Neutron Star Natal Kick and Jets in Core Collapse Supernovae

Bear, Ealeal; Soker, Noam

doi:10.3847/1538-4357/aaad07

Cited by 23 publications

(29 citation statements)

References 108 publications

(149 reference statements)

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“…4. The new addition of SNR 0540-69.3 is compatible with the conclusion of Bear & Soker (2018a) and strengthens it.…”

Section: A Point-symmetric Morphologysupporting

confidence: 73%

“…I also note that the transverse component of the natal kick velocity of the pulsar that I deduce here is almost opposite to the direction that Serafimovich et al ( 2005) argued for and that was refuted by Mignani et al (2010). Bear & Soker (2018a) present the distribution of the projected angles α between the jets' axis and the NS kick velocity for 12 SNRs. They conclude that the cumulative distribution function fits the random distribution (kick velocity is random with respect to the main jet-axis) at large angles, and is missing systems with small angles relative to the random distribution.…”

Section: A Point-symmetric Morphologycontrasting

confidence: 40%

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Imprints of the jittering jets explosion mechanism in the morphology of the supernova remnant SNR 0540-69.3

Soker

2021

Preprint

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I identify a point-symmetric structure in recently published velocity maps of different elements in a plane along the line of sight at the center of the supernova remnant SNR 0540-69.3, and argue that jittering jets that exploded this core collapse supernova shaped this point-symmetric structure. The four pairs of two opposite clumps that compose this point symmetric structure suggest that two to four pairs of jittering jets shaped the inner ejecta in this plane. In addition, intensity images of several spectral lines reveal a faint strip (the main jet-axis) that is part of this plane of jittering jets and its similarity to morphological features in a few other SNRs and in some planetary nebulae further suggests shaping by jets. My interpretation implies that in addition to instabilities, jets also mix elements in the ejecta of core collapse supernovae. Based on the point-symmetric structure and under the assumption that jittering jets exploded this supernova, I estimate the component of the neutron star natal kick velocity on the plane of the sky to be 235 km s −1 , and at an angle of 47 • to the direction of the main jet-axis. I analyse this natal kick direction together with other 12 SNRs in the frame of the jittering jets explosion mechanism.

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“…4. The new addition of SNR 0540-69.3 is compatible with the conclusion of Bear & Soker (2018a) and strengthens it.…”

Section: A Point-symmetric Morphologysupporting

confidence: 73%

Section: A Point-symmetric Morphologycontrasting

confidence: 40%

Imprints of the jittering jets explosion mechanism in the morphology of the supernova remnant SNR 0540-69.3

Soker

2021

Preprint

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“…We also note that other mechanisms have been proposed to explain the single NS velocities observed (e.g. Bear & Soker 2018)…”

Section: The Feasibility Of Our Best-fit α and β Valuesmentioning

confidence: 57%

Neutron star kicks – II. Revision and further testing of the conservation of momentum ‘kick’ model

Bray

Eldridge

2018

Monthly Notices of the Royal Astronomical Society

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In Bray & Eldridge (2016) we proposed a simple neutron star "kick" formula, v kick = α (M ejecta / M remnant )+β to explain the observed 2D velocities of young single neutron stars. Using this kick we found that there is no statistically significant preference for a kick orientation nor for any of the three initial mass function (IMF) slopes tested, and that populations including binary stars reproduced the kick distribution better than single star only populations. However, recent analysis by Janka (2017), prompted us to revisit our basic assumptions and our new analysis has led to revised "best-fit" kick values of α = 100 km s −1 and β = −170 km s −1 . The reduction of β to a negative value is due to using the 2D observed kick velocity distribution rather than the modelled 3D velocity distribution for neutron stars (NS). To further test the validity of the new kick, we have created synthetic populations of runaway star and double neutron star (DNS) binaries at solar metallicity (Z = 0.020) using our best-fit kick. We find our new kick values create runaway star velocities and DNS period distributions in agreement with the comparable observational distributions with only the DNS eccentricities in tension with the observations. From our DNS and BH-BH datasets we estimate a predicted DNS merger rate at solar metallicity of 3,864 +1,570 −2,371 Gpc −3 yr −1 and a BH-BH merger rate of 5 +40 −1 Gpc −3 yr −1 .

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“…From the magnitude of the velocity alone we can rule out binary disruption (Iben & Tutukov 1996;Fryer et al 1998). Some jet models predict large scale morphological distortions in the SNR along the axis defined by the pulsar's proper motion (Bear & Soker 2018). This is not seen in the case of SNR CTB 1 which is remarkably circularly symmetric in both optical Hα and non-thermal radio.…”

Section: Psr J0002+6216 and Pulsar Kick Mechanismsmentioning

confidence: 91%

The Tail of PSR J0002+6216 and the Supernova Remnant CTB 1

Schinzel

Kerr

Rau

et al. 2019

ApJL

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We have carried out VLA imaging and a Fermi timing analysis of the 115 ms γ-ray and radio pulsar PSR J0002+6216. We found that the pulsar lies at the apex of a narrowly collimated cometary-like 7 tail of non-thermal radio emission which we identify as a bow-shock pulsar wind nebula. The tail of the nebula points back toward the geometric center of the supernova remnant CTB 1 (G116.9+0.2) 28 away, at a position angle θ µ = 113 • . We measure a proper motion with 2.9 σ significance from a Fermi timing analysis giving µ=115±33 mas yr −1 and θ µ = 121 • ± 13 • , corresponding to a large transverse pulsar velocity of 1100 km s −1 at a distance of 2 kpc. This proper motion is of the right magnitude and direction to support the claim that PSR J0002+6216 was born from the same supernova that produced CTB 1. We explore the implications for pulsar birth periods, asymmetric supernova explosions, and mechanisms for pulsar natal kick velocities.

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Neutron Star Natal Kick and Jets in Core Collapse Supernovae

Cited by 23 publications

References 108 publications

Imprints of the jittering jets explosion mechanism in the morphology of the supernova remnant SNR 0540-69.3

Imprints of the jittering jets explosion mechanism in the morphology of the supernova remnant SNR 0540-69.3

Neutron star kicks – II. Revision and further testing of the conservation of momentum ‘kick’ model

The Tail of PSR J0002+6216 and the Supernova Remnant CTB 1

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