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

Gottlieb, Ore; Nagakura, Hiroki; Tchekhovskoy, Alexander; Natarajan, Priyamvada; Ramírez-Ruiz, E.; Banagiri, S.; Jacquemin-Ide, Jonatan; Kaaz, Nicholas; Kalogera, V.

doi:10.3847/2041-8213/ace03a

Cited by 7 publications

(12 citation statements)

References 81 publications

(81 reference statements)

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“…Each accretion disk of an episode has a mass of ≈10 −2 M e and the jets of each episode carry ≈10% of this mass. Although the asymmetrical accretion process onto the NS accompanied by rotation can lead to gravitational wave emission (e.g., Dall'Osso & Stella 2007;Menon et al 2023), based on the results of Gottlieb et al (2023), I expect that in the JJEM the jittering jets are the major source of gravitational waves.…”

Section: The Assumptions Of the Toy Modelmentioning

confidence: 99%

The Neutron Star to Black Hole Mass Gap in the Frame of the Jittering Jets Explosion Mechanism (JJEM)

Soker

2023

Res. Astron. Astrophys.

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I build a toy model in the frame of the jittering jets explosion mechanism (JJEM) of core collapse supernovae (CCSNe) that incorporates both the stochastically varying angular momentum component of the material that the newly born neutron star (NS) accretes and the constant angular momentum component and show that the JJEM can account for the $\simeq 2.5-5 M_\odot$ mass gap between NSs and black holes (BHs). The random component of the angular momentum results from pre-collapse core convection fluctuations that are amplified by post-collapse instabilities. The fixed angular momentum component results from pre-collapse core rotation. For slowly rotating pre-collapse cores the stochastic angular momentum fluctuations form intermittent accretion disks (or belts) around the NS with varying angular momentum axes in all directions. The intermittent accretion disk/belt launches jets in all directions that expel the core material in all directions early on, hence leaving a NS remnant. Rapidly rotating pre-collapse cores form an accretion disk with angular momentum axis that is about the same as the pre-collapse core rotation. The NS launches jets along this axis and hence the jets avoid the equatorial plane region. In-flowing core material continues to feed the central object from the equatorial plane increasing the NS mass to form a BH. The narrow transition from slow to rapid pre-collapse core rotation, i.e., from an efficient to inefficient jet feedback mechanism, accounts for the sparsely populated mass gap.

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Section: The Assumptions Of the Toy Modelmentioning

confidence: 99%

The Neutron Star to Black Hole Mass Gap in the Frame of the Jittering Jets Explosion Mechanism (JJEM)

Soker

2023

Res. Astron. Astrophys.

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“…The goal of this exploratory study is to estimate the expected contribution of jittering jets to gravitational wave emission from CCSNe. The motivation for this studyresults from recent studies that support the jittering jets explosion mechanism (JJEM) of CCSNe (e.g., Soker 2022aSoker , 2022cSoker , 2023bShishkin & Soker 2023), and the very recent study by Gottlieb et al (2023) who found that the turbulent cocoons that energetic relativistic jets form can be a strong source of gravitational waves. A cocoon is the convective bubble that a jet inflates, even if not relativistic (e.g., Izzo et al 2019), and is filled with the shocked jet's material and the shocked ambient material.…”

Section: Introductionmentioning

confidence: 99%

“…A cocoon is the convective bubble that a jet inflates, even if not relativistic (e.g., Izzo et al 2019), and is filled with the shocked jet's material and the shocked ambient material. Gottlieb et al (2023) simulated relativistic and very energetic jets, ≈10 52 -10 53 erg, that are relevant to rare CCSNe where the pre-explosion core is rapidly rotating and the collapsing core is likely to form a black hole. There are many studies of such rare CCSNe that have fixed-axis jets; some do not consider gravitational waves from jets (e.g., Khokhlov et al 1999;Aloy et al 2000;Maeda et al 2012;López-Cámara et al 2013;Bromberg & Tchekhovskoy 2016;Nishimura et al 2017;Wang et al 2019;Grimmett et al 2021;Gottlieb et al 2022;Perley et al 2022;Urrutia et al 2023a;Obergaulinger & Reichert 2023), while others do (e.g., analytically Segalis & Ori 2001;Du et al 2018;Yu 2020;Leiderschneider &Piran 2021 andnumerically Urrutia et al 2023b;Gottlieb et al 2023).…”

Section: Introductionmentioning

confidence: 99%

“…There are many studies of such rare CCSNe that have fixed-axis jets; some do not consider gravitational waves from jets (e.g., Khokhlov et al 1999;Aloy et al 2000;Maeda et al 2012;López-Cámara et al 2013;Bromberg & Tchekhovskoy 2016;Nishimura et al 2017;Wang et al 2019;Grimmett et al 2021;Gottlieb et al 2022;Perley et al 2022;Urrutia et al 2023a;Obergaulinger & Reichert 2023), while others do (e.g., analytically Segalis & Ori 2001;Du et al 2018;Yu 2020;Leiderschneider &Piran 2021 andnumerically Urrutia et al 2023b;Gottlieb et al 2023). The results of Gottlieb et al (2023) are suitable to apply to the JJEM.…”

Section: Introductionmentioning

confidence: 99%

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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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“…The jet wobbling is caused by the spontaneous tilt of the disk, induced by the stochastic torques applied to the disk by infalling gas. Consequently, a given observer will only see a fraction of the jet energy, so that the observed jet energy is in fact an order of magnitude lower than the true jet energy (Gottlieb et al 2023). In such cases, the total GRB jet energy is…”

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confidence: 99%

Collapsar Black Holes Are Likely Born Slowly Spinning

Gottlieb,

Jacquemin-Ide,

Lowell

et al. 2023

ApJL

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Collapsing stars constitute the main black hole (BH) formation channel, and are occasionally associated with the launch of relativistic jets that power γ-ray bursts (GRBs). Thus, collapsars offer an opportunity to infer the natal (before spin-up/down by accretion) BH spin directly from observations. We show that once the BH saturates with a large-scale magnetic flux, the jet power is dictated by the BH spin and mass accretion rate. Core-collapse simulations by Halevi et al. and GRB observations favor stellar density profiles that yield an accretion rate of m ̇ ≈ 10 − 2 M ⊙ s − 1 , weakly dependent on time. This leaves the spin as the main factor that governs the jet power. By comparing the jet power to characteristic GRB luminosities, we find that the majority of BHs associated with jets are likely born slowly spinning with a dimensionless spin of a ≃ 0.2, or a ≃ 0.5 for wobbling jets, with the main uncertainty originating in the unknown γ-ray radiative efficiency. This result could be applied to the entire core-collapse BH population, unless an anticorrelation between the stellar magnetic field and angular momentum is present. In a companion paper, Jacquemin-Ide et al., we show that regardless of the natal spin, the extraction of BH rotational energy leads to spin-down to a ≲ 0.2, consistent with gravitational-wave observations. We verify our results by performing the first 3D general-relativistic magnetohydrodynamic simulations of collapsar jets with characteristic GRB energies, powered by slowly spinning BHs. We find that jets of typical GRB power struggle to escape from the star, providing the first numerical indication that many jets fail to generate a GRB.

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

Cited by 7 publications

References 81 publications

The Neutron Star to Black Hole Mass Gap in the Frame of the Jittering Jets Explosion Mechanism (JJEM)

The Neutron Star to Black Hole Mass Gap in the Frame of the Jittering Jets Explosion Mechanism (JJEM)

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

Collapsar Black Holes Are Likely Born Slowly Spinning

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