Comparing Neutron Star Kicks to Supernova Remnant Asymmetries

Holland-Ashford, Tyler; Lopez, Laura A.; Auchettl, Katie; Temim, Tea; Ramírez-Ruiz, E.

doi:10.3847/1538-4357/aa7a5c

Cited by 81 publications

(81 citation statements)

References 213 publications

(308 reference statements)

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“…We note that four out of the six SNRs that they show in their figure 4 have been studied by us for jets, here and in previous papers. From the direction of the jets that we deduce and the NS motion given by Holland-Ashford et al (2017) in each of these four CCSNRs, we have tentative indications that the natal kick of the NS is more or less perpendicular to the axis of the last jets.…”

Section: Discussionmentioning

confidence: 69%

“…In a future work we plan to address the relative motion of the NS and the SNR within the frame of the JFM. For example, in a recent paper Holland-Ashford et al (2017) compare the morphology of CCSNRs with the motion of the NS at their center. We note that four out of the six SNRs that they show in their figure 4 have been studied by us for jets, here and in previous papers.…”

Section: Discussionmentioning

confidence: 99%

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The imprints of the last jets in core collapse supernovae

Bear

Grichener²,

Soker

2017

Monthly Notices of the Royal Astronomical Society

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We analyze the morphologies of three core collapse supernova remnants (CCSNRs) and the energy of jets in other CCSNRs and in Super Luminous Supernovae (SLSNe) of type Ib/Ic/IIb, and conclude that these properties are well explained by the last jets' episode as expected in the jet feedback explosion mechanism of core collapse supernovae (CCSNe). The presence of two opposite protrusions, termed ears, and our comparison of the CCSNR morphologies with morphologies of planetary nebulae strengthen the claim that jets play a major role in the explosion mechanism of CCSNe. We crudely estimate the energy that was required to inflate the ears in two CCSNRs, and assume that the ears were inflated by jets. We find that the energies of the jets that inflated ears in 11 CCSNRs span a range that is similar to that of jets in some energetic CCSNe (SLSNe), and that this energy, only of the last jets' episode, is much less than the explosion energy. This finding is compatible with the jet feedback explosion mechanism of CCSNe, where only the last jets, that carry a small fraction of the total energy carried by earlier jets, are expected to influence the outer parts of the ejecta. We reiterate our call for a paradigm shift from neutrino-driven to jet-driven explosion models of CCSNe.

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Section: Discussionmentioning

confidence: 69%

Section: Discussionmentioning

confidence: 99%

The imprints of the last jets in core collapse supernovae

Bear

Grichener²,

Soker

2017

Monthly Notices of the Royal Astronomical Society

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“…Even more, in the case that PSR J1907+062 is not associated with the SNR G40.5−0.5 and supposing that it was born at the centroid of the γ-ray emission and traveled for 11 kyr to its actual position leaving a relic TeV nebula behind, it would require a transverse velocity of ∼ 3800 km s −1 (for distance of 8 kpc). This is an unrealistic fast motion when compared to the velocity of Galactic pulsars (Holland-Ashford et al 2017;Verbunt et al 2017).…”

Section: Origin Of the Tev Emissionmentioning

confidence: 96%

Radio study of the extended TeV source VER J1907+062

Duvidovich

Petriella

Giacani

2019

Monthly Notices of the Royal Astronomical Society

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This paper aims to provide new insights on the origin of the TeV source VER J1907+062 through new high-quality radio observations. We used the Karl G. Jansky Very Large Array (VLA) to observe the whole extension of VER J1907+062 at 1.5 GHz with a mosaicking technique and the PSR J1907+0602 in a single pointing at 6 GHz. These data were used together with 12 CO and atomic hydrogen observations obtained from public surveys to investigate the interstellar medium in the direction of VER J1907+062. The new radio observations do not show any evidence of a pulsar wind nebula (PWN) driven by the pulsars present in the field and no radio counterpart to the proposed X-ray PWN powered by PSR J1907+0602 is seen in the new VLA image at 6 GHz down to a noise level of 10 µJy beam −1 . Molecular clouds were discovered over the eastern, southern, and western borders of the radio shell of G40.5−0.5, suggesting an association with the SNR. We explored several scenarios for the origin of VER J1907+062. We propose as the most probable scenario one in which the TeV emission is produced by two separated γ-ray sources located at different distances: one of leptonic origin and associated with a PWN powered by PSR J1907+0602 at ∼ 3.2 kpc and another of hadronic origin and produced by the interaction between G40.5−0.5 and the surrounding molecular gas at ∼ 8.7 kpc.

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“…This fact is derived from observations of large peculiar velocities (order of 100 km s −1 ) of isolated radio pulsars in comparison to their progenitors O-B stars with peculiar velocities of ≈ 10 − 15 km s −1 (Lyne & E-mail: ignotur@gmail.com Lorimer 1994). The young NSs are known to be located at some offset from the centre of the associated supernova remnants (SNRs; Frail et al 1994;Holland-Ashford et al 2017). Some NSs demonstrate a bow shock as a proof of direct association of the pulsar with the SNR and large pulsar speed e.g.…”

Section: Introductionmentioning

confidence: 99%

The observed velocity distribution of young pulsars – II. Analysis of complete PSRπ

Igoshev

2020

Monthly Notices of the Royal Astronomical Society

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Understanding the natal kicks, or birth velocities, of neutron stars are essential for understanding the evolution of massive binaries as well as double neutron star formation. We use maximum likelihood methods as published in Verbunt et al. to analyse a new large dataset of parallaxes and proper motions measured by Deller et al. This sample is roughly three times larger than number of measurements available before. For both the complete sample and its younger part (spin-down ages τ < 3 Myr), we find that a bimodal Maxwellian distribution describes the measured parallaxes and proper motions better than a single Maxwellian with probability of 99.3 and 95.0 per cent respectively. The bimodal Maxwellian distribution has three parameters: fraction of low-velocity pulsars and distribution parameters σ 1 and σ 2 for low and high-velocity modes. For a complete sample, these parameters are as follows: 42 +17 −15 per cent, σ 1 = 128 +22 −18 km s −1 and σ 2 = 298 ± 28 km s −1 . For younger pulsars, which are assumed to represent the natal kick, these parameters are as follows: 20 +11 −10 per cent, σ 1 = 56 +25 −15 km s −1 and σ 2 = 336 ± 45 km s −1 . In the young population, 5 ± 3 per cent of pulsars has velocities less than 60 km s −1 . We perform multiple Monte Carlo tests for the method taking into account realistic observational selection. We find that the method reliably estimates all parameters of the natal kick distribution. Results of the velocity analysis are weakly sensitive to the exact values of scale-lengths of the Galactic pulsar distribution.

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Comparing Neutron Star Kicks to Supernova Remnant Asymmetries

Cited by 81 publications

References 213 publications

The imprints of the last jets in core collapse supernovae

The imprints of the last jets in core collapse supernovae

Radio study of the extended TeV source VER J1907+062

The observed velocity distribution of young pulsars – II. Analysis of complete PSRπ

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