Possible post-kick jets in SN 1987A

Soker, Noam

doi:10.1016/j.newast.2020.101548

Cited by 4 publications

(1 citation statement)

References 62 publications

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“…The associations between the pulsars and supernova remnants (SNRs) have been of considerable interest topics in neutron stars (NSs) astrophysics, since the radio pulses were firstly observed in the Crab Nebula in 1968 (Staelin & Reifenstein 1968), as well as the discovery of the Vela pulsar (Large, Vaughan, & Mills 1968). The story is continuing with identifying the potential NS in SN 1987A (Page et al 2020;Greco et al 2021;Soker 2021). Thanks the efforts and developments of astronomical facilities in recent years, the number of pulsars and SNRs has increased significantly.…”

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confidence: 99%

Statistical tests of young radio pulsars with/without supernova remnants: implying two origins of neutron stars

Cui,

Zhang,

et al. 2021

Preprint

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The properties of the young pulsars and their relations to the supernova remnants (SNRs) have been the interesting topics. At present, 383 SNRs in the Milky Way galaxy have been published, which are associated with 64 radio pulsars and 46 pulsars with high energy emissions. However, we noticed that 630 young radio pulsars with spin periods of less than half a second have been not yet observed the SNRs surrounding or nearby them, which arises a question of that could the two types of young radio pulsars with/without SNRs hold distinctive characteristics? Here, we employ the statistical tests on the two groups of young radio pulsars with (52) and without (630) SNRs to reveal if they share different origins. Kolmogorov-Smirnov (K-S) and Mann-Whitney-Wilcoxon (M-W-W) tests indicate that the two samples have the different distributions with parameters of spin period ( ), derivative of spin period ( ), surface magnetic field strength ( ), and energy loss rate ( ). Meanwhile, the cumulative number ratio between the pulsars with and without SNRs at the different spindown ages decreases significantly after 10 − 20 Kyr. So we propose that the existence of the two types of supernovae (SNe), corresponding to their SNR lifetimes, which can be roughly ascribed to the low-energy and high-energy SNe. Furthermore, the low-energy SNe may be formed from the 8 − 12 M ⊙ progenitor, e.g., possibly experiencing the electron capture, while the main sequence stars of 12 − 25 M ⊙ may produce the high-energy SNe probably by the iron core collapse.

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Section: Introductionmentioning

confidence: 99%

Statistical tests of young radio pulsars with/without supernova remnants: implying two origins of neutron stars

Cui,

Zhang,

et al. 2021

Preprint

View full text Add to dashboard Cite

show abstract

Statistical tests of young radio pulsars with/without supernova remnants: implying two origins of neutron stars

Cui

Zhang

et al. 2021

Monthly Notices of the Royal Astronomical Society

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The properties of the young pulsars and their relations to the supernova remnants (SNRs) have been the interesting topics. At present, 383 SNRs in the Milky Way galaxy have been published, which are associated with 64 radio pulsars and 46 pulsars with high energy emissions. However, we noticed that 630 young radio pulsars with the spin periods of less than half a second have been not yet observed the SNRs surrounding or nearby them, which arises a question of that could the two types of young radio pulsars with/without SNRs hold the distinctive characteristics? Here, we employ the statistical tests on the two groups of young radio pulsars with (52) and without (630) SNRs to reveal if they share the different origins. Kolmogorov-Smirnov (K-S) and Mann-Whitney-Wilcoxon (M-W-W) tests indicate that the two samples have the different distributions with parameters of spin period (P), derivative of spin period ($\dot{P}$), surface magnetic field strength (B) and energy loss rate ($\dot{E}$). Meanwhile, the cumulative number ratio between the pulsars with and without SNRs at the different spindown ages decreases significantly after $\rm 10-20\, Kyr$. So we propose that the existence of the two types of supernovae (SNe), corresponding to their SNR lifetimes, which can be roughly ascribed to the low-energy and high-energy SNe. Furthermore, the low-energy SNe may be formed from the $\rm 8-12\, M_{\odot }$ progenitor, e.g., possibly experiencing the electron capture, while the main sequence stars of $\rm 12-25\, M_{\odot }$ may produce the high-energy SNe probably by the iron core collapse.

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Implications of post-kick jets in core-collapse supernovae

Soker

2023

Monthly Notices of the Royal Astronomical Society

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I examine the assumption that the jets that shape the axisymmetrical morphological features of core collapse supernova (CCSN) remnants are post-kick jets, i.e., the neutron star (NS) launches these jets after the explosion and after it acquired its natal kick velocity. I find that this assumption implies that the pre-collapse cores of CCSN progenitors have sufficient angular momentum fluctuations to support jittering jets that explode the star. From the finding that the shaping-jets neither tend to be aligned with the kick velocity nor to be perpendicular to it I argue that the assumption that the shaping-jets are post-kick jets has the following implications. (1) The NS accretes mass at a radius of $r_{\rm acc} \approx 5000 {~\rm km}$ from the center of the explosion at $\approx 10 {~\rm s}$ after explosion. (2) The required angular momentum fluctuations of the accreted gas to explain the medium values of jets-kick angles are also sufficient to support an intermittent pre-kick accretion disk, just before and during the explosion. Such an intermittent accretion disk is likely to launch jets that explode the star in the frame of the jittering jets explosion mechanism. This suggests that most likely the shaping-jets are the last jets in the jittering jets explosion mechanism rather than post-kick jets. (3) The jittering jets explosion mechanism expects that black holes have small natal kick velocities.

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Possible post-kick jets in SN 1987A

Cited by 4 publications

References 62 publications

Statistical tests of young radio pulsars with/without supernova remnants: implying two origins of neutron stars

Statistical tests of young radio pulsars with/without supernova remnants: implying two origins of neutron stars

Statistical tests of young radio pulsars with/without supernova remnants: implying two origins of neutron stars

Implications of post-kick jets in core-collapse supernovae

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