Riroriro: Simulating gravitational waves and evaluating their detectability in Python

Zeist, Wouter G.J. van; Stevance, H. F.; Eldridge, J. J.

doi:10.21105/joss.02968

Cited by 6 publications

(3 citation statements)

References 11 publications

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“…They do not account for general relativistic effects past the innermost stable circular orbit 𝑟 ISCO = 6𝐺 𝑀 𝑐 2 of the primary star. However, based on prior work with the code (van Zeist et al 2021), which accounts for up to third post-Newtonian terms, we expect that the merger time-scale will only be higher by fractions of years in this regime, and thus we do not consider effects stronger than this.…”

Section: T : Modelling Compact Remnant Binary Populations and Their M...mentioning

confidence: 99%

New constraints on the Bray conservation-of-momentum natal kick model from multiple distinct observations

Richards¹,

Eldridge²,

Briel³

et al. 2022

Preprint

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Natal supernova kicks, the linear momentum compact remnants receive during their formation, are an essential part of binary population synthesis (BPS) models. Although these kicks are well-supported by evidence, their underlying distributions and incorporation into BPS models is uncertain. In this work, we investigate the nature of natal kicks using a previously proposed analytical prescription where the strength of the kick is linearly proportional to the ejecta-remnant mass ratio. We vary the free parameters over large ranges of possible values, comparing these synthetic populations simultaneously against four constraints: the merger rate of compact binary neutron star (BNS) systems, the period-eccentricity distribution of galactic BNSs, the velocity distribution of single-star pulsars, and the likelihood for low-ejecta mass supernovae to produce low-velocity kicks. We find that different samples of the parameter space satisfy each tests, and only 1 per cent of the models satisfy all four constraints simultaneously. Although we cannot identify a single best kick model, we report 𝛼 = 80 ± 30 km s −1 , 𝛽 = 0 ± 20 km s −1 as the center of the region of the parameter space that fulfils all of our constraints, and expect 𝛽 ≥ 0 km s −1 as a further constraint. We also suggest further observations that will enable future refinement of the kick model. A sensitive test for the kick model will be the redshift evolution of the BNS merger rate since this is effectively a direct measure of the delay-time distribution for mergers. For our best fitting values, we find that the peak of the BNS merger rate is the present-day.

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Section: T : Modelling Compact Remnant Binary Populations and Their M...mentioning

confidence: 99%

New constraints on the Bray conservation-of-momentum natal kick model from multiple distinct observations

Richards¹,

Eldridge²,

Briel³

et al. 2022

Preprint

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“…Our results might therefore contribute to our understanding of PG 1553+113 as a binary SMBH candidate. No confirmation of a binary from GWs can be expected since the continuous GW signal from PG 1553 +113ʼs putative binary has a strain amplitude well below the detection threshold of foreseeable pulsar timing arrays (van Zeist et al 2021).…”

Section: Discussionmentioning

confidence: 98%

Constraining the PG 1553+113 Binary Hypothesis: Interpreting Hints of a New, 22 yr Period

Adhikari,

Peñil,

Westernacher-Schneider

et al. 2024

ApJ

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PG 1553+113 is a well-known blazar exhibiting evidence of a ∼2.2 yr quasiperiodic oscillation (QPO) in the radio, optical, X-ray, and γ-ray bands. Since QPO mechanisms often predict multiple QPOs, we search for a second QPO in its historical optical light curve covering a century of observations. Despite challenging data quality issues, we find hints of a 21.8 ± 4.7 yr oscillation. On its own, this ∼22 yr period has a modest statistical significance of 1.6σ when accounting for the look-elsewhere effect. However, the joint significance of both the 2.2 and 22 yr periods arising from colored noise alone is ∼3.6σ. The next peak of the 22 yr oscillation is predicted to occur around July 2025. We find that such a ∼10:1 relation between two periods can arise in the gas dynamics of a plausible supermassive black hole binary model of PG 1553+113. While the 22 yr QPO is preliminary, an interpretation of PG 1553+113's two QPOs in this binary model suggests that the binary engine has a mass ratio ≳0.2, an eccentricity ≲0.1, and accretes from a disk with characteristic aspect ratio ∼0.03. The putative binary radiates nHz gravitational waves, but the amplitude is ∼10–100 times too low for detection by foreseeable pulsar timing arrays.

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“…When simulating the gravitational waveforms from mergers of black holes or neutron stars that would be detectable by LIGO, particular methods of simplification that are commonly used include post-Newtonian approximations and limited numerical relativity. Such methods are used, for example, in LIGO's code suite LALS (LIGO Scientific Collaboration 2018), our own GW simulation package R (van Zeist et al 2021;Ghodla et al 2022) and the LISA-targeted package (Wagg et al 2022a,b). However, binaries in the frequency range of LISA have significantly wider orbits than those detectable by LIGO, so a simpler waveform model can be used, as the periods of these binaries effectively do not evolve over the time of observation.…”

Section: Simulating Gravitational Wavesmentioning

confidence: 99%

Gravitational wave spectral synthesis

Zeist¹,

Eldridge²,

Tang³

2023

Preprint

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We study the LISA sources that arise from isolated binary evolution, and how these depend on age and metallicity, using model stellar populations from . We calculate the combined GW spectrum of all the binaries within these population, including all types of compact binaries as well as those with living stars, and use these results to investigate the detectability of star clusters with LISA. We find at late times the dominant sources are WD-WD binaries, but at times before approx. 10 9 years we find a significant population of NS-WD and BH-WD binaries, which is related to the treatment of mass transfer and common envelope events in , wherein mass transfer is relatively likely to be stable. Metallicity also has an effect on the GW spectrum and on the relative dominance of different types of binaries. Our results suggest that nearby star clusters might produce GWs detectable by LISA or future missions throughout most of their evolution.

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Riroriro: Simulating gravitational waves and evaluating their detectability in Python

Cited by 6 publications

References 11 publications

New constraints on the Bray conservation-of-momentum natal kick model from multiple distinct observations

New constraints on the Bray conservation-of-momentum natal kick model from multiple distinct observations

Constraining the PG 1553+113 Binary Hypothesis: Interpreting Hints of a New, 22 yr Period

Gravitational wave spectral synthesis

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