Accretion-to-jet energy conversion efficiency in GW170817

Salafia, O. S.; Giacomazzo, B.

doi:10.1051/0004-6361/202038590

Cited by 20 publications

(15 citation statements)

References 180 publications

(195 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The electromagnetic counterpart of GW170817 strongly disfavoured a long-lived NS remnant, which would otherwise overproduce the X-ray flux at late time and inject too much energy in the relativistic ejecta to be consistent with the afterglow data (e.g. Granot, Guetta & Gill 2017;Margutti et al 2018;Pooley et al 2018;Xie, Zrake & MacFadyen 2018;Margalit & Metzger 2019;Makhathini et al 2020;Salafia & Giacomazzo 2020). Based on the assumption that GW170817 made a BH, many authors have concluded that the maximum mass of a non-rotating NS is M TOV 2.3 M (Margalit & Metzger 2017;Rezzolla, Most & Weih 2018;Shibata et al 2019; but see Ai, Gao & Zhang 2020, for a discussion of the less likely case that GW170817 did not make a BH).…”

mentioning

confidence: 96%

On the formation of GW190814

Beniamini

Bonnerot

2020

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

The LIGO-Virgo collaboration recently reported a puzzling event, GW190814, with component masses of 23 and 2.6M⊙. Motivated by the relatively small rate of such a coalescence (1–$23\rm \, Gpc^{-3}\, yr^{-1}$) and the fact that the mass of the secondary is close to the total mass of known binary neutron star (bNS) systems, we propose that GW190814 was a second-generation merger from a hierarchical triple system, i.e. the remnant from the bNS coalescence was able to merge again with the 23M⊙ black hole (BH) tertiary. We show that this occurs at a sufficiently high probability provided that the semimajor axis of the outer orbit is less than a few AU at the time of bNS coalescence. It remains to be explored whether the conditions for the formation of such tight triple systems are commonly realized in the Universe, especially in low metallicity (≲ 0.1Z⊙) environments. Our model provides a number of predictions. (1) The spin of the secondary in GW190814-like systems is 0.6–0.7. (2) The component mass distribution from a large sample of LIGO sources should have a narrow peak between 2.5 and ∼3.5M⊙, whereas the range between ∼3.5 and ∼5M⊙ stays empty (provided that stellar evolution does not generate such BHs in the ‘mass gap’). (3) About 90 per cent (10 per cent) of GW190814-like events have an eccentricity of e ≳ 2 × 10−3 (≳ 0.1) near gravitational wave frequency of 10 mHz. (4) A significant fraction ($\gtrsim 10{{\ \rm per\ cent}}$) of bNS mergers should have signatures of a massive tertiary at a distance of a few AU in the gravitational waveform. (5) There are 105 undetected radio-quiet bNS systems with a massive BH tertiary in the Milky Way.

show abstract

mentioning

confidence: 96%

On the formation of GW190814

Beniamini

Bonnerot

2020

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…It also showed the importance of population studies required to disentangle the microphysics of the source and its interaction with the environment, from the source geometry and energetics. Increasing the number of joint detections will make it possible to determine the equation of state of neutron stars 171 , to probe the properties of different components of the mass ejected during and after the merger [172][173][174] , to understand if the BNS mergers are the primary channel of formation of heavy elements and the details of the nuclear physics relevant to nucleosynthesis 175 , and to understand the structure of the relativistic jets and the physics behind their formation 176,177 .…”

Section: Dawn Of a New Multi-messenger Eramentioning

confidence: 99%

Gravitational-wave physics and astronomy in the 2020s and 2030s

et al. 2021

View full text Add to dashboard Cite

The past five years have witnessed a revolution in astronomy. The direct detection of gravitational waves (GW) emitted from the binary black hole (BBH) merger GW150914 (Fig. 1) by the Advanced Laser Interferometer Gravitational-Wave Observatory (LIGO) detector 1 on September 14, 2015 (reF. 2 ) was a watershed event, not only in demonstrating that GWs could be directly detected but more fundamentally in revealing new insights into these exotic objects and the Universe itself. On August 17, 2017, the Advanced LIGO and Advanced Virgo 3 detectors jointly detected GW170817, the merger of a binary neutron star (BNS) system 4 , an equally momentous event leading to the observation of electromagnetic (EM) radiation emitted across the entire spectrum through one of the most intense astronomical observing campaigns ever undertaken 5 .Coming nearly 100 years after Albert Einstein first predicted their existence 6 , but doubted that they could ever be measured, the first direct GW detections have undoubtedly opened a new window on the Universe. The scientific insights emerging from these detections have already revolutionized multiple domains of physics and astrophysics, yet, they are 'the tip of the iceberg' , representing only a small fraction of the future potential of GW astronomy. As is the case for the Universe seen through EM waves, different classes of astrophysical sources emit GWs across a broad spectrum ranging over more than 20 orders of magnitude, and require different detectors for the range of frequencies of interest (Fig. 2).In this Roadmap, we present the perspectives of the Gravitational Wave International Committee (GWIC, https://gwic.ligo.org) on the emerging field of GW astronomy and physics in the coming decades. The GWIC was formed in 1997 to facilitate international collaboration and cooperation in the construction, operation and use of the major GW detection facilities worldwide. Its primary goals are: to promote international cooperation in all phases of construction and scientific exploitation of GW detectors, to coordinate and support long-range planning for new instruments or existing instrument upgrades, and to promote the development of GW detection as an astronomical tool, exploiting especially the potential for multi-messenger astrophysics. Our intention in this Roadmap is to present a survey of the science opportunities and to highlight the future detectors that will be needed to realize those opportunities. The recent remarkable discoveries in GW astronomy have spurred the GWIC to re-examine and update the GWIC roadmap originally published a decade ago 7 .We first present an overview of GWs, the methods used to detect them and some scientific highlights from the past five years. Next, we provide a detailed survey

show abstract

“…Two often proposed candidates are the Blandford-Znajek (BZ) mechanism (Blandford & Znajek 1977) and neutrino pair annihilation (Eichler et al 1989;Mészáros & Rees 1992;Just et al 2016). Salafia & Giacomazzo (2021) (hereafter referred to as SG21) discuss both mechanisms in detail and derive disk accretion-to-jet energy conversion efficiencies. For GW170817, they calculate that both mechanisms have efficiencies which are consistent with GRB170817 and they can therefore not distinguish between the two.…”

Section: Grb Jetmentioning

confidence: 99%

Investigating the detection rates and inference of gravitational-wave and radio emission from black hole neutron star mergers

Boersma¹,

Leeuwen²

2022

Preprint

View full text Add to dashboard Cite

Context. Black hole neutron star (BHNS) mergers have recently been detected through their gravitational-wave (GW) emission. While no electromagnetic emission (EM) has yet been confidently associated with these systems, observing any such emission could provide information on, for example, the neutron star (NS) equation of state (EOS). BHNS mergers could produce EM emission as a short gamma-ray burst (sGRB), and/or an sGRB afterglow upon interaction with the circummerger medium. Aims. Here, we make predictions for the expected detection rates with the Square Kilometre Array Phase 1 (SKA1) of sGRB radio afterglows associated with BHNS mergers. We also investigate the benefits of a multimessenger analysis in inferring the properties of the merging binary. Methods. We simulate a population of BHNS mergers, making use of recent stellar population synthesis results, and estimate their sGRB afterglow flux to obtain the detection rates with SKA1. We investigate how this rate depends on the GW detector sensitivity, the primary black hole spin, and the NS EOS. We then perform a multimessenger Bayesian inference study on a fiducial BHNS merger. We simulate its sGRB afterglow and GW emission, as input to this study, using recent models for both and take systematic errors into account.Results. The expected rates of a combined GW and radio detection with the current generation GW detectors are likely low. Due to the much increased sensitivity of future GW detectors like the Einstein Telescope, the chances of an sGRB localisation and radio detection increase substantially. The unknown distribution of the BH spin has a big influence on the detection rates, however, and it is a large source of uncertainty. Furthermore, for our fiducial BHNS merger we are able to infer both the binary source parameters as well as the parameters of the sGRB afterglow simultaneously, when combining the GW and radio data. The radio data provides useful extra information on the binary parameters such as the mass ratio but this is limited by the systematic errors involved. Conclusions. The probability of finding an sGRB afterglow of a BHNS merger is low in the near future but rises significantly when the next generation GW detectors come online. Combining information from GW data with radio data is crucial to characterise the jet properties. A better understanding of the systematics will further increase the amount of information on the binary parameters that can be extracted from this radio data.

show abstract

Accretion-to-jet energy conversion efficiency in GW170817

Cited by 20 publications

References 180 publications

On the formation of GW190814

On the formation of GW190814

Gravitational-wave physics and astronomy in the 2020s and 2030s

Investigating the detection rates and inference of gravitational-wave and radio emission from black hole neutron star mergers

Contact Info

Product

Resources

About