Forward modelling the O3(a+b) GW transient mass distributions with <scp>bpass</scp> by varying compact remnant mass and SNe kick prescriptions

Ghodla, Sohan; Zeist, Wouter G.J. van; Eldridge, J. J.; Stevance, H. F.; Stanway, Elizabeth R.

doi:10.1093/mnras/stac120

Cited by 17 publications

(16 citation statements)

References 54 publications

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“…with the most recent fiducial parameters 𝛼 = 100 +30 −20 km s −1 and 𝛽 = −170 +100 −100 km s −1 from Bray & Eldridge (2018), and 𝑀 NS the mass of a neutron star. We note that the Bray kick has an extra 𝑀 NS /𝑀 rem as a coefficient to 𝛽, as in Ghodla et al (2022). This factor was not present in the original kick proposed by Bray & Eldridge (2016), and has been introduced in work since then.…”

Section: Introductionmentioning

confidence: 93%

“…We note that the fiducial value of the Bray kick does not lie on the Eldridge et al (2018) contour. This is due to modifications we have made in the BPASS code around the calculation of the rejuvenation age (for details on this, the reader is referred to Ghodla et al (2022), Section 2.1). The BNS merger rates reported by the LVK are given in Table 1, and shown against our F G data in Figure 1.…”

Section: Bns Merger Ratesmentioning

confidence: 99%

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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: Introductionmentioning

confidence: 93%

Section: Bns Merger Ratesmentioning

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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“…In this work we have used a satellite routine of the suite referred to as v1 to make additions in a post-processing manner (discussed below) to the models. was previously used in Ghodla et al (2022), but we name it here for the first time. Apart from the implementation discussed below in section 4.2, 4.3, we also consider pulsation pair-instability (PPI -see Woosley et al 2007) in by following the fits in Stevenson et al (2019) (eq.…”

Section: Bpass Input Parametersmentioning

confidence: 99%

“…For determining the mass of the compact remnant, we use the standard remnant mass implementation in , (see, Ghodla et al 2022). Finally,…”

Section: Implementation Of Tidal Chementioning

confidence: 99%

Evaluating chemically homogeneous evolution in stellar binaries: Electromagnetic implications -- Ionizing photons, SLSN-I, GRB, Ic-BL

Ghodla¹,

Eldridge²,

Stanway³

et al. 2022

Preprint

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We investigate the occurrence of rapid rotation induced Chemically Homogeneous Evolution (CHE) caused by strong tides and mass accretion in binary systems. Using , we derive a relation for the minimum initial angular frequency required by a single star to experience CHE. This is then extended to derive a similar relation for accretion induced CHE in binaries by generalizing the analytical relation in Packet (1981). In contrast to traditionally assumed 5-10 per cent accretion of initial mass for spinning up an accretor (resulting in CHE) with 𝑍 0.004 and 𝑀 20M , this value can drop to ∼ 2 per cent for efficient angular momentum accretion. On the other hand, for certain systems, one might overestimate the efficiency of accretion induced spin-up. We conduct a population study using by evolving stars under the influence of strong tides in short-period binaries and also account for the updated effect of accretion induced rapid rotation. We find accretion CHE (compared to tidal CHE) to be the dominant means of producing homogeneous stars even at 10 per cent angular momentum accretion efficiency during mass transfer. Unlike tidal CHE, it is seen that CH stars arising due to accretion can retain a larger fraction of their angular momentum till core-collapse. Thus we show that accretion CHE could be an important formation channel for electromagnetic transients like GRBs/Ic-BL (SLSN-I/Ic-BL) under the collapsar (magnetar) formalism and a single CH star could lead to both the transients under their respective formation scenario.

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“…This allows us to take a different approach when comparing observational systems and theory: instead of creating a model to match the observations as best as possible, we can search through our existing predictions and find systems which are similar to those observed (e.g. Xiao et al 2019;Tang et al 2020;Stanway et al 2020;Stevance et al 2020;Stevance & Eldridge 2021;Byrne et al 2021;Briel et al 2022;Chrimes et al 2022;Ghodla et al 2022;Stevance et al 2022).…”

Section: Introductionmentioning

confidence: 99%

VFTS 243 as predicted by the BPASS fiducial models

Stevance¹,

Ghodla²,

Richards³

et al. 2022

Preprint

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The recent discovery of an unambiguous quiescent BH and main sequence O star companion in VFTS 243 opens the door to new constraints on theoretical stellar evolution and population models looking to reproduce the progenitors of black hole -black hole binaries. Here we show that the Binary Population and Spectral Synthesis fiducial models (BPASSv2.2.1) natively predict VFTS 243-like systems: We find that VFTS 243 likely originated from a binary system in a ∼15 day orbit with primary mass ranging from 40 to 50 M and secondary star with initial mass 24-25 M . Additionally we find that the death of the primary star must have resulted in a low energy explosion 𝐸 < 10 50 ergs. With a uniform prior we find that the kick velocity of the new-born black hole was < 33 km s −1 (90 percent credible interval). The very low eccentricity reported for VFTS 243 and the subsequent conclusion by the authors that the SN kick must have been very small is in line with the peak in the posterior distribution between 0 and 5 km s −1 . Finally, the reduced Hobbs kick distribution commonly used in black hole population synthesis is strongly disfavoured, whereas the Bray kick with the most recent parameter calibration predicts 2 ± 3.5 km s −1 , which is very consistent with the posterior velocity distributions obtained for our matching VFTS 243-like models using a uniform kick prior.

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Forward modelling the O3(a+b) GW transient mass distributions with bpass by varying compact remnant mass and SNe kick prescriptions

Cited by 17 publications

References 54 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

Evaluating chemically homogeneous evolution in stellar binaries: Electromagnetic implications -- Ionizing photons, SLSN-I, GRB, Ic-BL

VFTS 243 as predicted by the BPASS fiducial models

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