Evidence for three-dimensional spin–velocity alignment in a pulsar

Yao, Jumei; Zhu, Weiwei; Manchester, R. N.; Coles, W. A.; Li, Di; Wang, Na; Krämer, M.; Stinebring, Daniel R.; Feng, Yi; Yan, W. M.; Miao, Chenchen; Yuan, Mao; Wang, Pei; Lu, Jiguang

doi:10.1038/s41550-021-01360-w

Cited by 42 publications

(47 citation statements)

References 37 publications

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“…More interestingly, from the H α image of S147 presented by Gvaramadze (2006), the filamentary structure seems to be more concentrated in the south-east, opposite to the direction of the pulsar proper motion. The distance of this remnant is estimated to be approximately 1.3 kpc, consistent with that of PSR J0538+2817 (Dinc ¸el et al 2015;Yao et al 2021). Sofue et al (1980) presented a 5 GHz map of S147 and measured its angular radius as θ s = 83 ± 3 , which corresponds to a size of R s = 32.1 ± 4.8 pc at a distance of 1.33 ± 0.19 kpc (Yao et al 2021).…”

Section: Psr J0538+2817 and S147supporting

confidence: 67%

“…After converting it to the local standard of rest (LSR), the proper motion becomes µ α = −24.4 ± 0.1 mas yr −1 and µ δ = 57.2 ± 0.1 mas yr −1 (Dinc ¸el et al 2015). Then, assuming a distance of 1.33 ± 0.19 kpc, the transverse velocity in the LSR is 391 ± 56 km s −1 (Yao et al 2021). From the transverse velocity and the conjecture of its association with S147, its kinematic age can be derived as 34.8±0.4 kyr (Yao et al 2021).…”

Section: Psr J0538+2817 and S147mentioning

confidence: 98%

“…Then, assuming a distance of 1.33 ± 0.19 kpc, the transverse velocity in the LSR is 391 ± 56 km s −1 (Yao et al 2021). From the transverse velocity and the conjecture of its association with S147, its kinematic age can be derived as 34.8±0.4 kyr (Yao et al 2021). In general, we summarize the observed and derived parameters of PSR J0538+2817 in Table 1 for reference.…”

Section: Psr J0538+2817 and S147mentioning

confidence: 98%

“…Recently, Yao et al (2021) reported the evidence for 3D spinvelocity alignment of PSR J0538+2817. They adopted a scintillation method to get the radial velocity of this pulsar by using the observations made with the Five-hundred-meter Aperture Spherical Radio Telescope (FAST).…”

Section: Introductionmentioning

confidence: 99%

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Is the Birth of PSR J0538+2817 Accompanied by a Gamma-ray Burst?

Xu,

Geng,

Wang

et al. 2021

Preprint

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Recently, the Five-hundred-meter Aperture Spherical radio Telescope (FAST) measured the three-dimensional velocity of PSR J0538+2817 in its associated supernova remnant S147 and found a possible spin-velocity alignment in this pulsar. Here we show that the high velocity and the spin-velocity alignment in this pulsar can be explained by the so-called electromagnetic rocket mechanism. In this framework, the pulsar is kicked in the direction of the spin axis, which naturally explains the spin-velocity alignment. We scrutinize the evolution of this pulsar and show that the pulsar kick can create a highly relativistic jet at the opposite direction of the kick velocity. The lifetime and energetics of the jet is estimated. It is argued that the jet can generate a Gamma-ray Burst (GRB). The long term dynamical evolution of the jet is calculated. It is found that the shock radius of the jet should expand to about 32 pc at present, which is well consistent with the observed radius of the supernova remnant S147 (32.1 ± 4.8 pc). Additionally, our calculations indicate that the current velocity of the GRB remnant should be about 440 km s −1 , which is also consistent with the observed blast wave velocity of the remnant of S147 (500 km s −1 ).

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Section: Psr J0538+2817 and S147supporting

confidence: 67%

Section: Psr J0538+2817 and S147mentioning

confidence: 98%

Section: Psr J0538+2817 and S147mentioning

confidence: 98%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Is the Birth of PSR J0538+2817 Accompanied by a Gamma-ray Burst?

Xu,

Geng,

Wang

et al. 2021

Preprint

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“…We note that other studies have found associations with foreground sources. The most clear associations are for pulsars within supernova remnants -the screen in the Crab nebula has be used to probe pulsar separation of giant pulse emission regions (Main et al 2021), andYao et al (2021) measured the distance between PSR J0538+2817 and the supernova remnant shell using scintillation arcs, suggesting a 3D spin-velocity alignment of the pulsar. Dexter et al (2017) used the VLBA + VLA to measure angular broadening of several pulsars, and were able to associate scattering screens of three sources with foreground HII regions, and three sources within Carina-Sagittarius spiral arm of the Milky Way.…”

Section: Screen Association With Sh 2-27mentioning

confidence: 99%

Modelling annual scintillation arc variations in PSR J1643-1224 using the Large European Array for Pulsars

Mall,

Main,

Antoniadis

et al. 2022

Preprint

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In this work we study variations in the parabolic scintillation arcs of the binary millisecond pulsar PSR J1643−1224 over five years using the Large European Array for Pulsars (LEAP). The 2D power spectrum of scintillation, called the secondary spectrum, often shows a parabolic distribution of power, where the arc curvature encodes the relative velocities and distances of the pulsar, ionised interstellar medium (IISM), and Earth. We observe a clear parabolic scintillation arc which varies in curvature throughout the year. The distribution of power in the secondary spectra are inconsistent with a single scattering screen which is fully 1D, or entirely isotropic. We fit the observed arc curvature variations with two models; an isotropic scattering screen, and a model with two independent 1D screens. We measure the distance to the scattering screen to be in the range 114-223 pc, depending on the model, consistent with the known distance of the foreground large-diameter HII region Sh 2-27 (112 ± 17 pc), suggesting that it is the dominant source of scattering. We obtain only weak constraints on the pulsar's orbital inclination and angle of periastron, since the scintillation pattern is not very sensitive to the pulsar's motion, since the screen is much closer to the Earth than the pulsar. More measurements of this kind -where scattering screens can be associated with foreground objects -will help to inform the origins and distribution of scattering screens within our galaxy.

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Interplay between neutrino kicks and hydrodynamic kicks of neutron stars and black holes

Janka,

Kresse

2024

Astrophys Space Sci

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Neutron stars (NSs) are observed with high space velocities and elliptical orbits in binaries. The magnitude of these effects points to natal kicks that originate from asymmetries during the supernova (SN) explosions. Using a growing set of long-time 3D SN simulations with the Prometheus-Vertex code, we explore the interplay of NS kicks that are induced by asymmetric neutrino emission and by asymmetric mass ejection. Anisotropic neutrino emission can arise from a large-amplitude dipolar convection asymmetry inside the proto-NS (PNS) termed LESA (Lepton-number Emission Self-sustained Asymmetry) and from aspherical accretion downflows around the PNS, which can lead to anisotropic neutrino emission (absorption/scattering) with a neutrino-induced NS kick roughly opposite to (aligned with) the kick by asymmetric mass ejection. In massive progenitors, hydrodynamic kicks can reach up to more than 1300 km s−1, whereas our calculated neutrino kicks reach (55–140) km s−1 (estimated upper bounds of (170–265) km s−1) and only ∼(10–50) km s−1, if LESA is the main cause of asymmetric neutrino emission. Therefore, hydrodynamic NS kicks dominate in explosions of high-mass progenitors, whereas LESA-induced neutrino kicks dominate for NSs born in low-energy SNe of the lowest-mass progenitors, when these explode nearly spherically. Our models suggest that the Crab pulsar with its velocity of ∼160 km s−1, if born in the low-energy explosion of a low-mass, single-star progenitor, should have received a hydrodynamic kick in a considerably asymmetric explosion. Black holes, if formed by the collapse of short-lived PNSs and solely kicked by anisotropic neutrino emission, obtain velocities of only some km s−1.

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Evidence for three-dimensional spin–velocity alignment in a pulsar

Cited by 42 publications

References 37 publications

Is the Birth of PSR J0538+2817 Accompanied by a Gamma-ray Burst?

Is the Birth of PSR J0538+2817 Accompanied by a Gamma-ray Burst?

Modelling annual scintillation arc variations in PSR J1643-1224 using the Large European Array for Pulsars

Interplay between neutrino kicks and hydrodynamic kicks of neutron stars and black holes

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