Pulsar kicks and<i>γ</i>-ray burst

Cui, Xiaohong; Wang, Hong Guang; Xu, R. X.; Qiao, G. J.

doi:10.1051/0004-6361:20077200

Cited by 10 publications

(4 citation statements)

References 31 publications

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“…Pulsars are created in supernovae, and the birth process is expected to impart a high 'kick velocity'. Various mechanisms have been proposed for these kicks, including an asymmetric neutrino emission in the presence of super-strong magnetic fields (Lai & Qian 1998), a postnatal electromagnetic rocket mechanism (Harrison & Tademaru 1975), asymmetric explosion of γ-ray bursts (Cui et al 2007) and hydrodynamical instabilities in the collapsed supernova core (Lai & Goldreich 2000). While the evidence for such kicks is unequivocal (Johnston et al 2005), their physical origin remains unclear.…”

Section: Proper Motionsmentioning

confidence: 99%

Timing of young radio pulsars – I. Timing noise, periodic modulation, and proper motion

Parthasarathy

Shannon

Johnston

et al. 2019

Monthly Notices of the Royal Astronomical Society

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The smooth spin-down of young pulsars is perturbed by two non-deterministic phenomenon, glitches and timing noise. Although the timing noise provides insights into nuclear and plasma physics at extreme densities, it acts as a barrier to high-precision pulsar timing experiments. An improved methodology based on Bayesian inference is developed to simultaneously model the stochastic and deterministic parameters for a sample of 85 high-E radio pulsars observed for ∼ 10 years with the 64-m Parkes radio telescope. Timing noise is known to be a red process and we develop a parametrization based on the red-noise amplitude (A red ) and spectral index (β). We measure the median A red to be −10.4 +1.8 −1.7 yr 3/2 and β to be −5.2 +3.0 −3.8 and show that the strength of timing noise scales proportionally to ν 1 | ν| −0.6±0.1 , where ν is the spin frequency of the pulsar and ν its spin-down rate. Finally, we measure significant braking indices for 19 pulsars, proper motions for two pulsars and discuss the presence of periodic modulation in the arrival times of five pulsars.

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Section: Proper Motionsmentioning

confidence: 99%

Timing of young radio pulsars – I. Timing noise, periodic modulation, and proper motion

Parthasarathy

Shannon

Johnston

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…Lyne & Lorimer (1994) and Hobbs et al (2005) analysed a large number of pulsar proper motions and demonstrated that their transverse velocities are typically several hundred km s −1 . Various explanations have been proposed for these high velocities, including a postnatal electromagnetic rocket mechanism (Harrison & Tademaru 1975), asymmetric neutrino emission in the presence of super-strong magnetic fields (Lai & Qian 1998), hydrodynamical instabilities in the collapsed supernova core (Lai & Goldreich 2000) and the asymmetric explosion of γ-ray bursts (Cui et al 2007). Knowledge of pulsar proper motions and velocities is essential for many aspects of pulsar and neutron star astrophysics including determinations of the birth rate of pulsars, associations with supernova remnants and the Galactic distribution of the progenitor population.…”

Section: Introductionmentioning

confidence: 99%

Proper motions of 15 pulsars: a comparison between Bayesian and frequentist algorithms

Wang

Yuan

et al. 2016

Mon. Not. R. Astron. Soc.

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We present proper motions for 15 pulsars which are observed regularly by the Nanshan 25-m radio telescope. Two methods, the frequentist method (Coles et al. 2011) and the Bayesian (Lentati et al. 2014) method, are used and the results are compared. We demonstrate that the two methods can be applied to young pulsar data sets that exhibit large amounts of timing noise with steep spectral exponents and give consistent results. The measured positions also agree with very-long-baseline interferometric positions. Proper motions for four pulsars are obtained for the first time, and improved values are obtained for five pulsars.

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“…However, what if the expanding of a fireball outside quark surface is not spherically symmetric? An asymmetric explosion may result both in a GRB-like fire jet and in a kick on quark stars, and the statistical result of Cui et al [61] indicated that the kick velocity of pulsars could be consistent with an asymmetric explosion of GRBs.…”

Section: An Idea Of Understanding Grb X-ray Flaresmentioning

confidence: 99%

X-ray flares of γ-ray bursts: Quakes of solid quark stars?

Liang

2009

Sci. China Ser. G-Phys. Mech. Astron.

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A star-quake model is proposed to understand X-ray flares of both long and short γ-ray bursts (GRBs) in a solid quark star regime. Two kinds of central engines for GRBs are available if pulsar-like stars are actually (solid) quark stars, i.e., the SNE-type GRBs and the SGR-type GRBs. It is found that a quark star could be solidified about 10 3 to 10 6 s later after its birth if the critical temperature of phase transition is a few Metga-electron-volts, and then a new source of free energy (i.e., elastic and gravitational ones, rather than rotational or magnetic energy) could be possible to power GRB X-ray flares.γ-rays, bursts: X-rays, neutron stars, elementary particles Swift, a multi-wavelength γ-ray burst (GRB) mission [1] , has led to great progress in understanding the nature of the GRB phenomenon (see recent reviews by Meszaros [2] and Zhang [3] ). With its promptly slewing capacity and high sensitivity, it catches the early afterglows and the extended prompt emission in details for the first time.This not only provides an opportunity to examine the conventional models established in the pre-Swift era [4][5][6][7][8] , but also facilitates studies of the transition between the prompt emission and the afterglow [8][9][10] , and even gives insight into the properties of both the progenitors and the GRB central engines [5,11] .The GRB survey with CGRO (Compton γ-ray Observatory)/BATSE identified two types of GRBs, long-soft and short-hard GRBs, separated with burst duration of about 2 s [12] . On one hand, with firmed detections of GRB-supernovae connections for four nearby cases [13][14][15][16][17] , it is now generally accepted that long GRBs are associated with energetic core-collapse supernovae [18,19] (see a recent review by Woosley et al. [20] ). Interestingly, Li [21] found that the peak spectral energy of GRBs is correlated with the peak bolometric luminosity of the underlying supernovae (SNe), based on the four pair GRB-SNe connections. The X-ray transient 080109 associated with a normal core-collapse SN 2008D [22] also complies with this relation [23] . Signatures of long GRB-SNe connection may be also derived from a red bump in late optical afterglow lightcurves [14,24] and a long time lag between the GRB precursor and the main burst observed in some GRBs [25] . On the other hand, short GRBs coincide with the early-type stellar population with no or little current star formation [26][27][28][29][30][31] (see a recent review by Nakar [32] ), favoring mergers of compact object binaries as the progenitors of the short GRBs [33][34][35][36] .Although the progenitors of the long and short GRBs are different, the models for their central engines are similar, and essentially all can be simply classed as a rotating compact object that drives an ultra-relativistic outflow to produce both the prompt γ-rays and afterglows in lower energy bands. These models are highly constrained by the observations of the prompt γ-rays and multi-wavelength afterglows. It is well believed that the prompt γ-rays are produced b...

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Pulsar kicks andγ-ray burst

Cited by 10 publications

References 31 publications

Timing of young radio pulsars – I. Timing noise, periodic modulation, and proper motion

Timing of young radio pulsars – I. Timing noise, periodic modulation, and proper motion

Proper motions of 15 pulsars: a comparison between Bayesian and frequentist algorithms

X-ray flares of γ-ray bursts: Quakes of solid quark stars?

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