Gravitational Wave Radiation from Newborn Accreting Magnetars

Cheng, Quan; Zheng, Xiaoping; Fan, X.; Huang, Xi

doi:10.1088/1674-4527/acaa90

Cited by 3 publications

(3 citation statements)

References 107 publications

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“…The saturation amplitudes of the secular bar mode and inertial r mode are quite uncertain. Considering that the GW radiation from the magnetic deformation of the remnants may be relatively strong compared to the r-mode instability (Glampedakis & Gualtieri 2018;Cheng et al 2023), it is believed that the GW radiation from the r-mode instability will have a minor effect on our results. For the secular bar-mode instability, all of our samples during their evolution progress show a lower ratio of rotational kinetic energy T to gravitational binding energy W than 0.14, i.e., T/|W| < 0.14, which means the secular bar-mode instability is ineffective for our samples.…”

Section: Gmentioning

confidence: 92%

Revisiting the Constraint on the Equation of State of Neutron Stars Based on Binary Neutron Star Mergers

Li,

Chen,

Lin

et al. 2024

ApJ

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The merger of a neutron star (NS)–NS binary can form different productions of compact remnants, among which a supramassive NS (SMNS) can create an internal plateau, and the following steep decay marks the collapse of the SMNS. The proportion of the SMNS and the corresponding collapse time are often used to constrain the NS equation of state (EOS). This paper revisits this topic by considering the effect of an accretion disk on a compact remnant, which is not considered in previous works. Compared with previous works, the collapse-time distribution (peaks ∼100 s) of SMNSs formed from an NS–NS merger is almost unaffected by the initial surface magnetic field (B s,i ) of the NS, but the total energy output of the magnetic dipole radiation from the SMNSs depends on B s,i significantly. Coupling the constraints from the SMNS fraction, we exclude some EOSs and obtain three candidate EOSs, i.e., DD2, ENG, and MPA1. By comparing the distributions of the collapse time and the luminosity of the internal plateau (in the short gamma-ray bursts) for observations obtained based on the three candidate EOSs, it is shown that only the EOS of ENG is favored. Our sample, based on the ENG EOS and a mass distribution motivated by Galactic systems, suggests that approximately 99% of NS–NS mergers collapse to form a black hole (BH) within 107s. This includes scenarios promptly forming a BH (36.5%), an SMNS (60.7%), or a stable NS that transitions into a BH or an SMNS following accretion (2.1%). It also indicates that the remnants for GW170817 and GW190425, and the second object of GW190814, are more likely to be BHs.

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Section: Gmentioning

confidence: 92%

Revisiting the Constraint on the Equation of State of Neutron Stars Based on Binary Neutron Star Mergers

Li,

Chen,

Lin

et al. 2024

ApJ

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“…Gravitational waves from CCSNe are yet to be detected (e.g., Szczepańczyk et al 2023). Recent studies concentrate on the expected gravitational waves from CCSNe during the explosion process (e.g., Powell & Müller 2019;Lin et al 2023;Mezzacappa et al 2023;Pastor-Marcos et al 2023;Wolfe et al 2023; for more on the results of some studies see Section 3) and shortly after explosion, e.g., in relation to magnetar formation (e.g., Cheng et al 2023;Menon et al 2023).…”

Section: Introductionmentioning

confidence: 99%

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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“…Gravitational waves from CCSNe are yet to be detected (e.g., Szczepańczyk et al 2023). Recent studies concentrate on the expected gravitational waves from CCSNe during the explosion process (e.g., Powell & Müller 2019;Lin et al 2023;Mezzacappa et al 2023;Wolfe et al 2023;Pastor-Marcos et al 2023; for more on the results of some studies see section 3) and shortly after explosion, e.g., in relation to magnetar formation (e.g., Cheng et al 2023;Menon, Guetta, & Dall'Osso 2023).…”

Section: Introductionmentioning

confidence: 99%

Boosting Jittering Jets by Neutrino Heating in Core Collapse Supernovae

Soker¹

2022

Res. Astron. Astrophys.

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I estimate the energy that neutrino heating adds to the outflow that jets induce in the collapsing core material in core collapse supernovae (CCSNe), and find that this energy crudely doubles the energy that the jets deposit into the outer core. I consider the jittering jets explosion mechanism where there are several stochastic jet-launching episodes, each lasting for about 0.01-0.1 seconds. The collapsing core material passes through the stalled shock at about 100 km and then slowly flows onto the proto-neutron star (NS). I assume that the proto-NS launches jittering jets, and that the jets break out from the stalled shock. I examine the boosting process by which the high-pressure gas inside the stalled shock, the gain region material, expands alongside the jets and does work on the material that the jets shock, the cocoon. This work is crudely equal to the energy that the original jets carry. I argue that the coupling between instabilities, stochastic rotation, magnetic fields, and jittering jets lead to most CCSN explosions. In other cases, the pre-collapse core is rapidly rotating and therefore ordered rotation replaces stochastic rotation and fixed jets replace jittering jets.

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Gravitational Wave Radiation from Newborn Accreting Magnetars

Cited by 3 publications

References 107 publications

Revisiting the Constraint on the Equation of State of Neutron Stars Based on Binary Neutron Star Mergers

Revisiting the Constraint on the Equation of State of Neutron Stars Based on Binary Neutron Star Mergers

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

Boosting Jittering Jets by Neutrino Heating in Core Collapse Supernovae

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