Gravitational waves from the propagation of long gamma-ray burst jets

Urrutia, Gerardo; Colle, Fabio De; Moreno, Claudia; Zanolin, M.

doi:10.1093/mnras/stac3433

Cited by 6 publications

(4 citation statements)

References 64 publications

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“…The on-axis emission, i.e., when the jets' axis is at a very small angle to the line of sight, has a strain amplitude that is more than an order of magnitude smaller than for the off-axis emission and the strain amplitude peaks at frequencies of 10-100 Hz. I note that the simulations by Urrutia et al (2023b), who study gravitational waves from jets in gamma-ray bursts but do not concentrate on turbulence, yield different spectra and lower strains. To scale for one pair of jittering jets I consider the threedimensional simulations by Papish & Soker (2014b).…”

Section: Estimating Gravitational Waves From Jittering Jetsmentioning

confidence: 94%

Predicting Gravitational Waves from Jittering-jets-driven Core Collapse Supernovae

Soker

2023

Res. Astron. Astrophys.

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I estimate the frequencies of gravitational waves from jittering jets that explode core collapse supernovae (CCSNe) to crudely be 5-30 Hz, and with strains that might allow detection of Galactic CCSNe. The jittering jets explosion mechanism (JJEM) asserts that most CCSNe are exploded by jittering jets that the newly born neutron star (NS) launches within few seconds. According to the JJEM, instabilities in the accreted gas lead to the formation of intermittent accretion disks that launch the jittering jets. Earlier studies that did not include jets calculated the gravitational frequencies that instabilities around the NS emit to have a peak in the crude frequency range of 100-2000 Hz. Based on a recent study, I take the source of the gravitational waves of jittering jets to be the turbulent bubbles (cocoons) that the jets inflate as they interact with the outer layers of the core of the star at thousands of kilometres from the NS. The lower frequencies and larger strain than those of gravitational waves from instabilities in CCSNe allow future, and maybe present, detectors to identify the gravitational wave signals of jittering jets. Detection of gravitational waves from local CCSNe might distinguish between the neutrino-driven explosion mechanism and the JJEM.

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Section: Estimating Gravitational Waves From Jittering Jetsmentioning

confidence: 94%

Predicting Gravitational Waves from Jittering-jets-driven Core Collapse Supernovae

Soker

2023

Res. Astron. Astrophys.

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“…Their enormous power makes LGRB jets interesting GW sources. The GW frequency is inversely proportional to the timescale over which the metric is perturbed, and for jets, this timescale is set by the longer of the launching and acceleration timescales (Sago et al 2004;Hiramatsu et al 2005;Akiba et al 2013;Birnholtz & Piran 2013;Yu 2020;Leiderschneider & Piran 2021;Urrutia et al 2022). Thus, the characteristic duration of LGRBs, 10 s, places the GW emission from LGRB jets at the sub-Hertz frequency band, too low for LVK, but potentially detectable by the proposed space-based DECi-hertz Interferometer Gravitational wave Observatory (Kawamura et al 2011).…”

Section: Introductionmentioning

confidence: 99%

Jetted and Turbulent Stellar Deaths: New LVK-detectable Gravitational-wave Sources

Gottlieb

Nagakura

Tchekhovskoy

et al. 2023

ApJL

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Upcoming LIGO–Virgo–KAGRA (LVK) observing runs are expected to detect a variety of inspiralling gravitational-wave (GW) events that come from black hole and neutron star binary mergers. Detection of noninspiral GW sources is also anticipated. We report the discovery of a new class of noninspiral GW sources—the end states of massive stars—that can produce the brightest simulated stochastic GW burst signal in the LVK bands known to date, and could be detectable in LVK run A+. Some dying massive stars launch bipolar relativistic jets, which inflate a turbulent energetic bubble—cocoon—inside of the star. We simulate such a system using state-of-the-art 3D general relativistic magnetohydrodynamic simulations and show that these cocoons emit quasi-isotropic GW emission in the LVK band, ∼10–100 Hz, over a characteristic jet activity timescale ∼10–100 s. Our first-principles simulations show that jets exhibit a wobbling behavior, in which case cocoon-powered GWs might be detected already in LVK run A+, but it is more likely that these GWs will be detected by the third-generation GW detectors with an estimated rate of ∼10 events yr−1. The detection rate drops to ∼1% of that value if all jets were to feature a traditional axisymmetric structure instead of a wobble. Accompanied by electromagnetic emission from the energetic core-collapse supernova and the cocoon, we predict that collapsars are powerful multimessenger events.

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“…Afle et al (2023) use multidimensional models to analyze the detectability of f-mode GW frequencies with third generation GW detectors. More exotically, Urrutia et al (2023) explore the impact of the viewing angle of GW emission from long gamma-ray burst jets.…”

Section: Introductionmentioning

confidence: 99%

Characterizing the Directionality of Gravitational Wave Emission from Matter Motions within Core-collapse Supernovae

Pajkos,

VanCamp,

Pan

et al. 2023

ApJ

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We analyze the directional dependence of the gravitational wave (GW) emission from 15 3D neutrino radiation hydrodynamic simulations of core-collapse supernovae (CCSNe). Using spin weighted spherical harmonics, we develop a new analytic technique to quantify the evolution of the distribution of GW emission over all angles. We construct a physics-informed toy model that can be used to approximate GW distributions for general ellipsoid-like systems, and use it to provide closed form expressions for the distribution of GWs for different CCSN phases. Using these toy models, we approximate the protoneutron star (PNS) dynamics during multiple CCSN stages and obtain similar GW distributions to simulation outputs. When considering all viewing angles, we apply this new technique to quantify the evolution of preferred directions of GW emission. For nonrotating cases, this dominant viewing angle drifts isotropically throughout the supernova, set by the dynamical timescale of the PNS. For rotating cases, during core bounce and the following tens of milliseconds, the strongest GW signal is observed along the equator. During the accretion phase, comparable—if not stronger—GW amplitudes are generated along the axis of rotation, which can be enhanced by the low T/∣W∣ instability. We show two dominant factors influencing the directionality of GW emission are the degree of initial rotation and explosion morphology. Lastly, looking forward, we note the sensitive interplay between GW detector site and supernova orientation, along with its effect on detecting individual polarization modes.

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Gravitational waves from the propagation of long gamma-ray burst jets

Cited by 6 publications

References 64 publications

Predicting Gravitational Waves from Jittering-jets-driven Core Collapse Supernovae

Predicting Gravitational Waves from Jittering-jets-driven Core Collapse Supernovae

Jetted and Turbulent Stellar Deaths: New LVK-detectable Gravitational-wave Sources

Characterizing the Directionality of Gravitational Wave Emission from Matter Motions within Core-collapse Supernovae

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