly growing population of compact binary coalescence gravitational-wave signals.

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Piccinni, Ornella Juliana. "Status and Perspectives of Continuous Gravitational Wave Searches." Galaxies 10, no. 3 (May 25, 2022): 72. http://dx.doi.org/10.3390/galaxies10030072.

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The birth of gravitational wave astronomy was triggered by the first detection of a signal produced by the merger of two compact objects (also known as a compact binary coalescence event). The following detections made by the Earth-based network of advanced interferometers had a significant impact in many fields of science: astrophysics, cosmology, nuclear physics and fundamental physics. However, compact binary coalescence signals are not the only type of gravitational waves potentially detectable by LIGO, Virgo, and KAGRA. An interesting family of still undetected signals, and the ones that are considered in this review, are the so-called continuous waves, paradigmatically exemplified by the gravitational radiation emitted by galactic, fast-spinning isolated neutron stars with a certain degree of asymmetry in their mass distribution. In this work, I will review the status and the latest results from the analyses of advanced detector data.

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Komossa, S., and J. A. Zensus. "Compact object mergers: observations of supermassive binary black holes and stellar tidal disruption events." Proceedings of the International Astronomical Union 10, S312 (August 2014): 13–25. http://dx.doi.org/10.1017/s1743921315007395.

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AbstractThe capture and disruption of stars by supermassive black holes (SMBHs), and the formation and coalescence of binaries, are inevitable consequences of the presence of SMBHs at the cores of galaxies. Pairs of active galactic nuclei (AGN) and binary SMBHs are important stages in the evolution of galaxy mergers, and an intense search for these systems is currently ongoing. In the early and advanced stages of galaxy merging, observations of the triggering of accretion onto one or both BHs inform us about feedback processes and BH growth. Identification of the compact binary SMBHs at parsec and sub-parsec scales provides us with important constraints on the interaction processes that govern the shrinkage of the binary beyond the “final parsec”. Coalescing binary SMBHs are among the most powerful sources of gravitational waves (GWs) in the universe. Stellar tidal disruption events (TDEs) appear as luminous, transient, accretion flares when part of the stellar material is accreted by the SMBH. About 30 events have been identified by multi-wavelength observations by now, and they will be detected in the thousands in future ground-based or space-based transient surveys. The study of TDEs provides us with a variety of new astrophysical tools and applications, related to fundamental physics or astrophysics. Here, we provide a review of the current status of observations of SMBH pairs and binaries, and TDEs, and discuss astrophysical implications.

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Talbot, Colm, and Eric Thrane. "Flexible and Accurate Evaluation of Gravitational-wave Malmquist Bias with Machine Learning." Astrophysical Journal 927, no. 1 (March 1, 2022): 76. http://dx.doi.org/10.3847/1538-4357/ac4bc0.

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Abstract Many astronomical surveys are limited by the brightness of the sources, and gravitational-wave searches are no exception. The detectability of gravitational waves from merging binaries is affected by the mass and spin of the constituent compact objects. To perform unbiased inference on the distribution of compact binaries, it is necessary to account for this selection effect, which is known as Malmquist bias. Since systematic error from selection effects grows with the number of events, it will be increasingly important over the coming years to accurately estimate the observational selection function for gravitational-wave astronomy. We employ density estimation methods to accurately and efficiently compute the compact binary coalescence selection function. We introduce a simple pre-processing method, which significantly reduces the complexity of the required machine-learning models. We demonstrate that our method has smaller statistical errors at comparable computational cost than the method currently most widely used allowing us to probe narrower distributions of spin magnitudes. The currently used method leaves 10%–50% of the interesting black hole spin models inaccessible; our new method can probe >99% of the models and has a lower uncertainty for >80% of the models.

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Ray, Anarya, Ignacio Magaña Hernandez, Siddharth Mohite, Jolien Creighton, and Shasvath Kapadia. "Nonparametric Inference of the Population of Compact Binaries from Gravitational-wave Observations Using Binned Gaussian Processes." Astrophysical Journal 957, no. 1 (October 25, 2023): 37. http://dx.doi.org/10.3847/1538-4357/acf452.

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Abstract The observation of gravitational waves from multiple compact binary coalescences by the LIGO–Virgo–KAGRA detector networks has enabled us to infer the underlying distribution of compact binaries across a wide range of masses, spins, and redshifts. In light of the new features found in the mass spectrum of binary black holes and the uncertainty regarding binary formation models, nonparametric population inference has become increasingly popular. In this work, we develop a data-driven clustering framework that can identify features in the component mass distribution of compact binaries simultaneously with those in the corresponding redshift distribution, from gravitational-wave data in the presence of significant measurement uncertainties, while making very few assumptions about the functional form of these distributions. Our generalized model is capable of inferring correlations among various population properties, such as the redshift evolution of the shape of the mass distribution itself, in contrast to most existing nonparametric inference schemes. We test our model on simulated data and demonstrate the accuracy with which it can reconstruct the underlying distributions of component masses and redshifts. We also reanalyze public LIGO–Virgo–KAGRA data from events in GWTC-3 using our model and compare our results with those from some alternative parametric and nonparametric population inference approaches. Finally, we investigate the potential presence of correlations between mass and redshift in the population of binary black holes in GWTC-3 (those observed by the LIGO–Virgo–KAGRA detector network in their first three observing runs), without making any assumptions about the specific nature of these correlations.

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Tsutsui, T., A. Nishizawa, and S. Morisaki. "Early warning of precessing neutron-star black hole binary mergers with the near-future gravitational-wave detectors." Monthly Notices of the Royal Astronomical Society 512, no. 3 (March 17, 2022): 3878–84. http://dx.doi.org/10.1093/mnras/stac715.

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ABSTRACT Since gravitational and electromagnetic waves from a compact binary coalescence carry independent information about the source, the joint observation is important for understanding the physical mechanisms of the emissions. Rapid detection and source localization of a gravitational wave signal are crucial for the joint observation to be successful. For a signal with a high signal-to-noise ratio, it is even possible to detect it before the merger, which is called early warning. In this article, we estimate the performances of the early warning for neutron-star black hole binaries, considering the precession effect of a binary orbit, with the near-future detectors such as A+, AdV+, KAGRA+ , and Voyager. We find that a gravitational wave source can be localized in $100 \, \rm {deg^2}$ on the sky before ∼10–$40 \, \rm {s}$ of time to merger once per year.

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O'Shaughnessy, R., V. Kalogera, and Krzysztof Belczynski. "BINARY COMPACT OBJECT COALESCENCE RATES: THE ROLE OF ELLIPTICAL GALAXIES." Astrophysical Journal 716, no. 1 (May 20, 2010): 615–33. http://dx.doi.org/10.1088/0004-637x/716/1/615.

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Usman, Samantha A., Alexander H. Nitz, Ian W. Harry, Christopher M. Biwer, Duncan A. Brown, Miriam Cabero, Collin D. Capano, et al. "The PyCBC search for gravitational waves from compact binary coalescence." Classical and Quantum Gravity 33, no. 21 (October 10, 2016): 215004. http://dx.doi.org/10.1088/0264-9381/33/21/215004.

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Ni, Wei-Tou, Gang Wang, and An-Ming Wu. "Astrodynamical middle-frequency interferometric gravitational wave observatory AMIGO: Mission concept and orbit design." International Journal of Modern Physics D 29, no. 04 (March 2020): 1940007. http://dx.doi.org/10.1142/s0218271819400078.

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AMIGO is a first-generation Astrodynamical Middle-frequency Interferometric Gravitational Wave (GW) Observatory. The scientific goals of AMIGO are to bridge the spectra gap between first-generation high-frequency and low-frequency GW sensitivities: to detect intermediate mass BH coalescence; to detect inspiral phase and predict time of binary black hole coalescences together with binary neutron star & black hole-neutron star coalescences for ground interferometers; to detect compact binary inspirals for studying stellar evolution and galactic population. The mission concept is to use time delay interferometry (TDI) for a nearly triangular formation of three drag-free spacecraft with nominal arm length 10,000 km, emitting laser power 2–10 W and telescope diameter 300–500 mm. The design GW sensitivity in the middle frequency band is [Formula: see text] Hz[Formula: see text]. Both geocentric and heliocentric orbit formations are considered. All options have LISA-like formations, that is, the triangular formation is [Formula: see text] inclined to the orbit plane. For all solar orbit options of AMIGO, the first-generation TDI satisfies the laser frequency-noise suppression requirement. We also investigate for each option of orbits under study, whether constant equal-arm implementation is feasible. For the solar-orbit options, the acceleration to maintain the formation can be designed to be less than 15 nm/s2 with the thruster requirement in the 15 [Formula: see text]N range. AMIGO would be a good place to test the feasibility of the constant equal-arm option. Fuel requirement, thruster noise requirement and test mass acceleration actuation requirement are briefly considered. From the orbit study, the solar orbit option is the mission orbit preference. We study the deployment for this orbit option. After a last-stage launch from 300 km Low Earth Orbit (LEO), each S/C’s maneuver to an appropriate 2-degree-behind-the-Earth AMIGO formation in 95 days requires only a [Formula: see text]v of about 80 m/s.

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Mozzon, S., L. K. Nuttall, A. Lundgren, T. Dent, S. Kumar, and A. H. Nitz. "Dynamic normalization for compact binary coalescence searches in non-stationary noise." Classical and Quantum Gravity 37, no. 21 (October 20, 2020): 215014. http://dx.doi.org/10.1088/1361-6382/abac6c.

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Cannon, Kipp, Romain Cariou, Adrian Chapman, Mireia Crispin-Ortuzar, Nickolas Fotopoulos, Melissa Frei, Chad Hanna, et al. "TOWARD EARLY-WARNING DETECTION OF GRAVITATIONAL WAVES FROM COMPACT BINARY COALESCENCE." Astrophysical Journal 748, no. 2 (March 15, 2012): 136. http://dx.doi.org/10.1088/0004-637x/748/2/136.

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Mencagli, Mattia, Natalia Nazarova, and Mario Spera. "ISTEDDAS: a new direct N-Body code to study merging compact-object binaries." Journal of Physics: Conference Series 2207, no. 1 (March 1, 2022): 012051. http://dx.doi.org/10.1088/1742-6596/2207/1/012051.

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Abstract On September 14, 2015, the two detectors of the Laser Interferometer Gravitational wave Observatory (LIGO) reported the first detection of gravitational waves, a signal generated from the coalescence of two stellar-mass black holes. The discovery represented the beginning of an entirely new way to investigate the Universe. From the theoretical point of view, the formation and evolution of compact-object binaries are still very uncertain. One of the main issues is that most stars form in dense stellar environments, and numerical simulations of merging compact-object binaries in such crowded stellar systems are very challenging. In this work, we review the main numerical bottlenecks that hamper our knowledge on merging binaries in dense environments and we present a new GPU-accelerated N-body code, which is currently under development, called isteddas, that can overcome most of the obstacles.

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Rastello, Sara, Michela Mapelli, Ugo N. Di Carlo, Nicola Giacobbo, Filippo Santoliquido, Mario Spera, Alessandro Ballone, and Giuliano Iorio. "Dynamics of black hole–neutron star binaries in young star clusters." Monthly Notices of the Royal Astronomical Society 497, no. 2 (July 10, 2020): 1563–70. http://dx.doi.org/10.1093/mnras/staa2018.

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ABSTRACT Young star clusters are likely the most common birthplace of massive stars across cosmic time and influence the formation of compact binaries in several ways. Here, we simulate the formation of black hole–neutron star binaries (BHNSs) in young star clusters, by means of the binary population synthesis code MOBSE interfaced with the N-body code NBODY6++GPU. BHNSs formed in young star clusters (dynamical BHNSs) are significantly more massive than BHNSs formed from isolated binaries (isolated BHNSs): ∼40 per cent of the dynamical BHNS mergers have a total mass of >15 M⊙, while only ∼0.01 per cent of the isolated BHNS mergers have mass in excess of this value. Hence, our models strongly support a dynamical formation scenario for GW190814, given its total mass of ∼26 M⊙, if this event is a BHNS merger. All our dynamical BHNSs are ejected from their parent star cluster before they reach coalescence. Thus, a significant fraction of BHNS mergers occurring in the field might have originated in a young star cluster. The mass spectrum of BHNS mergers from gravitational-wave detections will provide a clue to differentiate between dynamical and isolated formation of BHNSs.

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Hamilton, Chris, and Roman R. Rafikov. "Relativistic Phase Space Diffusion of Compact Object Binaries in Stellar Clusters and Hierarchical Triples." Astrophysical Journal 961, no. 2 (January 30, 2024): 237. http://dx.doi.org/10.3847/1538-4357/ad0be2.

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Abstract The LIGO/Virgo detections of compact object mergers have posed a challenge for theories of binary evolution and coalescence. One promising avenue for producing mergers dynamically is through secular eccentricity oscillations driven by an external perturber, be it a tertiary companion (as in the Lidov–Kozai, LK, mechanism) or the tidal field of the stellar cluster in which the binary orbits. The simplest theoretical models of these oscillations use a “doubly averaged” (DA) approximation, averaging both over the binary’s internal Keplerian orbit and its “outer” barycentric orbit relative to the perturber. However, DA theories do not account for fluctuations of the perturbing torque on the outer orbital timescale, which are known to increase a binary’s eccentricity beyond the maximum DA value, potentially accelerating mergers. Here we reconsider the impact of these short-timescale fluctuations in the test-particle quadrupolar limit for binaries perturbed by arbitrary spherical cluster potentials (including LK as a special case), in particular including 1pN general relativistic (GR) apsidal precession of the internal orbit. Focusing on the behavior of the binary orbital elements around peak eccentricity, we discover a new effect, relativistic phase space diffusion (RPSD), in which a binary can jump to a completely new dynamical trajectory on an outer orbital timescale, violating the approximate conservation of DA integrals of motion. RPSD arises from an interplay between secular behavior at extremely high eccentricity, short-timescale fluctuations, and rapid GR precession, and can change the subsequent secular evolution dramatically. This effect occurs even in hierarchical triples, but has not been uncovered until now.

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Abbott, B. P., R. Abbott, T. D. Abbott, S. Abraham, F. Acernese, K. Ackley, C. Adams, et al. "GW190425: Observation of a Compact Binary Coalescence with Total Mass ∼ 3.4 M ⊙." Astrophysical Journal 892, no. 1 (March 19, 2020): L3. http://dx.doi.org/10.3847/2041-8213/ab75f5.

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Kopparapu, Ravi Kumar, Chad Hanna, Vicky Kalogera, Richard O’Shaughnessy, Gabriela González, Patrick R. Brady, and Stephen Fairhurst. "Host Galaxies Catalog Used in LIGO Searches for Compact Binary Coalescence Events." Astrophysical Journal 675, no. 2 (March 10, 2008): 1459–67. http://dx.doi.org/10.1086/527348.

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Nielsen, Alex B. "Compact binary coalescence parameter estimations for 2.5 post-Newtonian aligned spinning waveforms." Classical and Quantum Gravity 30, no. 7 (March 15, 2013): 075023. http://dx.doi.org/10.1088/0264-9381/30/7/075023.

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Dobie, Dougal, Tara Murphy, David L. Kaplan, Kenta Hotokezaka, Juan Pablo Bonilla Ataides, Elizabeth K. Mahony, and Elaine M. Sadler. "Radio afterglows from compact binary coalescences: prospects for next-generation telescopes." Monthly Notices of the Royal Astronomical Society 505, no. 2 (May 22, 2021): 2647–61. http://dx.doi.org/10.1093/mnras/stab1468.

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ABSTRACT The detection of gravitational waves from a neutron star merger, GW170817, marked the dawn of a new era in time-domain astronomy. Monitoring of the radio emission produced by the merger, including high-resolution radio imaging, enabled measurements of merger properties including the energetics and inclination angle. In this work, we compare the capabilities of current and future gravitational wave facilities to the sensitivity of radio facilities to quantify the prospects for detecting the radio afterglows of gravitational wave events. We consider three observing strategies to identify future mergers – wide field follow-up, targeting galaxies within the merger localization and deep monitoring of known counterparts. We find that while planned radio facilities like the Square Kilometre Array will be capable of detecting mergers at gigaparsec distances, no facilities are sufficiently sensitive to detect mergers at the range of proposed third-generation gravitational wave detectors that would operate starting in the 2030s.

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Mandel, Ilya, Christopher P. L. Berry, Frank Ohme, Stephen Fairhurst, and Will M. Farr. "Parameter estimation on compact binary coalescences with abruptly terminating gravitational waveforms." Classical and Quantum Gravity 31, no. 15 (July 14, 2014): 155005. http://dx.doi.org/10.1088/0264-9381/31/15/155005.

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Singh, Mukesh Kumar, Shasvath J. Kapadia, Md Arif Shaikh, Deep Chatterjee, and Parameswaran Ajith. "Improved early warning of compact binary mergers using higher modes of gravitational radiation: a population study." Monthly Notices of the Royal Astronomical Society 502, no. 2 (January 19, 2021): 1612–22. http://dx.doi.org/10.1093/mnras/stab125.

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ABSTRACT A gravitational wave early warning of a compact binary coalescence event, with a sufficiently tight localization skymap, would allow telescopes to point in the direction of the potential electromagnetic counterpart before its onset. Use of higher modes of gravitational radiation, in addition to the dominant mode typically used in templated real-time searches, was recently shown to produce significant improvements in early-warning times and skyarea localizations for a range of asymmetric mass binaries. We perform a large-scale study to assess the benefits of this method for a population of compact binary merger observations. In particular, we inject 100 000 such signals in Gaussian noise, with component masses $m_1 \in \left[1, 60 \right] \, \mathrm{M}_{\odot }$ and $m_2 \in \left[1, 3 \right] \, \mathrm{M}_{\odot }$. We consider three scenarios involving ground-based detectors: the fifth (O5) observing run of the Advanced LIGO-Virgo-KAGRA network, its projected Voyager upgrade, as well as a proposed third-generation (3G) network. We find that for fixed early-warning times of 20–60 s, the inclusion of the higher modes can provide localization improvements of a factor of ≳2 for up to ${\sim}60{{\ \rm per\ cent}}$ ($70 {{\ \rm per\ cent}}$) of the neutron star–black hole (NSBH) systems in the O5 (Voyager) scenario. Considering only those NSBH systems that can produce potential electromagnetic counterparts, such improvements in the localization can be expected for ${\sim}5\!-\!35{{\ \rm per\ cent}}$ $(20\!-\!50{{\ \rm per\ cent}})$ binaries in O5 (Voyager). For the 3G scenario, a significant fraction of the events have time gains of a minute to several minutes, assuming fiducial target localization areas of 100–1000 deg2.

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Stachie, Cosmin, Tito Dal Canton, Nelson Christensen, Marie-Anne Bizouard, Michael Briggs, Eric Burns, Jordan Camp, and Michael Coughlin. "Searches for Modulated γ-Ray Precursors to Compact Binary Mergers in Fermi-GBM Data." Astrophysical Journal 930, no. 1 (May 1, 2022): 45. http://dx.doi.org/10.3847/1538-4357/ac5f53.

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Abstract GW170817 is the only gravitational-wave event for which a confirmed γ-ray counterpart, GRB 170817A, has been detected. Here, we present a method to search for another type of γ-ray signal, a γ-ray burst precursor, associated with a compact binary merger. If emitted shortly before the coalescence, a high-energy electromagnetic (EM) flash travels through a highly dynamical and relativistic environment, created by the two compact objects orbiting each other. Thus, the EM signal arriving at an Earth observer could present a somewhat predictable time-dependent modulation. We describe a targeted search method for light curves exhibiting such a modulation, parameterized by the observer-frame component masses and binary merger time, using Fermi-GBM data. The sensitivity of the method is assessed based on simulated signals added to GBM data. The method is then applied to a selection of potentially interesting compact binary mergers detected during the second (O2) and third (O3) observing runs of Advanced LIGO and Advanced Virgo. We find no significant modulated γ-ray precursor signal associated with any of the considered events.

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Regimbau, Tania. "The Quest for the Astrophysical Gravitational-Wave Background with Terrestrial Detectors." Symmetry 14, no. 2 (January 29, 2022): 270. http://dx.doi.org/10.3390/sym14020270.

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We present the gravitational-wave background and its properties focusing on the background from compact binary coalescences in terrestrial detectors. We also introduce the standard data analysis method used to search for this background and discuss its detectability with second and third generation networks of detectors. To illustrate, we first use simple models and then discuss more realistic models based on simulations.

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Dupree, William, and Sukanta Bose. "Multi-detector null-stream-based $\chi^2$ statistic for compact binary coalescence searches." Classical and Quantum Gravity 36, no. 19 (September 11, 2019): 195012. http://dx.doi.org/10.1088/1361-6382/ab30cf.

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Van Den Broeck, C. "Astrophysics, cosmology, and fundamental physics with compact binary coalescence and the Einstein Telescope." Journal of Physics: Conference Series 484 (March 5, 2014): 012008. http://dx.doi.org/10.1088/1742-6596/484/1/012008.

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Biwer, C. M., Collin D. Capano, Soumi De, Miriam Cabero, Duncan A. Brown, Alexander H. Nitz, and V. Raymond. "PyCBC Inference: A Python-based Parameter Estimation Toolkit for Compact Binary Coalescence Signals." Publications of the Astronomical Society of the Pacific 131, no. 996 (January 11, 2019): 024503. http://dx.doi.org/10.1088/1538-3873/aaef0b.

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Mandel, Ilya, and Richard O'Shaughnessy. "Compact binary coalescences in the band of ground-based gravitational-wave detectors." Classical and Quantum Gravity 27, no. 11 (May 11, 2010): 114007. http://dx.doi.org/10.1088/0264-9381/27/11/114007.

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Nitz, Alexander H., Collin D. Capano, Sumit Kumar, Yi-Fan Wang, Shilpa Kastha, Marlin Schäfer, Rahul Dhurkunde, and Miriam Cabero. "3-OGC: Catalog of Gravitational Waves from Compact-binary Mergers." Astrophysical Journal 922, no. 1 (November 1, 2021): 76. http://dx.doi.org/10.3847/1538-4357/ac1c03.

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Abstract We present the third open gravitational-wave catalog (3-OGC) of compact-binary coalescences, based on the analysis of the public LIGO and Virgo data from 2015 through 2019 (O1, O2, O3a). Our updated catalog includes a population of 57 observations, including 4 binary black hole mergers that had not been previously reported. This consists of 55 binary black hole mergers and the 2 binary neutron star mergers, GW170817 and GW190425. We find no additional significant binary neutron star or neutron star–black hole merger events. The most confident new detection is the binary black hole merger GW190925_232845, which was observed by the LIGO–Hanford and Virgo observatories with  astro > 0.99 ; its primary and secondary component masses are 20.2 − 2.5 + 3.9 M ⊙ and 15.6 − 2.6 + 2.1 M ⊙ , respectively. We estimate the parameters of all binary black hole events using an up-to-date waveform model that includes both subdominant harmonics and precession effects. To enable deep follow up as our understanding of the underlying populations evolves, we make available our comprehensive catalog of events, including the subthreshold population of candidates, and the posterior samples of our source parameter estimates.

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Maurya, S. K., G. Mustafa, M. Govender, and Ksh Newton Singh. "Exploring physical properties of minimally deformed strange star model and constraints on maximum mass limit in f(𝒬) gravity." Journal of Cosmology and Astroparticle Physics 2022, no. 10 (October 1, 2022): 003. http://dx.doi.org/10.1088/1475-7516/2022/10/003.

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Abstract Our current investigation is inherently linked to the observations of gravitational waves from the GW190814 event which suggests that the source of the signals can be ascribed to a compact binary coalescence of a 22.2 to 24.3M ⊙ black hole and a compact object endowed with a mass of 2.50 to 2.67M ⊙. In the current exposition, we are concerned with modeling of the lower mass component of the coalescence pair. We utilize the f(𝒬) gravity together with the Minimal Geometric Deformation (MGD) technique to obtain compact stellar objects with masses aligned with the GW190814 event. Starting off with the Tolman IV ansatz for one of the metric functions, together with an MIT Bag model equation of state we are able to reduce the problem of fully describing the gravitational behavior of the seed solution to a quadrature. Through the MGD technique, we introduce anisotropy by deforming the radial part of the gravitational potential. This enables us to obtain two new classes of solutions which depend on the metricity parameter, 𝒬 and the deformation constant, β. We show that these two parameters play a crucial role in determining the thermodynamical behavior and stability of our models. In particular, we show that the interplay between the metricity parameter and the deformation constant predicts the mass of the progenitor articulating as the secondary component of GW190814.

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Nitz, Alexander H., and Yi-Fan Wang. "Search for Gravitational Waves from the Coalescence of Subsolar Mass and Eccentric Compact Binaries." Astrophysical Journal 915, no. 1 (July 1, 2021): 54. http://dx.doi.org/10.3847/1538-4357/ac01d9.

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Liu, Yuan, Zhihui Du, Shin Kee Chung, Shaun Hooper, David Blair, and Linqing Wen. "GPU-accelerated low-latency real-time searches for gravitational waves from compact binary coalescence." Classical and Quantum Gravity 29, no. 23 (November 2, 2012): 235018. http://dx.doi.org/10.1088/0264-9381/29/23/235018.

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Hu, Chin-Ping, Lupin Chun-Che Lin, Kuo-Chuan Pan, Kwan-Lok Li, Chien-Chang Yen, Albert K. H. Kong, and C. Y. Hui. "A Comprehensive Analysis of the Gravitational Wave Events with the Stacked Hilbert–Huang Transform: From Compact Binary Coalescence to Supernova." Astrophysical Journal 935, no. 2 (August 1, 2022): 127. http://dx.doi.org/10.3847/1538-4357/ac8165.

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Abstract We analyze the gravitational wave signals with a model-independent time-frequency analysis, which is improved from the Hilbert–Huang transform (HHT) and optimized for characterizing the frequency variability on the time-frequency map. Instead of the regular HHT algorithm, i.e., obtaining intrinsic mode functions with ensemble empirical mode decomposition and yielding the instantaneous frequencies, we propose an alternative algorithm that operates the ensemble mean on the time-frequency map. We systematically analyze the known gravitational wave events of the compact binary coalescence observed in the first gravitational-wave transient catalog, and in the simulated gravitational wave signals from core-collapse supernovae (CCSNe) with our method. The time-frequency maps of the binary black hole coalescence cases show much more detail compared to those wavelet spectra. Moreover, the oscillation in the instantaneous frequency caused by mode-mixing could be reduced with our algorithm. For the CCSNe data, the oscillation from the proto-neutron star and the radiation from the standing accretion shock instability can be precisely determined with the HHT in great detail. More importantly, the initial stage of different modes of oscillations can be clearly separated. These results provide new hints for further establishment of the detecting algorithm and new probes to investigate the underlying physical mechanisms.

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Vedovato, G., E. Milotti, G. A. Prodi, S. Bini, M. Drago, V. Gayathri, O. Halim, et al. "Minimally-modeled search of higher multipole gravitational-wave radiation in compact binary coalescences." Classical and Quantum Gravity 39, no. 4 (January 24, 2022): 045001. http://dx.doi.org/10.1088/1361-6382/ac45da.

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Abstract As the Advanced LIGO and Advanced Virgo interferometers, soon to be joined by the KAGRA interferometer, increase their sensitivity, they detect an ever-larger number of gravitational waves with a significant presence of higher multipoles (HMs) in addition to the dominant (2, 2) multipole. These HMs can be detected with different approaches, such as the minimally-modeled burst search methods, and here we discuss one such approach based on the coherent WaveBurst (cWB) pipeline. During the inspiral phase the HMs produce chirps whose instantaneous frequency is a multiple of the dominant (2, 2) multipole, and here we describe how cWB can be used to detect these spectral features. The search is performed within suitable regions of the time-frequency representation; their shape is determined by optimizing the receiver operating characteristics. This novel method has already been used in the GW190814 discovery paper (Abbott et al 2020 Astrophys. J. Lett. 896 L44) and is very fast and flexible. Here we describe in full detail the procedure used to detect the (3, 3) multipole in GW190814 as well as searches for other HMs during the inspiral phase, and apply it to another event that displays HMs, GW190412, replicating the results obtained with different methods. The procedure described here can be used for the fast analysis of HMs and to support the findings obtained with the model-based Bayesian parameter estimates.

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Dietz, A. "Estimation of compact binary coalescense rates from short gamma-ray burst redshift measurements." Astronomy & Astrophysics 529 (April 11, 2011): A97. http://dx.doi.org/10.1051/0004-6361/201016166.

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Kapadia, Shasvath J., Dimple, Dhruv Jain, Kuntal Misra, K. G. Arun, and Resmi Lekshmi. "Rates and Beaming Angles of Gamma-Ray Bursts Associated with Compact Binary Coalescences." Astrophysical Journal Letters 976, no. 1 (November 1, 2024): L10. http://dx.doi.org/10.3847/2041-8213/ad8dc7.

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Abstract Some, if not all, binary neutron star (BNS) coalescences, and a fraction of neutron star–black hole (NSBH) mergers, are thought to produce sufficient mass ejection to power gamma-ray bursts (GRBs). However, this fraction, as well as the distribution of beaming angles of BNS-associated GRBs, is poorly constrained from observation. Recent work applied machine learning tools to analyze GRB light curves observed by Fermi/Gamma-Ray Burst Monitor (GBM) and Swift/Burst Alert Telescope (BAT). GRBs were segregated into multiple distinct clusters, with the tantalizing possibility that one of them (BNS cluster) could be associated with BNSs and another (NSBH cluster) with NSBHs. As a proof of principle, assuming that all GRBs detected by Fermi/GBM and Swift/BAT associated with BNSs (NSBHs) lie in the BNS (NSBH) cluster, we estimate their rates (Gpc−3 yr−1). We compare these rates with corresponding BNS and NSBH rates estimated by the LIGO–Virgo–KAGRA (LVK) collaboration from the first three observing runs (O1, O2, O3). We find that the BNS rates are consistent with LVK’s rate estimates, assuming a uniform distribution of beaming fractions (f b ∈ [0.01, 0.1]). Conversely, using the LVK’s BNS rate estimates, assuming all BNS mergers produce GRBs, we are able to constrain the beaming angle distribution to θ j ∈ [0.°8, 33.°5] at 90% confidence. We similarly place limits on the fraction of GRB-bright NSBHs as f B ∈ [1.3%, 63%] (f B ∈ [0.4%, 15%]) with Fermi/GBM (Swift/BAT) data.

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Win, Aung Naing, Yu-Ming Chu, Hasrat Hussain Shah, Syed Zaheer Abbas, and Munawar Shah. "Electromagnetic counterpart to gravitational waves from coalescence of binary black hole with magnetic monopole charge." International Journal of Modern Physics A 35, no. 31 (November 10, 2020): 2050205. http://dx.doi.org/10.1142/s0217751x2050205x.

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A Satellite Fermi GBM detected recent putative short Gamma Ray Bursts (GRBs) in coincident with the gravitational wave signal GW 150914 produced by the merger of binary black hole (BH). If at least one BH possess magnetic monopole charge in the binary BH system then the short-duration GRBs may produce during the final phase of a binary BH merger. The detection of gravitational waves GW 150914, GW 151226 and LVT 151012 by LIGO gave the evidence that merging of the compact object like binary BH often happens in our universe. In this paper, we report the qualitative model to discuss the generation of electromagnetic radiation from the merging of two BHs with equal masses and at least one BH carrying the magnetic monopole charge in the binary system. In this model, BH possess a magnetic monopole charge that may not be neutralized before the coalescence. During the inspiralling process, the magnetic monopole charge on the BH would produced the electric dipole moment. Short duration GRB would produce by the rapidly evolution of the electric dipole moment which may detectable on Earth. We predict that this model would be beneficial in the future to explain the generation of gravitational wave (GW) plus a electromagnetic signal of multi-wavelength from mergers of magnetically charged BHs.

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Wei, Wei, E. A. Huerta, Mengshen Yun, Nicholas Loutrel, Md Arif Shaikh, Prayush Kumar, Roland Haas, and Volodymyr Kindratenko. "Deep Learning with Quantized Neural Networks for Gravitational-wave Forecasting of Eccentric Compact Binary Coalescence." Astrophysical Journal 919, no. 2 (September 28, 2021): 82. http://dx.doi.org/10.3847/1538-4357/ac1121.

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Zhang, Bing. "Charged Compact Binary Coalescence Signal and Electromagnetic Counterpart of Plunging Black Hole–Neutron Star Mergers." Astrophysical Journal 873, no. 2 (March 8, 2019): L9. http://dx.doi.org/10.3847/2041-8213/ab0ae8.

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Artale, M. Celeste, Yann Bouffanais, Michela Mapelli, Nicola Giacobbo, Nadeen B. Sabha, Filippo Santoliquido, Mario Pasquato, and Mario Spera. "An astrophysically motivated ranking criterion for low-latency electromagnetic follow-up of gravitational wave events." Monthly Notices of the Royal Astronomical Society 495, no. 2 (May 7, 2020): 1841–52. http://dx.doi.org/10.1093/mnras/staa1252.

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ABSTRACT We investigate the properties of the host galaxies of compact binary mergers across cosmic time. To this end, we combine population synthesis simulations together with galaxy catalogues from the hydrodynamical cosmological simulation eagle to derive the properties of the host galaxies of binary neutron star (BNS), black hole-neutron star (BHNS), and binary black hole (BBH) mergers. Within this framework, we derive the host galaxy probability, i.e. the probability that a galaxy hosts a compact binary coalescence as a function of its stellar mass, star formation rate, Ks magnitude, and B magnitude. This quantity is particularly important for low-latency searches of gravitational wave (GW) sources as it provides a way to rank galaxies lying inside the credible region in the sky of a given GW detection, hence reducing the number of viable host candidates. Furthermore, even if no electromagnetic counterpart is detected, the proposed ranking criterion can still be used to classify the galaxies contained in the error box. Our results show that massive galaxies (or equivalently galaxies with a high luminosity in Ks band) have a higher probability of hosting BNS, BHNS, and BBH mergers. We provide the probabilities in a suitable format to be implemented in future low-latency searches.

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Journal articles on the topic 'Coalescence de binaire compacte'

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